VOTable 1.4
RESOURCE (results)
INFO QUERY_STATUS = OK
INFO QUERY_TIMESTAMP = 2026-07-25T03:04:16.677
INFO QUERY = SELECT * FROM ivoa.ObsCore WHERE dataproduct_type IN ( 'image', 'cube' )
TABLE
FIELD obs_publisher_did |  | char[33*] | meta.ref.ivoid | obscore:Curation.PublisherDID | publisher dataset identifier
FIELD obs_collection |  | char[4] | meta.id | obscore:DataID.Collection | short name for the data collection
FIELD facility_name |  | char[3] | meta.id;instr.tel | obscore:Provenance.ObsConfig.Facility.name | telescope name
FIELD instrument_name |  | char[4] | meta.id;instr | obscore:Provenance.ObsConfig.Instrument.name | instrument name
FIELD obs_id |  | char[64*] | meta.id | obscore:DataID.observationID | internal dataset identifier
FIELD dataproduct_type |  | char[5*] | meta.code.class | obscore:ObsDataset.dataProductType | type of product
FIELD calib_level |  | int | meta.code;obs.calib | obscore:ObsDataset.calibLevel | calibration level (2 or 3). 2 if product_type = MOUS, 3 if product_type = GOUS
FIELD collections |  | char[128*] |  |  | Indicates that there are external products
FIELD target_name |  | char[256*] | meta.id;src | obscore:Target.Name | name of intended target
FIELD s_ra | deg | double | pos.eq.ra | obscore:Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 | RA of central coordinates
FIELD s_dec | deg | double | pos.eq.dec | obscore:Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 | DEC of central coordinates
FIELD s_fov | deg | double | phys.angSize;instr.fov | obscore:Char.SpatialAxis.Coverage.Bounds.Extent.diameter | size of the region covered (~diameter of minimum bounding circle)
FIELD s_region |  | char[*] | pos.outline;obs.field | obscore:Char.SpatialAxis.Coverage.Support.Area | region bounded by observation
FIELD s_xel1 |  | int | meta.number | obscore:Char.SpatialAxis.numBins1 | Number of elements along the first spatial axis
FIELD s_xel2 |  | int | meta.number | obscore:Char.SpatialAxis.numBins2 | Number of elements along the second spatial axis
FIELD em_xel |  | int | meta.number | obscore:Char.SpectralAxis.numBins | Number of elements along the spectral axis
FIELD t_xel |  | int | meta.number | obscore:Char.TimeAxis.numBins | Number of elements along the time axis
FIELD pol_xel |  | int | meta.number | obscore:Char.PolarizationAxis.numBins | Number of polarization samples
FIELD s_resolution | arcsec | double | pos.angResolution | obscore:Char.SpatialAxis.Resolution.refval.value | typical spatial resolution
FIELD t_min | d | double | time.start;obs.exposure | obscore:Char.TimeAxis.Coverage.Bounds.Limits.StartTime | start time of observation (MJD)
FIELD t_max | d | double | time.end;obs.exposure | obscore:Char.TimeAxis.Coverage.Bounds.Limits.StopTime | end time of observation (MJD)
FIELD t_exptime | s | double | time.duration;obs.exposure | obscore:Char.TimeAxis.Coverage.Support.Extent | exposure time of observation
FIELD t_resolution | s | double | time.resolution | obscore:Char.TimeAxis.Resolution.refval.value | typical temporal resolution
FIELD em_min | m | double | em.wl;stat.min | obscore:Char.SpectralAxis.Coverage.Bounds.Limits.LoLimit | start spectral coordinate value
FIELD em_max | m | double | em.wl;stat.max | obscore:Char.SpectralAxis.Coverage.Bounds.Limits.HiLimit | stop spectral coordinate value
FIELD em_res_power |  | double | spect.resolution | obscore:Char.SpectralAxis.Resolution.ResolPower.refval | typical spectral resolution
FIELD pol_states |  | char[64*] | meta.code;phys.polarization | obscore:Char.PolarizationAxis.stateList | polarization states present in the data
FIELD o_ucd |  | char[35] | meta.ucd | obscore:Char.ObservableAxis.ucd | UCD describing the observable axis (pixel values)
FIELD access_url |  | char[72*] | meta.ref.url | obscore:Access.Reference | URL to download the data
FIELD access_format |  | char[9] | meta.code.mime | obscore:Access.Format | Content format of the data
FIELD access_estsize | kbyte | int | phys.size;meta.file | obscore:Access.Size | Estimated size of datasets in kilobytes
FIELD proposal_id |  | char[64*] | meta.id;obs.proposal | obscore:Provenance.Proposal.identifier | Identifier of proposal to which NO observation belongs.
FIELD data_rights |  | char[11] | meta.code | obscore:Curation.Rights | Access to data.
FIELD gal_longitude | deg | double | pos.galactic.lon |  | Galactic longitude of the observation for RA/Dec. Estimated using PyEphem and RA/Dec.
FIELD gal_latitude | deg | double | pos.galactic.lat |  | Galactic latitude of the observation for RA/Dec. Estimated using PyEphem and RA/Dec.
FIELD band_list |  | char[30*] |  |  | Space delimited list of bands
FIELD em_resolution | m | double | spect.resolution;stat.mean | obscore:Char.SpectralAxis.Resolution.refval.value | Estimated frequency resolution from all the spectral windows, using median values of channel widths.
FIELD bandwidth | Hz | double | em.freq;instr.bandpass | obscore:Char.SpectralAxis.Coverage.Bounds.Extent | Total Bandwidth
FIELD antenna_arrays |  | char[660*] | meta.code.member;instr.setup |  | Blank-separated list of Pad:Antenna pairs, i.e., A109:DV09 J504:DV02 J505:DV05 for antennas DV09, DV02 and DV05 sitting on pads A109, J504, and J505, respectively.
FIELD is_mosaic |  | char |  |  | Flag to indicate if this ASDM represents a mosaic or not.
FIELD obs_release_date |  | char[*] | time.release | obscore:Curation.releaseDate | timestamp of date the data becomes publicly available
FIELD spatial_resolution | arcsec | double |  |  | Average of the maximum and minimum spatial resolution values of all spectral windows
FIELD frequency_support | GHz | char[4000*] | em.freq;obs;meta.main | obscore:Char.SpectralAxis.Coverage.Location.support | All frequency ranges used by the field
FIELD frequency | GHz | double | em.freq;obs;meta.main | obscore:Char.SpectralAxis.Coverage.Location.refval | Observed (tuned) reference frequency on the sky.
FIELD velocity_resolution | m/s | double | phys.veloc;spect.resolution | obscore:Char.VelocityAxis.Resolution.refval | Estimated velocity resolution from all the spectral windows, from frequency resolution.
FIELD obs_creator_name |  | char[256*] | meta.id | obscore:DataID.Creator | case-insensitive partial match over the full PI name. Wildcards can be used
FIELD pub_title |  | char[256*] |  |  | Case insensitive search through the title of the publication.
FIELD first_author |  | char[256*] |  |  | The first author as provided by <a href="http://telbib.eso.org">telbib.eso.org</a>.
FIELD authors |  | char[4000*] |  |  | Full list of first author and all co-authors
FIELD pub_abstract |  | char[4000*] |  |  | Case insensitive text search through the abstract of the publication.
FIELD publication_year |  | int |  |  | The year the publication did appear in the printed version of the refereed journal.
FIELD proposal_abstract |  | char[4000*] | meta.abstract |  | Text search on the proposal abstract. Only abstracts will be returned which contain the given text. The search is case-insensitive.
FIELD schedblock_name |  | char[128*] | meta.code;obs;instr.setup |  | Name of the Scheduling Block used as a template for executing the ASDM containing this Field.
FIELD proposal_authors |  | char[2000*] | meta.id.CoI |  | Full name of CoIs .
FIELD sensitivity_10kms | mJy/beam | double |  |  | Estimated noise in an nominal 10km/s bandwidth. Note this is an indication only, it does not include the effects of flagging or Hanning smoothing, and a 10km/s bandwidth may not be achievable with the data as taken.
FIELD cont_sensitivity_bandwidth | mJy/beam | double |  |  | Estimated noise in the aggregated continuum bandwidth. Note this is an indication only, it does not include the effects of flagging or dynamic range limitations.
FIELD pwv | mm | float | obs.atmos.extinction |  | Estimated precipitable water vapour from the XML_CALWVR_ENTITIES table.
FIELD group_ous_uid |  | char[64*] |  |  | Group OUS ID
FIELD member_ous_uid |  | char[64*] |  |  | Member OUS ID
FIELD asdm_uid |  | char[32*] | meta.id |  | UID of the ASDM containing this Field.
FIELD obs_title |  | char[256*] | meta.title;obs | obscore:DataID.Title | Case-insensitive search over the project title
FIELD type |  | char[16*] |  |  | Type flags.
FIELD scan_intent |  | char[256*] | meta.code.class;obs |  | Scan intent list for the observed field.
FIELD science_observation |  | char | meta.code.class;obs |  | Flag to indicate whether this is a science observation.
FIELD spatial_scale_max | arcsec | double | pos.angResolution;stat.max | obscore:Characterisation.SpatialAxis.Coverage.Bounds.limits.Interval.HiLim | Due to the fact that radio antennas can not be placed infinitely close, measurements do have a smallest separation which translates into a maximal angular distance beyond which features can not be resolved reliably any more. Adding observations with the ALMA Total Power array can add those missing largest scales.
FIELD qa2_passed |  | char | meta.code |  | Quality Assessment 2 status: does the Member / Group OUS fulfil the PI's requirements?
FIELD bib_reference |  | char[4000*] | meta.bib.bibcode | obscore:Curation.Reference | Bibliography code
FIELD science_keyword |  | char[200*] |  |  | 
FIELD scientific_category |  | char[200*] |  |  | 
FIELD pi_userid |  | char[256*] |  |  | 
FIELD pi_name |  | char[256*] |  |  | 
FIELD spectral_resolution | kHz | double |  |  | 
FIELD lastModified |  | char[32*] |  |  | Time stamp of last modification of the metadata
ADS/JAO.ALMA#2021.1.00280.L	ALMA	JAO	ALMA	uid://A001/X15a2/Xe47.source.vuds_cosmos_5101288969.spw.25	cube	2		vuds_cosmos_5101288969	149.8777291666148	2.3315583333345336	0.00560163435901402	Polygon ICRS 149.877905 2.334354 149.878923 2.334093 149.879773 2.333476 149.880335 2.332589 149.880510 2.331909 149.880527 2.331382 149.880266 2.330366 149.879648 2.329517 149.879231 2.329194 149.878595 2.328895 149.877553 2.328763 149.876536 2.329024 149.875686 2.329641 149.875123 2.330527 149.874948 2.331207 149.874932 2.331734 149.875014 2.332255 149.875273 2.332908 149.875942 2.333716 149.876863 2.334222			480	1	2	0.9473804223445729	59667.986964	59672.028219	4415.04	4415.04	0.0010601514130454766	0.0010672135148489207	72422.31237686284	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X15a2/Xe47	application/x-votable+xml; content=datalink		2021.1.00280.L	Public	236.4961121565114	41.99767879305837	7	1.4734701531292603E-8	1.875E9	A001:DA57 A002:DA52 A003:DV18 A004:DA51 A005:DV13 A006:DV17 A007:DV04 A009:DV11 A010:DV15 A011:DV25 A013:DA43 A015:DV21 A016:DA61 A017:DV16 A019:DV14 A022:DV02 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A030:DA41 A031:DA59 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A038:DV22 A039:DV23 A040:DA50 A041:DV05 A042:DA60 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A049:DA44 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A067:DA46 A068:DA54 A072:DA53 A074:DA56	F	2023-05-10T15:26:10.000	0.9473804223445729	[280.91..282.78GHz,3904.30kHz,698uJy/beam@10km/s,49.4uJy/beam@native, XX YY] U [282.66..284.53GHz,3904.30kHz,680.1uJy/beam@10km/s,48.3uJy/beam@native, XX YY] U [292.85..294.72GHz,7812.01kHz,652.9uJy/beam@10km/s,47.2uJy/beam@native, XX YY] U [294.73..296.59GHz,7812.01kHz,651.6uJy/beam@10km/s,47.3uJy/beam@native, XX YY]	281.84704733663045	4114.04360866923	ALMA	Characterising the contribution of dust-obscured star formation at ≳ 5 using 18 serendipitously identified [C II] emitters JWST PRIMER: a lack of outshining in four normal z = 4 ‑ 6 galaxies from the ALMA-CRISTAL Survey Multiphase images of a powerful supernova-driven wind in the early Universe The ALMA-CRISTAL Survey: Spatial extent of [C II] line emission in star-forming galaxies at z = 4‑6 The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies The ALMA-CRISTAL Survey: Weak Evidence for Star-formation-driven Outflows in z ∼ 5 Main-sequence Galaxies The ALMA-CRISTAL survey: Discovery of a 15 kpc-long gas plume in a z = 4.54 Lyman-α blob The ALMA-CRISTAL survey: Extended [CII] emission in an interacting galaxy system at z ∼ 5.5 The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ∼1 Gyr old: I. Survey overview and case studies The ALMA-CRISTAL survey: Resolved kinematic studies of main sequence star-formin	Accard, C. Birkin, Jack E. Davies, Rebecca L. Faisst, A. L. Faisst, Andreas L. Herrera-Camus, R. Ikeda, Ryota Lee, Lilian L. Li, Juno Lines, N. E. P. Mitsuhashi, Ikki Posses, A. Ren, Wenke Solimano, M. Tsujita, Akiyoshi Wang, Wuji van Leeuwen, I. F.	Accard, C.; Béthermin, M.; Boquien, M.; Buat, V.; Vallini, L.; Renaud, F.; Kraljic, K.; Aravena, M.; Cassata, P.; da Cunha, E.; Dam, P.; de Looze, I.; Dessauges-Zavadsky, M.; Dubois, Y.; Faisst, A.; Fudamoto, Y.; Ginolfi, M.; Gruppioni, C.; Han, S.; Herrera-Camus, R.; Inami, H.; Koekemoer, A. M.; Lemaux, B. C.; Li, J.; Li, Y.; Mobasher, B.; Molina, J.; Nanni, A.; Palla, M.; Pozzi, F.; Relaño, M.; Romano, M.; Sawant, P.; Spilker, J.; Tsujita, A.; Veraldi, E.; Villanueva, V.; Wang, W.; Yi, S. K.; Zamorani, G. Birkin, Jack E.; Spilker, Justin S.; Herrera-Camus, Rodrigo; Davies, Rebecca L.; Lee, Lilian L.; Aravena, Manuel; Assef, Roberto J.; Barcos-Muñoz, Loreto; Bolatto, Alberto; Diaz-Santos, Tanio; Faisst, Andreas L.; Ferrara, Andrea; Fisher, Deanne B.; González-López, Jorge; Ikeda, Ryota; Knudsen, Kirsten; Li, Juno; Li, Yuan; de Looze, Ilse; Lutz, Dieter; Mitsuhashi, Ikki; Posses, Ana; Relaño, Monica; Solimano, Manuel; Tadaki, Ken-ichi; Villanueva, Vicente Davies, Rebecca L.; Fisher, D. B.; Herrera-Camus, R.;	Characterizing dust attenuation is crucial for revealing the intrinsic physical properties of galaxies. We present an analysis of dust attenuation in 18 spectroscopically confirmed star-forming main-sequence galaxies at z = 4.4−5.7 observed with JWST/NIRSpec IFU and NIRCam, selected from the ALPINE and CRISTAL ALMA large programs. We fit the emission-line fluxes from NIRSpec and the broadband photometry from NIRCam with PROSPECTOR, using both spatially integrated emission and ∼0.6 kpc pixel-by-pixel measurements. We derive the stellar-to-nebular dust attenuation ratio (f = E(B − V)<SUB>star</SUB>/E(B − V)<SUB>neb</SUB>) from the SED fits and the Balmer decrement with Hα and Hβ. Although individual galaxies show large scatter, the best-fit value is <inline-formula> <mml:math><mml:mi>f</mml:mi><mml:mo>=</mml:mo><mml:mn>0.5</mml:mn><mml:msubsup><mml:mrow><mml:mn>1</mml:mn></mml:mrow><mml:mrow><mml:mo>−</mml:mo><mml:mn>0.03</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>0.04</mml:mn></mml:mrow></mml:msubs	2024	ALMA has revolutionized our ability to characterize the cold gas and dust in distant galaxies, enabling pathfinding studies on global scales matched by premier observatories at other wavelengths. With deep HST imaging and the imminent launch of JWST, we are entering an era where stars and warm gas are studied in detail on kiloparsec scales. In this context we propose to carry out the CRISTAL Large Program, making good on one of the key design goals of ALMA to study early galaxies in [CII] emission on highly resolved scales. CRISTAL targets 19 typical z ~ 4-5 galaxies at kiloparsec physical resolution spanning a factor of 30 in stellar mass, and will produce detailed kinematic and morphological maps of the cool gas in and surrounding these galaxies. CRISTAL will provide the next leap forward and a lasting legacy in high-redshift galaxy kinematics, galactic outflows and halos, and ISM properties. CRISTAL enables the next frontier of multiwavelength resolved galaxy studies, combining ALMA, HST, and imminently JW	vuds_cos_e_07_TM2	Narayanan, Desika; Bolatto, Alberto; Davies, Rebecca; Lutz, Dieter; da Cunha, Elisabete; Knudsen, Kirsten; Bovino, Stefano; Barcos-Munoz, Loreto; Bouwens, Rychard; Fisher, Deanne; Genzel, Reinhard; Nagar, Neil; Smit, Renske; Diaz-Santos, Tanio; Assef, Roberto; Veilleux, Sylvain; Uebler, Hannah; Bowler, Rebecca; Naab, Thorsten; Calistro Rivera, Gabriela; Ikeda, Ryota; Price, Sedona; Sternberg, Amiel; Mitsuhashi, Ikki; Casey, Caitlin; Tacconi, Linda; Davies, Richard; Infante, Leopoldo; Hodge, Jacqueline;	0.6979570472494137	0.024010022422568535	1.4178485	uid://A001/X15a2/Xe44	uid://A001/X15a2/Xe47	uid://A002/Xf6d51d/X192a	CRISTAL: a survey of gas, dust and stars on kiloparsec scales in star-forming galaxies at z~4-5	L	TARGET	T	9.232303944471154	T	2024A&A...689A.145S 2024A&A...690A.197M 2024ApJ...976...70L 2024MNRAS.534.2062V 2025A&A...693A.237I 2025A&A...699A..80H 2025A&A...699A.256P 2025A&A...701A.260L 2025A&A...702A.206A 2025ApJ...985..243B 2025MNRAS.539.2685L 2025MNRAS.544..211R 2026ApJ...997..319T 2026ApJ..1000..308W 2026ApJ..1004...22F 2026ApJS..282...19F 2026MNRAS.549ag874D	Galaxy structure & evolution;null	Galaxy evolution	rhc	Herrera-Camus, Rodrigo	3904.296875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00280.L	ALMA	JAO	ALMA	uid://A001/X15a2/Xe47.source.vuds_cosmos_5101288969.spw.27	cube	2		vuds_cosmos_5101288969	149.8777291666148	2.3315583333345336	0.00560163435901402	Polygon ICRS 149.877905 2.334354 149.878923 2.334093 149.879773 2.333476 149.880335 2.332589 149.880510 2.331909 149.880527 2.331382 149.880266 2.330366 149.879648 2.329517 149.879231 2.329194 149.878595 2.328895 149.877553 2.328763 149.876536 2.329024 149.875686 2.329641 149.875123 2.330527 149.874948 2.331207 149.874932 2.331734 149.875014 2.332255 149.875273 2.332908 149.875942 2.333716 149.876863 2.334222			480	1	2	0.9473804223445729	59667.986964	59672.028219	4415.04	4415.04	0.0010536308347449445	0.0010606060454477978	72870.51050413486	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X15a2/Xe47	application/x-votable+xml; content=datalink		2021.1.00280.L	Public	236.4961121565114	41.99767879305837	7	1.4553407850096823E-8	1.875E9	A001:DA57 A002:DA52 A003:DV18 A004:DA51 A005:DV13 A006:DV17 A007:DV04 A009:DV11 A010:DV15 A011:DV25 A013:DA43 A015:DV21 A016:DA61 A017:DV16 A019:DV14 A022:DV02 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A030:DA41 A031:DA59 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A038:DV22 A039:DV23 A040:DA50 A041:DV05 A042:DA60 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A049:DA44 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A067:DA46 A068:DA54 A072:DA53 A074:DA56	F	2023-05-10T15:26:10.000	0.9473804223445729	[280.91..282.78GHz,3904.30kHz,698uJy/beam@10km/s,49.4uJy/beam@native, XX YY] U [282.66..284.53GHz,3904.30kHz,680.1uJy/beam@10km/s,48.3uJy/beam@native, XX YY] U [292.85..294.72GHz,7812.01kHz,652.9uJy/beam@10km/s,47.2uJy/beam@native, XX YY] U [294.73..296.59GHz,7812.01kHz,651.6uJy/beam@10km/s,47.3uJy/beam@native, XX YY]	283.5970973043045	4114.04360866923	ALMA	Characterising the contribution of dust-obscured star formation at ≳ 5 using 18 serendipitously identified [C II] emitters JWST PRIMER: a lack of outshining in four normal z = 4 ‑ 6 galaxies from the ALMA-CRISTAL Survey Multiphase images of a powerful supernova-driven wind in the early Universe The ALMA-CRISTAL Survey: Spatial extent of [C II] line emission in star-forming galaxies at z = 4‑6 The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies The ALMA-CRISTAL Survey: Weak Evidence for Star-formation-driven Outflows in z ∼ 5 Main-sequence Galaxies The ALMA-CRISTAL survey: Discovery of a 15 kpc-long gas plume in a z = 4.54 Lyman-α blob The ALMA-CRISTAL survey: Extended [CII] emission in an interacting galaxy system at z ∼ 5.5 The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ∼1 Gyr old: I. Survey overview and case studies The ALMA-CRISTAL survey: Resolved kinematic studies of main sequence star-formin	Accard, C. Birkin, Jack E. Davies, Rebecca L. Faisst, A. L. Faisst, Andreas L. Herrera-Camus, R. Ikeda, Ryota Lee, Lilian L. Li, Juno Lines, N. E. P. Mitsuhashi, Ikki Posses, A. Ren, Wenke Solimano, M. Tsujita, Akiyoshi Wang, Wuji van Leeuwen, I. F.	Accard, C.; Béthermin, M.; Boquien, M.; Buat, V.; Vallini, L.; Renaud, F.; Kraljic, K.; Aravena, M.; Cassata, P.; da Cunha, E.; Dam, P.; de Looze, I.; Dessauges-Zavadsky, M.; Dubois, Y.; Faisst, A.; Fudamoto, Y.; Ginolfi, M.; Gruppioni, C.; Han, S.; Herrera-Camus, R.; Inami, H.; Koekemoer, A. M.; Lemaux, B. C.; Li, J.; Li, Y.; Mobasher, B.; Molina, J.; Nanni, A.; Palla, M.; Pozzi, F.; Relaño, M.; Romano, M.; Sawant, P.; Spilker, J.; Tsujita, A.; Veraldi, E.; Villanueva, V.; Wang, W.; Yi, S. K.; Zamorani, G. Birkin, Jack E.; Spilker, Justin S.; Herrera-Camus, Rodrigo; Davies, Rebecca L.; Lee, Lilian L.; Aravena, Manuel; Assef, Roberto J.; Barcos-Muñoz, Loreto; Bolatto, Alberto; Diaz-Santos, Tanio; Faisst, Andreas L.; Ferrara, Andrea; Fisher, Deanne B.; González-López, Jorge; Ikeda, Ryota; Knudsen, Kirsten; Li, Juno; Li, Yuan; de Looze, Ilse; Lutz, Dieter; Mitsuhashi, Ikki; Posses, Ana; Relaño, Monica; Solimano, Manuel; Tadaki, Ken-ichi; Villanueva, Vicente Davies, Rebecca L.; Fisher, D. B.; Herrera-Camus, R.;	Characterizing dust attenuation is crucial for revealing the intrinsic physical properties of galaxies. We present an analysis of dust attenuation in 18 spectroscopically confirmed star-forming main-sequence galaxies at z = 4.4−5.7 observed with JWST/NIRSpec IFU and NIRCam, selected from the ALPINE and CRISTAL ALMA large programs. We fit the emission-line fluxes from NIRSpec and the broadband photometry from NIRCam with PROSPECTOR, using both spatially integrated emission and ∼0.6 kpc pixel-by-pixel measurements. We derive the stellar-to-nebular dust attenuation ratio (f = E(B − V)<SUB>star</SUB>/E(B − V)<SUB>neb</SUB>) from the SED fits and the Balmer decrement with Hα and Hβ. Although individual galaxies show large scatter, the best-fit value is <inline-formula> <mml:math><mml:mi>f</mml:mi><mml:mo>=</mml:mo><mml:mn>0.5</mml:mn><mml:msubsup><mml:mrow><mml:mn>1</mml:mn></mml:mrow><mml:mrow><mml:mo>−</mml:mo><mml:mn>0.03</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>0.04</mml:mn></mml:mrow></mml:msubs	2024	ALMA has revolutionized our ability to characterize the cold gas and dust in distant galaxies, enabling pathfinding studies on global scales matched by premier observatories at other wavelengths. With deep HST imaging and the imminent launch of JWST, we are entering an era where stars and warm gas are studied in detail on kiloparsec scales. In this context we propose to carry out the CRISTAL Large Program, making good on one of the key design goals of ALMA to study early galaxies in [CII] emission on highly resolved scales. CRISTAL targets 19 typical z ~ 4-5 galaxies at kiloparsec physical resolution spanning a factor of 30 in stellar mass, and will produce detailed kinematic and morphological maps of the cool gas in and surrounding these galaxies. CRISTAL will provide the next leap forward and a lasting legacy in high-redshift galaxy kinematics, galactic outflows and halos, and ISM properties. CRISTAL enables the next frontier of multiwavelength resolved galaxy studies, combining ALMA, HST, and imminently JW	vuds_cos_e_07_TM2	Narayanan, Desika; Bolatto, Alberto; Davies, Rebecca; Lutz, Dieter; da Cunha, Elisabete; Knudsen, Kirsten; Bovino, Stefano; Barcos-Munoz, Loreto; Bouwens, Rychard; Fisher, Deanne; Genzel, Reinhard; Nagar, Neil; Smit, Renske; Diaz-Santos, Tanio; Assef, Roberto; Veilleux, Sylvain; Uebler, Hannah; Bowler, Rebecca; Naab, Thorsten; Calistro Rivera, Gabriela; Ikeda, Ryota; Price, Sedona; Sternberg, Amiel; Mitsuhashi, Ikki; Casey, Caitlin; Tacconi, Linda; Davies, Richard; Infante, Leopoldo; Hodge, Jacqueline;	0.6801074634429114	0.024010022422568535	1.4178485	uid://A001/X15a2/Xe44	uid://A001/X15a2/Xe47	uid://A002/Xf6d51d/X192a	CRISTAL: a survey of gas, dust and stars on kiloparsec scales in star-forming galaxies at z~4-5	L	TARGET	T	9.232303944471154	T	2024A&A...689A.145S 2024A&A...690A.197M 2024ApJ...976...70L 2024MNRAS.534.2062V 2025A&A...693A.237I 2025A&A...699A..80H 2025A&A...699A.256P 2025A&A...701A.260L 2025A&A...702A.206A 2025ApJ...985..243B 2025MNRAS.539.2685L 2025MNRAS.544..211R 2026ApJ...997..319T 2026ApJ..1000..308W 2026ApJ..1004...22F 2026ApJS..282...19F 2026MNRAS.549ag874D	Galaxy structure & evolution;null	Galaxy evolution	rhc	Herrera-Camus, Rodrigo	3904.296875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00280.L	ALMA	JAO	ALMA	uid://A001/X15a2/Xe47.source.vuds_cosmos_5101288969.spw.31	cube	2		vuds_cosmos_5101288969	149.8777291666148	2.3315583333345336	0.00560163435901402	Polygon ICRS 149.877905 2.334354 149.878923 2.334093 149.879773 2.333476 149.880335 2.332589 149.880510 2.331909 149.880527 2.331382 149.880266 2.330366 149.879648 2.329517 149.879231 2.329194 149.878595 2.328895 149.877553 2.328763 149.876536 2.329024 149.875686 2.329641 149.875123 2.330527 149.874948 2.331207 149.874932 2.331734 149.875014 2.332255 149.875273 2.332908 149.875942 2.333716 149.876863 2.334222			240	1	2	0.9473804223445729	59667.986964	59672.028219	4415.04	4415.04	0.0010107852512189458	0.0010171894957653768	37724.0558680341	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X15a2/Xe47	application/x-votable+xml; content=datalink		2021.1.00280.L	Public	236.4961121565114	41.99767879305837	7	2.6791864999301455E-8	1.875E9	A001:DA57 A002:DA52 A003:DV18 A004:DA51 A005:DV13 A006:DV17 A007:DV04 A009:DV11 A010:DV15 A011:DV25 A013:DA43 A015:DV21 A016:DA61 A017:DV16 A019:DV14 A022:DV02 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A030:DA41 A031:DA59 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A038:DV22 A039:DV23 A040:DA50 A041:DV05 A042:DA60 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A049:DA44 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A067:DA46 A068:DA54 A072:DA53 A074:DA56	F	2023-05-10T15:26:10.000	0.9473804223445729	[280.91..282.78GHz,3904.30kHz,698uJy/beam@10km/s,49.4uJy/beam@native, XX YY] U [282.66..284.53GHz,3904.30kHz,680.1uJy/beam@10km/s,48.3uJy/beam@native, XX YY] U [292.85..294.72GHz,7812.01kHz,652.9uJy/beam@10km/s,47.2uJy/beam@native, XX YY] U [294.73..296.59GHz,7812.01kHz,651.6uJy/beam@10km/s,47.3uJy/beam@native, XX YY]	295.65994172454316	4114.04360866923	ALMA	Characterising the contribution of dust-obscured star formation at ≳ 5 using 18 serendipitously identified [C II] emitters JWST PRIMER: a lack of outshining in four normal z = 4 ‑ 6 galaxies from the ALMA-CRISTAL Survey Multiphase images of a powerful supernova-driven wind in the early Universe The ALMA-CRISTAL Survey: Spatial extent of [C II] line emission in star-forming galaxies at z = 4‑6 The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies The ALMA-CRISTAL Survey: Weak Evidence for Star-formation-driven Outflows in z ∼ 5 Main-sequence Galaxies The ALMA-CRISTAL survey: Discovery of a 15 kpc-long gas plume in a z = 4.54 Lyman-α blob The ALMA-CRISTAL survey: Extended [CII] emission in an interacting galaxy system at z ∼ 5.5 The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ∼1 Gyr old: I. Survey overview and case studies The ALMA-CRISTAL survey: Resolved kinematic studies of main sequence star-formin	Accard, C. Birkin, Jack E. Davies, Rebecca L. Faisst, A. L. Faisst, Andreas L. Herrera-Camus, R. Ikeda, Ryota Lee, Lilian L. Li, Juno Lines, N. E. P. Mitsuhashi, Ikki Posses, A. Ren, Wenke Solimano, M. Tsujita, Akiyoshi Wang, Wuji van Leeuwen, I. F.	Accard, C.; Béthermin, M.; Boquien, M.; Buat, V.; Vallini, L.; Renaud, F.; Kraljic, K.; Aravena, M.; Cassata, P.; da Cunha, E.; Dam, P.; de Looze, I.; Dessauges-Zavadsky, M.; Dubois, Y.; Faisst, A.; Fudamoto, Y.; Ginolfi, M.; Gruppioni, C.; Han, S.; Herrera-Camus, R.; Inami, H.; Koekemoer, A. M.; Lemaux, B. C.; Li, J.; Li, Y.; Mobasher, B.; Molina, J.; Nanni, A.; Palla, M.; Pozzi, F.; Relaño, M.; Romano, M.; Sawant, P.; Spilker, J.; Tsujita, A.; Veraldi, E.; Villanueva, V.; Wang, W.; Yi, S. K.; Zamorani, G. Birkin, Jack E.; Spilker, Justin S.; Herrera-Camus, Rodrigo; Davies, Rebecca L.; Lee, Lilian L.; Aravena, Manuel; Assef, Roberto J.; Barcos-Muñoz, Loreto; Bolatto, Alberto; Diaz-Santos, Tanio; Faisst, Andreas L.; Ferrara, Andrea; Fisher, Deanne B.; González-López, Jorge; Ikeda, Ryota; Knudsen, Kirsten; Li, Juno; Li, Yuan; de Looze, Ilse; Lutz, Dieter; Mitsuhashi, Ikki; Posses, Ana; Relaño, Monica; Solimano, Manuel; Tadaki, Ken-ichi; Villanueva, Vicente Davies, Rebecca L.; Fisher, D. B.; Herrera-Camus, R.;	Characterizing dust attenuation is crucial for revealing the intrinsic physical properties of galaxies. We present an analysis of dust attenuation in 18 spectroscopically confirmed star-forming main-sequence galaxies at z = 4.4−5.7 observed with JWST/NIRSpec IFU and NIRCam, selected from the ALPINE and CRISTAL ALMA large programs. We fit the emission-line fluxes from NIRSpec and the broadband photometry from NIRCam with PROSPECTOR, using both spatially integrated emission and ∼0.6 kpc pixel-by-pixel measurements. We derive the stellar-to-nebular dust attenuation ratio (f = E(B − V)<SUB>star</SUB>/E(B − V)<SUB>neb</SUB>) from the SED fits and the Balmer decrement with Hα and Hβ. Although individual galaxies show large scatter, the best-fit value is <inline-formula> <mml:math><mml:mi>f</mml:mi><mml:mo>=</mml:mo><mml:mn>0.5</mml:mn><mml:msubsup><mml:mrow><mml:mn>1</mml:mn></mml:mrow><mml:mrow><mml:mo>−</mml:mo><mml:mn>0.03</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>0.04</mml:mn></mml:mrow></mml:msubs	2024	ALMA has revolutionized our ability to characterize the cold gas and dust in distant galaxies, enabling pathfinding studies on global scales matched by premier observatories at other wavelengths. With deep HST imaging and the imminent launch of JWST, we are entering an era where stars and warm gas are studied in detail on kiloparsec scales. In this context we propose to carry out the CRISTAL Large Program, making good on one of the key design goals of ALMA to study early galaxies in [CII] emission on highly resolved scales. CRISTAL targets 19 typical z ~ 4-5 galaxies at kiloparsec physical resolution spanning a factor of 30 in stellar mass, and will produce detailed kinematic and morphological maps of the cool gas in and surrounding these galaxies. CRISTAL will provide the next leap forward and a lasting legacy in high-redshift galaxy kinematics, galactic outflows and halos, and ISM properties. CRISTAL enables the next frontier of multiwavelength resolved galaxy studies, combining ALMA, HST, and imminently JW	vuds_cos_e_07_TM2	Narayanan, Desika; Bolatto, Alberto; Davies, Rebecca; Lutz, Dieter; da Cunha, Elisabete; Knudsen, Kirsten; Bovino, Stefano; Barcos-Munoz, Loreto; Bouwens, Rychard; Fisher, Deanne; Genzel, Reinhard; Nagar, Neil; Smit, Renske; Diaz-Santos, Tanio; Assef, Roberto; Veilleux, Sylvain; Uebler, Hannah; Bowler, Rebecca; Naab, Thorsten; Calistro Rivera, Gabriela; Ikeda, Ryota; Price, Sedona; Sternberg, Amiel; Mitsuhashi, Ikki; Casey, Caitlin; Tacconi, Linda; Davies, Richard; Infante, Leopoldo; Hodge, Jacqueline;	0.6515668934607254	0.024010022422568535	1.4178485	uid://A001/X15a2/Xe44	uid://A001/X15a2/Xe47	uid://A002/Xf6d51d/X192a	CRISTAL: a survey of gas, dust and stars on kiloparsec scales in star-forming galaxies at z~4-5	L	TARGET	T	9.232303944471154	T	2024A&A...689A.145S 2024A&A...690A.197M 2024ApJ...976...70L 2024MNRAS.534.2062V 2025A&A...693A.237I 2025A&A...699A..80H 2025A&A...699A.256P 2025A&A...701A.260L 2025A&A...702A.206A 2025ApJ...985..243B 2025MNRAS.539.2685L 2025MNRAS.544..211R 2026ApJ...997..319T 2026ApJ..1000..308W 2026ApJ..1004...22F 2026ApJS..282...19F 2026MNRAS.549ag874D	Galaxy structure & evolution;null	Galaxy evolution	rhc	Herrera-Camus, Rodrigo	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00280.L	ALMA	JAO	ALMA	uid://A001/X15a2/Xe47.source.vuds_cosmos_5101288969.spw.29	cube	2		vuds_cosmos_5101288969	149.8777291666148	2.3315583333345336	0.00560163435901402	Polygon ICRS 149.877905 2.334354 149.878923 2.334093 149.879773 2.333476 149.880335 2.332589 149.880510 2.331909 149.880527 2.331382 149.880266 2.330366 149.879648 2.329517 149.879231 2.329194 149.878595 2.328895 149.877553 2.328763 149.876536 2.329024 149.875686 2.329641 149.875123 2.330527 149.874948 2.331207 149.874932 2.331734 149.875014 2.332255 149.875273 2.332908 149.875942 2.333716 149.876863 2.334222			240	1	2	0.9473804223445729	59667.986964	59672.028219	4415.04	4415.04	0.001017216052219103	0.0010237023074097648	37484.05478142597	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X15a2/Xe47	application/x-votable+xml; content=datalink		2021.1.00280.L	Public	236.4961121565114	41.99767879305837	7	2.7134952789408947E-8	1.875E9	A001:DA57 A002:DA52 A003:DV18 A004:DA51 A005:DV13 A006:DV17 A007:DV04 A009:DV11 A010:DV15 A011:DV25 A013:DA43 A015:DV21 A016:DA61 A017:DV16 A019:DV14 A022:DV02 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A030:DA41 A031:DA59 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A038:DV22 A039:DV23 A040:DA50 A041:DV05 A042:DA60 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A049:DA44 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A067:DA46 A068:DA54 A072:DA53 A074:DA56	F	2023-05-10T15:26:10.000	0.9473804223445729	[280.91..282.78GHz,3904.30kHz,698uJy/beam@10km/s,49.4uJy/beam@native, XX YY] U [282.66..284.53GHz,3904.30kHz,680.1uJy/beam@10km/s,48.3uJy/beam@native, XX YY] U [292.85..294.72GHz,7812.01kHz,652.9uJy/beam@10km/s,47.2uJy/beam@native, XX YY] U [294.73..296.59GHz,7812.01kHz,651.6uJy/beam@10km/s,47.3uJy/beam@native, XX YY]	293.7848881877496	4114.04360866923	ALMA	Characterising the contribution of dust-obscured star formation at ≳ 5 using 18 serendipitously identified [C II] emitters JWST PRIMER: a lack of outshining in four normal z = 4 ‑ 6 galaxies from the ALMA-CRISTAL Survey Multiphase images of a powerful supernova-driven wind in the early Universe The ALMA-CRISTAL Survey: Spatial extent of [C II] line emission in star-forming galaxies at z = 4‑6 The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies The ALMA-CRISTAL Survey: Weak Evidence for Star-formation-driven Outflows in z ∼ 5 Main-sequence Galaxies The ALMA-CRISTAL survey: Discovery of a 15 kpc-long gas plume in a z = 4.54 Lyman-α blob The ALMA-CRISTAL survey: Extended [CII] emission in an interacting galaxy system at z ∼ 5.5 The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ∼1 Gyr old: I. Survey overview and case studies The ALMA-CRISTAL survey: Resolved kinematic studies of main sequence star-formin	Accard, C. Birkin, Jack E. Davies, Rebecca L. Faisst, A. L. Faisst, Andreas L. Herrera-Camus, R. Ikeda, Ryota Lee, Lilian L. Li, Juno Lines, N. E. P. Mitsuhashi, Ikki Posses, A. Ren, Wenke Solimano, M. Tsujita, Akiyoshi Wang, Wuji van Leeuwen, I. F.	Accard, C.; Béthermin, M.; Boquien, M.; Buat, V.; Vallini, L.; Renaud, F.; Kraljic, K.; Aravena, M.; Cassata, P.; da Cunha, E.; Dam, P.; de Looze, I.; Dessauges-Zavadsky, M.; Dubois, Y.; Faisst, A.; Fudamoto, Y.; Ginolfi, M.; Gruppioni, C.; Han, S.; Herrera-Camus, R.; Inami, H.; Koekemoer, A. M.; Lemaux, B. C.; Li, J.; Li, Y.; Mobasher, B.; Molina, J.; Nanni, A.; Palla, M.; Pozzi, F.; Relaño, M.; Romano, M.; Sawant, P.; Spilker, J.; Tsujita, A.; Veraldi, E.; Villanueva, V.; Wang, W.; Yi, S. K.; Zamorani, G. Birkin, Jack E.; Spilker, Justin S.; Herrera-Camus, Rodrigo; Davies, Rebecca L.; Lee, Lilian L.; Aravena, Manuel; Assef, Roberto J.; Barcos-Muñoz, Loreto; Bolatto, Alberto; Diaz-Santos, Tanio; Faisst, Andreas L.; Ferrara, Andrea; Fisher, Deanne B.; González-López, Jorge; Ikeda, Ryota; Knudsen, Kirsten; Li, Juno; Li, Yuan; de Looze, Ilse; Lutz, Dieter; Mitsuhashi, Ikki; Posses, Ana; Relaño, Monica; Solimano, Manuel; Tadaki, Ken-ichi; Villanueva, Vicente Davies, Rebecca L.; Fisher, D. B.; Herrera-Camus, R.;	Characterizing dust attenuation is crucial for revealing the intrinsic physical properties of galaxies. We present an analysis of dust attenuation in 18 spectroscopically confirmed star-forming main-sequence galaxies at z = 4.4−5.7 observed with JWST/NIRSpec IFU and NIRCam, selected from the ALPINE and CRISTAL ALMA large programs. We fit the emission-line fluxes from NIRSpec and the broadband photometry from NIRCam with PROSPECTOR, using both spatially integrated emission and ∼0.6 kpc pixel-by-pixel measurements. We derive the stellar-to-nebular dust attenuation ratio (f = E(B − V)<SUB>star</SUB>/E(B − V)<SUB>neb</SUB>) from the SED fits and the Balmer decrement with Hα and Hβ. Although individual galaxies show large scatter, the best-fit value is <inline-formula> <mml:math><mml:mi>f</mml:mi><mml:mo>=</mml:mo><mml:mn>0.5</mml:mn><mml:msubsup><mml:mrow><mml:mn>1</mml:mn></mml:mrow><mml:mrow><mml:mo>−</mml:mo><mml:mn>0.03</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>0.04</mml:mn></mml:mrow></mml:msubs	2024	ALMA has revolutionized our ability to characterize the cold gas and dust in distant galaxies, enabling pathfinding studies on global scales matched by premier observatories at other wavelengths. With deep HST imaging and the imminent launch of JWST, we are entering an era where stars and warm gas are studied in detail on kiloparsec scales. In this context we propose to carry out the CRISTAL Large Program, making good on one of the key design goals of ALMA to study early galaxies in [CII] emission on highly resolved scales. CRISTAL targets 19 typical z ~ 4-5 galaxies at kiloparsec physical resolution spanning a factor of 30 in stellar mass, and will produce detailed kinematic and morphological maps of the cool gas in and surrounding these galaxies. CRISTAL will provide the next leap forward and a lasting legacy in high-redshift galaxy kinematics, galactic outflows and halos, and ISM properties. CRISTAL enables the next frontier of multiwavelength resolved galaxy studies, combining ALMA, HST, and imminently JW	vuds_cos_e_07_TM2	Narayanan, Desika; Bolatto, Alberto; Davies, Rebecca; Lutz, Dieter; da Cunha, Elisabete; Knudsen, Kirsten; Bovino, Stefano; Barcos-Munoz, Loreto; Bouwens, Rychard; Fisher, Deanne; Genzel, Reinhard; Nagar, Neil; Smit, Renske; Diaz-Santos, Tanio; Assef, Roberto; Veilleux, Sylvain; Uebler, Hannah; Bowler, Rebecca; Naab, Thorsten; Calistro Rivera, Gabriela; Ikeda, Ryota; Price, Sedona; Sternberg, Amiel; Mitsuhashi, Ikki; Casey, Caitlin; Tacconi, Linda; Davies, Richard; Infante, Leopoldo; Hodge, Jacqueline;	0.6528500154472863	0.024010022422568535	1.4178485	uid://A001/X15a2/Xe44	uid://A001/X15a2/Xe47	uid://A002/Xf6d51d/X192a	CRISTAL: a survey of gas, dust and stars on kiloparsec scales in star-forming galaxies at z~4-5	L	TARGET	T	9.232303944471154	T	2024A&A...689A.145S 2024A&A...690A.197M 2024ApJ...976...70L 2024MNRAS.534.2062V 2025A&A...693A.237I 2025A&A...699A..80H 2025A&A...699A.256P 2025A&A...701A.260L 2025A&A...702A.206A 2025ApJ...985..243B 2025MNRAS.539.2685L 2025MNRAS.544..211R 2026ApJ...997..319T 2026ApJ..1000..308W 2026ApJ..1004...22F 2026ApJS..282...19F 2026MNRAS.549ag874D	Galaxy structure & evolution;null	Galaxy evolution	rhc	Herrera-Camus, Rodrigo	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.1.00063.S	ALMA	JAO	ALMA	uid://A001/X1465/X3afc.source.J0423-0120.spw.22	cube	2		J0423-0120	65.8158363499986	-1.3425182027800084	0.008198646616831453	Circle ICRS 65.815836 -1.342518 0.004099			2048	1	2	3.599968363420269	58826.158649	58826.172666	1209.6	1209.6	8.988912915403266E-4	9.043119862489277E-4	295408.74469611555	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1465/X3afc	application/x-votable+xml; content=datalink		2019.1.00063.S	Public	195.29010352877754	-33.13991409726489	7	3.0609951027612676E-9	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11 N605:CM04	F	2021-05-14T05:51:35.000	3.599968363420269	[330.57..330.63GHz,60.58kHz,16.1mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [331.51..333.51GHz,1128.91kHz,14.3mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [342.51..344.51GHz,1128.91kHz,12.5mJy/beam@10km/s,944.7uJy/beam@native, XX YY] U [345.78..345.84GHz,60.58kHz,13.9mJy/beam@10km/s,6mJy/beam@native, XX YY]	332.51399985587284	52.52482313299516	ALMA						We propose to use the ACA to image the molecular environments of three well-known T Tauri stars at intermediate size of a few thousand au between that of protostellar cores and protoplanetary disks. The resolution of ~5 arcseconds lies in an observational blind spot, generally below the resolution of singledish telescopes and largely filtered out by interferometry. There are indications from scattered light images, CO maps, and theoretical predictions on the interaction between young stars and their surrounding clouds that infall onto disks can continue well into the Class II phase. These ACA mosaics will reveal the structure and kinematics of the kilo-au environment with much greater clarity than before.	GM_Aur_t_a_07_7M	Dullemond, Cornelis;	14.254885524686413	0.6970994455771604	0.91	uid://A001/X1465/X3afb	uid://A001/X1465/X3afc	uid://A002/Xe48598/X38382	The kilo-au environments of T Tauri stars	S	BANDPASS FLUX WVR	F	20.34714124624758	T		Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.1.00063.S	ALMA	JAO	ALMA	uid://A001/X1465/X3afc.source.J0423-0120.spw.18	cube	2		J0423-0120	65.8158363499986	-1.3425182027800084	0.008198646616831453	Circle ICRS 65.815836 -1.342518 0.004099			2048	1	2	3.599968363420269	58826.158649	58826.172666	1209.6	1209.6	8.701893643381298E-4	8.752684381891564E-4	303381.61010532326	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1465/X3afc	application/x-votable+xml; content=datalink		2019.1.00063.S	Public	195.29010352877754	-33.13991409726489	7	2.8680862915755685E-9	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11 N605:CM04	F	2021-05-14T05:51:35.000	3.599968363420269	[330.57..330.63GHz,60.58kHz,16.1mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [331.51..333.51GHz,1128.91kHz,14.3mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [342.51..344.51GHz,1128.91kHz,12.5mJy/beam@10km/s,944.7uJy/beam@native, XX YY] U [345.78..345.84GHz,60.58kHz,13.9mJy/beam@10km/s,6mJy/beam@native, XX YY]	343.5144591311892	52.52482313299516	ALMA						We propose to use the ACA to image the molecular environments of three well-known T Tauri stars at intermediate size of a few thousand au between that of protostellar cores and protoplanetary disks. The resolution of ~5 arcseconds lies in an observational blind spot, generally below the resolution of singledish telescopes and largely filtered out by interferometry. There are indications from scattered light images, CO maps, and theoretical predictions on the interaction between young stars and their surrounding clouds that infall onto disks can continue well into the Class II phase. These ACA mosaics will reveal the structure and kinematics of the kilo-au environment with much greater clarity than before.	GM_Aur_t_a_07_7M	Dullemond, Cornelis;	12.480630283846041	0.6970994455771604	0.91	uid://A001/X1465/X3afb	uid://A001/X1465/X3afc	uid://A002/Xe48598/X38382	The kilo-au environments of T Tauri stars	S	BANDPASS FLUX WVR	F	20.34714124624758	T		Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.1.00063.S	ALMA	JAO	ALMA	uid://A001/X1465/X3afc.source.J0423-0120.spw.16	cube	2		J0423-0120	65.8158363499986	-1.3425182027800084	0.008198646616831453	Circle ICRS 65.815836 -1.342518 0.004099			1024	1	2	3.599968363420269	58826.158649	58826.172666	1209.6	1209.6	8.668486874026486E-4	8.670052299187491E-4	5707633.840877718	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1465/X3afc	application/x-votable+xml; content=datalink		2019.1.00063.S	Public	195.29010352877754	-33.13991409726489	7	1.5186401804638815E-10	6.25E7	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11 N605:CM04	F	2021-05-14T05:51:35.000	3.599968363420269	[330.57..330.63GHz,60.58kHz,16.1mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [331.51..333.51GHz,1128.91kHz,14.3mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [342.51..344.51GHz,1128.91kHz,12.5mJy/beam@10km/s,944.7uJy/beam@native, XX YY] U [345.78..345.84GHz,60.58kHz,13.9mJy/beam@10km/s,6mJy/beam@native, XX YY]	345.8105177706255	52.52482313299516	ALMA						We propose to use the ACA to image the molecular environments of three well-known T Tauri stars at intermediate size of a few thousand au between that of protostellar cores and protoplanetary disks. The resolution of ~5 arcseconds lies in an observational blind spot, generally below the resolution of singledish telescopes and largely filtered out by interferometry. There are indications from scattered light images, CO maps, and theoretical predictions on the interaction between young stars and their surrounding clouds that infall onto disks can continue well into the Class II phase. These ACA mosaics will reveal the structure and kinematics of the kilo-au environment with much greater clarity than before.	GM_Aur_t_a_07_7M	Dullemond, Cornelis;	13.887291518229208	0.6970994455771604	0.91	uid://A001/X1465/X3afb	uid://A001/X1465/X3afc	uid://A002/Xe48598/X38382	The kilo-au environments of T Tauri stars	S	BANDPASS FLUX WVR	F	20.34714124624758	T		Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	60.577392578125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.1.00063.S	ALMA	JAO	ALMA	uid://A001/X1465/X3afc.source.J0423-0120.spw.20	cube	2		J0423-0120	65.8158363499986	-1.3425182027800084	0.008198646616831453	Circle ICRS 65.815836 -1.342518 0.004099			1024	1	2	3.599968363420269	58826.158649	58826.172666	1209.6	1209.6	9.067224222575048E-4	9.068936988588799E-4	5457622.166419588	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1465/X3afc	application/x-votable+xml; content=datalink		2019.1.00063.S	Public	195.29010352877754	-33.13991409726489	7	1.6615775400902276E-10	6.25E7	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11 N605:CM04	F	2021-05-14T05:51:35.000	3.599968363420269	[330.57..330.63GHz,60.58kHz,16.1mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [331.51..333.51GHz,1128.91kHz,14.3mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [342.51..344.51GHz,1128.91kHz,12.5mJy/beam@10km/s,944.7uJy/beam@native, XX YY] U [345.78..345.84GHz,60.58kHz,13.9mJy/beam@10km/s,6mJy/beam@native, XX YY]	330.60189219011005	52.52482313299516	ALMA						We propose to use the ACA to image the molecular environments of three well-known T Tauri stars at intermediate size of a few thousand au between that of protostellar cores and protoplanetary disks. The resolution of ~5 arcseconds lies in an observational blind spot, generally below the resolution of singledish telescopes and largely filtered out by interferometry. There are indications from scattered light images, CO maps, and theoretical predictions on the interaction between young stars and their surrounding clouds that infall onto disks can continue well into the Class II phase. These ACA mosaics will reveal the structure and kinematics of the kilo-au environment with much greater clarity than before.	GM_Aur_t_a_07_7M	Dullemond, Cornelis;	16.124282454011293	0.6970994455771604	0.91	uid://A001/X1465/X3afb	uid://A001/X1465/X3afc	uid://A002/Xe48598/X38382	The kilo-au environments of T Tauri stars	S	BANDPASS FLUX WVR	F	20.34714124624758	T		Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	60.577392578125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00563.S	ALMA	JAO	ALMA	uid://A001/X3833/X33f6.source.eHOPS-oph-44.spw.21	cube	2		eHOPS-oph-44	247.8985800000024	-24.02489000001104	0.007162046089694549	Polygon ICRS 247.900469 -24.028028 247.899071 -24.028443 247.897605 -24.028359 247.896691 -24.028028 247.896081 -24.027649 247.895144 -24.026615 247.894690 -24.025339 247.894690 -24.024441 247.894851 -24.023783 247.895559 -24.022607 247.896691 -24.021752 247.898089 -24.021337 247.899555 -24.021421 247.900884 -24.021993 247.901438 -24.022439 247.902016 -24.023165 247.902470 -24.024441 247.902493 -24.025115 247.902309 -24.025997 247.901601 -24.027173			2048	1	2	25.783269587243346	61031.632718	61120.45059	4992.288	4992.288	0.001360051386093205	0.0013604406207299799	3611959.696008926	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X33f6	application/x-votable+xml; content=datalink		2025.1.00563.S	Proprietary	354.17150600124484	16.269257186872036	6	3.766988253989769E-10	6.25E7	T702:PM03 T703:PM01	F	2027-03-25T19:09:01.000	23.273393786715232	[218.19..218.25GHz,35.28kHz,36.5mJy/beam@10km/s,12.4mJy/beam@native, XX YY] U [219.53..219.59GHz,61.04kHz,34.1mJy/beam@10km/s,11.7mJy/beam@native, XX YY] U [220.36..220.43GHz,61.04kHz,41.9mJy/beam@10km/s,14.4mJy/beam@native, XX YY] U [230.41..230.66GHz,141.11kHz,42.1mJy/beam@10km/s,7.4mJy/beam@native, XX YY] U [231.51..233.50GHz,31250.00kHz,35mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	220.3957691366087	48.452383422557126	ALMA						We propose to conduct an ACA stand-alone outflow survey of the complete population of 83 protostars in four nearby (d ~ 150 pc) southern molecular clouds: Ophiuchus, Corona Australis, Lupus, and the Pipe Nebula. We will use these data to measure outflow opening angles in order to determine the rate with which outflows widen, the maximum opening angles reached, and the resulting implications for the fraction of total initial dense core mass that outflows are capable of removing. This survey is motivated by recently published results suggesting outflows cease widening at earlier evolutionary stages than canonically believed, with smaller maximum opening angles that prevent outflows from removing sufficient mass to explain the observed star formation efficiency of 25% - 50% on dense core scales. While tantalizing, these results suffer from low statistical power. Our proposed survey will significantly improve the statistical power with which outflow opening angle trends can be determined, yielding new insights in	eHOPS-op_b_06_TP	Stephens, Ian; Mardones, Diego; Maureira, Maria Jose; Hsieh, Chenghan; Arce, Hector; Pineda, Jaime; Bourke, Tyler; Segura-Cox, Dominique; Myers, Phil; Arun, Aiswarya;	41.894352117573185	2.0121079856778854	0.7112223	uid://A001/X3833/X33f1	uid://A001/X3833/X33f6	uid://A002/X133dde2/Xe7b9	The Role of Protostellar Outflows in Regulating Star Formation: A Survey of Southern Outflows	S	TARGET	T	412.5338486731924	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	mdunham	Dunham, Michael	61.03515625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00563.S	ALMA	JAO	ALMA	uid://A001/X3833/X33f6.source.eHOPS-oph-44.spw.19	cube	2		eHOPS-oph-44	247.8985800000024	-24.02489000001104	0.007162046089694549	Polygon ICRS 247.900469 -24.028028 247.899071 -24.028443 247.897605 -24.028359 247.896691 -24.028028 247.896081 -24.027649 247.895144 -24.026615 247.894690 -24.025339 247.894690 -24.024441 247.894851 -24.023783 247.895559 -24.022607 247.896691 -24.021752 247.898089 -24.021337 247.899555 -24.021421 247.900884 -24.021993 247.901438 -24.022439 247.902016 -24.023165 247.902470 -24.024441 247.902493 -24.025115 247.902309 -24.025997 247.901601 -24.027173			2048	1	2	25.783269587243346	61031.632718	61120.45059	4992.288	4992.288	0.0013652436200519422	0.0013656355321214355	3598223.696008926	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X33f6	application/x-votable+xml; content=datalink		2025.1.00563.S	Proprietary	354.17150600124484	16.269257186872036	6	3.7958087407455045E-10	6.25E7	T702:PM03 T703:PM01	F	2027-03-25T19:09:01.000	23.273393786715232	[218.19..218.25GHz,35.28kHz,36.5mJy/beam@10km/s,12.4mJy/beam@native, XX YY] U [219.53..219.59GHz,61.04kHz,34.1mJy/beam@10km/s,11.7mJy/beam@native, XX YY] U [220.36..220.43GHz,61.04kHz,41.9mJy/beam@10km/s,14.4mJy/beam@native, XX YY] U [230.41..230.66GHz,141.11kHz,42.1mJy/beam@10km/s,7.4mJy/beam@native, XX YY] U [231.51..233.50GHz,31250.00kHz,35mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	219.55747396276007	48.452383422557126	ALMA						We propose to conduct an ACA stand-alone outflow survey of the complete population of 83 protostars in four nearby (d ~ 150 pc) southern molecular clouds: Ophiuchus, Corona Australis, Lupus, and the Pipe Nebula. We will use these data to measure outflow opening angles in order to determine the rate with which outflows widen, the maximum opening angles reached, and the resulting implications for the fraction of total initial dense core mass that outflows are capable of removing. This survey is motivated by recently published results suggesting outflows cease widening at earlier evolutionary stages than canonically believed, with smaller maximum opening angles that prevent outflows from removing sufficient mass to explain the observed star formation efficiency of 25% - 50% on dense core scales. While tantalizing, these results suffer from low statistical power. Our proposed survey will significantly improve the statistical power with which outflow opening angle trends can be determined, yielding new insights in	eHOPS-op_b_06_TP	Stephens, Ian; Mardones, Diego; Maureira, Maria Jose; Hsieh, Chenghan; Arce, Hector; Pineda, Jaime; Bourke, Tyler; Segura-Cox, Dominique; Myers, Phil; Arun, Aiswarya;	34.07544244278492	2.0121079856778854	0.7112223	uid://A001/X3833/X33f1	uid://A001/X3833/X33f6	uid://A002/X133dde2/Xe7b9	The Role of Protostellar Outflows in Regulating Star Formation: A Survey of Southern Outflows	S	TARGET	T	412.5338486731924	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	mdunham	Dunham, Michael	61.03515625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00563.S	ALMA	JAO	ALMA	uid://A001/X3833/X33f6.source.eHOPS-oph-44.spw.25	image	2		eHOPS-oph-44	247.8985800000024	-24.02489000001104	0.007162046089694549	Polygon ICRS 247.900469 -24.028028 247.899071 -24.028443 247.897605 -24.028359 247.896691 -24.028028 247.896081 -24.027649 247.895144 -24.026615 247.894690 -24.025339 247.894690 -24.024441 247.894851 -24.023783 247.895559 -24.022607 247.896691 -24.021752 247.898089 -24.021337 247.899555 -24.021421 247.900884 -24.021993 247.901438 -24.022439 247.902016 -24.023165 247.902470 -24.024441 247.902493 -24.025115 247.902309 -24.025997 247.901601 -24.027173			128	1	2	25.783269587243346	61031.632718	61120.45059	4992.288	4992.288	0.0012839298394564768	0.0012949393386276825	7409.347292900743	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X33f6	application/x-votable+xml; content=datalink		2025.1.00563.S	Proprietary	354.17150600124484	16.269257186872036	6	1.733085686429815E-7	2.0E9	T702:PM03 T703:PM01	F	2027-03-25T19:09:01.000	23.273393786715232	[218.19..218.25GHz,35.28kHz,36.5mJy/beam@10km/s,12.4mJy/beam@native, XX YY] U [219.53..219.59GHz,61.04kHz,34.1mJy/beam@10km/s,11.7mJy/beam@native, XX YY] U [220.36..220.43GHz,61.04kHz,41.9mJy/beam@10km/s,14.4mJy/beam@native, XX YY] U [230.41..230.66GHz,141.11kHz,42.1mJy/beam@10km/s,7.4mJy/beam@native, XX YY] U [231.51..233.50GHz,31250.00kHz,35mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	232.50339682034422	48.452383422557126	ALMA						We propose to conduct an ACA stand-alone outflow survey of the complete population of 83 protostars in four nearby (d ~ 150 pc) southern molecular clouds: Ophiuchus, Corona Australis, Lupus, and the Pipe Nebula. We will use these data to measure outflow opening angles in order to determine the rate with which outflows widen, the maximum opening angles reached, and the resulting implications for the fraction of total initial dense core mass that outflows are capable of removing. This survey is motivated by recently published results suggesting outflows cease widening at earlier evolutionary stages than canonically believed, with smaller maximum opening angles that prevent outflows from removing sufficient mass to explain the observed star formation efficiency of 25% - 50% on dense core scales. While tantalizing, these results suffer from low statistical power. Our proposed survey will significantly improve the statistical power with which outflow opening angle trends can be determined, yielding new insights in	eHOPS-op_b_06_TP	Stephens, Ian; Mardones, Diego; Maureira, Maria Jose; Hsieh, Chenghan; Arce, Hector; Pineda, Jaime; Bourke, Tyler; Segura-Cox, Dominique; Myers, Phil; Arun, Aiswarya;	35.04341181926826	2.0121079856778854	0.7112223	uid://A001/X3833/X33f1	uid://A001/X3833/X33f6	uid://A002/X133dde2/Xe7b9	The Role of Protostellar Outflows in Regulating Star Formation: A Survey of Southern Outflows	S	TARGET	T	412.5338486731924	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	mdunham	Dunham, Michael	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00563.S	ALMA	JAO	ALMA	uid://A001/X3833/X33f6.source.eHOPS-oph-44.spw.17	cube	2		eHOPS-oph-44	247.8985800000024	-24.02489000001104	0.007162046089694549	Polygon ICRS 247.900469 -24.028028 247.899071 -24.028443 247.897605 -24.028359 247.896691 -24.028028 247.896081 -24.027649 247.895144 -24.026615 247.894690 -24.025339 247.894690 -24.024441 247.894851 -24.023783 247.895559 -24.022607 247.896691 -24.021752 247.898089 -24.021337 247.899555 -24.021421 247.900884 -24.021993 247.901438 -24.022439 247.902016 -24.023165 247.902470 -24.024441 247.902493 -24.025115 247.902309 -24.025997 247.901601 -24.027173			2048	1	2	25.783269587243346	61031.632718	61120.45059	4992.288	4992.288	0.001373614287749863	0.001374011541891458	6187362.454092008	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X33f6	application/x-votable+xml; content=datalink		2025.1.00563.S	Proprietary	354.17150600124484	16.269257186872036	6	2.2209683854489262E-10	6.25E7	T702:PM03 T703:PM01	F	2027-03-25T19:09:01.000	23.273393786715232	[218.19..218.25GHz,35.28kHz,36.5mJy/beam@10km/s,12.4mJy/beam@native, XX YY] U [219.53..219.59GHz,61.04kHz,34.1mJy/beam@10km/s,11.7mJy/beam@native, XX YY] U [220.36..220.43GHz,61.04kHz,41.9mJy/beam@10km/s,14.4mJy/beam@native, XX YY] U [230.41..230.66GHz,141.11kHz,42.1mJy/beam@10km/s,7.4mJy/beam@native, XX YY] U [231.51..233.50GHz,31250.00kHz,35mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	218.21927937392098	48.452383422557126	ALMA						We propose to conduct an ACA stand-alone outflow survey of the complete population of 83 protostars in four nearby (d ~ 150 pc) southern molecular clouds: Ophiuchus, Corona Australis, Lupus, and the Pipe Nebula. We will use these data to measure outflow opening angles in order to determine the rate with which outflows widen, the maximum opening angles reached, and the resulting implications for the fraction of total initial dense core mass that outflows are capable of removing. This survey is motivated by recently published results suggesting outflows cease widening at earlier evolutionary stages than canonically believed, with smaller maximum opening angles that prevent outflows from removing sufficient mass to explain the observed star formation efficiency of 25% - 50% on dense core scales. While tantalizing, these results suffer from low statistical power. Our proposed survey will significantly improve the statistical power with which outflow opening angle trends can be determined, yielding new insights in	eHOPS-op_b_06_TP	Stephens, Ian; Mardones, Diego; Maureira, Maria Jose; Hsieh, Chenghan; Arce, Hector; Pineda, Jaime; Bourke, Tyler; Segura-Cox, Dominique; Myers, Phil; Arun, Aiswarya;	36.459242844208944	2.0121079856778854	0.7112223	uid://A001/X3833/X33f1	uid://A001/X3833/X33f6	uid://A002/X133dde2/Xe7b9	The Role of Protostellar Outflows in Regulating Star Formation: A Survey of Southern Outflows	S	TARGET	T	412.5338486731924	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	mdunham	Dunham, Michael	35.2783203125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00563.S	ALMA	JAO	ALMA	uid://A001/X3833/X33f6.source.eHOPS-oph-44.spw.23	cube	2		eHOPS-oph-44	247.8985800000024	-24.02489000001104	0.007162046089694549	Polygon ICRS 247.900469 -24.028028 247.899071 -24.028443 247.897605 -24.028359 247.896691 -24.028028 247.896081 -24.027649 247.895144 -24.026615 247.894690 -24.025339 247.894690 -24.024441 247.894851 -24.023783 247.895559 -24.022607 247.896691 -24.021752 247.898089 -24.021337 247.899555 -24.021421 247.900884 -24.021993 247.901438 -24.022439 247.902016 -24.023165 247.902470 -24.024441 247.902493 -24.025115 247.902309 -24.025997 247.901601 -24.027173			2048	1	2	25.783269587243346	61031.632718	61120.45059	4992.288	4992.288	0.001299715287641543	0.001301127962223768	1633020.2784262334	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X33f6	application/x-votable+xml; content=datalink		2025.1.00563.S	Proprietary	354.17150600124484	16.269257186872036	6	7.960043206848638E-10	2.5E8	T702:PM03 T703:PM01	F	2027-03-25T19:09:01.000	23.273393786715232	[218.19..218.25GHz,35.28kHz,36.5mJy/beam@10km/s,12.4mJy/beam@native, XX YY] U [219.53..219.59GHz,61.04kHz,34.1mJy/beam@10km/s,11.7mJy/beam@native, XX YY] U [220.36..220.43GHz,61.04kHz,41.9mJy/beam@10km/s,14.4mJy/beam@native, XX YY] U [230.41..230.66GHz,141.11kHz,42.1mJy/beam@10km/s,7.4mJy/beam@native, XX YY] U [231.51..233.50GHz,31250.00kHz,35mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	230.53488245493293	48.452383422557126	ALMA						We propose to conduct an ACA stand-alone outflow survey of the complete population of 83 protostars in four nearby (d ~ 150 pc) southern molecular clouds: Ophiuchus, Corona Australis, Lupus, and the Pipe Nebula. We will use these data to measure outflow opening angles in order to determine the rate with which outflows widen, the maximum opening angles reached, and the resulting implications for the fraction of total initial dense core mass that outflows are capable of removing. This survey is motivated by recently published results suggesting outflows cease widening at earlier evolutionary stages than canonically believed, with smaller maximum opening angles that prevent outflows from removing sufficient mass to explain the observed star formation efficiency of 25% - 50% on dense core scales. While tantalizing, these results suffer from low statistical power. Our proposed survey will significantly improve the statistical power with which outflow opening angle trends can be determined, yielding new insights in	eHOPS-op_b_06_TP	Stephens, Ian; Mardones, Diego; Maureira, Maria Jose; Hsieh, Chenghan; Arce, Hector; Pineda, Jaime; Bourke, Tyler; Segura-Cox, Dominique; Myers, Phil; Arun, Aiswarya;	42.08856598810886	2.0121079856778854	0.7112223	uid://A001/X3833/X33f1	uid://A001/X3833/X33f6	uid://A002/X133dde2/Xe7b9	The Role of Protostellar Outflows in Regulating Star Formation: A Survey of Southern Outflows	S	TARGET	T	412.5338486731924	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	mdunham	Dunham, Michael	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00120.S	ALMA	JAO	ALMA	uid://A001/X14ed/X1de.source.IRAS_21543-1421.spw.20	cube	2		IRAS_21543-1421	329.2575833333389	-14.113372222222292	0.012282740404305971	Circle ICRS 329.257583 -14.113372 0.006141			2048	1	2	5.312298230431473	59487.086715	59487.090215	302.4	302.4	0.0013571812473460467	0.0013633504884971958	391323.36541146215	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14ed/X1de	application/x-votable+xml; content=datalink		2019.2.00120.S	Public	41.70500322347198	-47.410232808154696	6	3.4837946441472723E-9	1.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N604:CM11	F	2022-11-04T19:43:08.000	5.312298230431473	[218.00..220.00GHz,1128.91kHz,17.5mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [219.89..220.89GHz,564.45kHz,22.8mJy/beam@10km/s,2mJy/beam@native, XX YY] U [230.03..231.03GHz,564.45kHz,22.2mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [231.50..233.50GHz,1128.91kHz,16.5mJy/beam@10km/s,1mJy/beam@native, XX YY]	220.39367942341278	735.6607732013813	ALMA	A radical transition in the post-main-sequence system U Equulei	Kamiński, Tomek	Kamiński, Tomek; Schmidt, Mirek R.; Djupvik, Anlaug Amanda; Menten, Karl M.; Kraus, Alex; Iłkiewicz, Krystian; Steinmetz, Thomas; Mobeen, Muhammad Zain; Szczerba, Ryszard	Context. U Equ is an unusual maser-hosting infrared source discovered in the 1990s. It was tentatively classified as a post-asymptotic giant branch (post-AGB) star with a unique optical spectrum displaying rare emission and absorption features from molecular gas at a temperature of about 500 K. In 2022, we serendipitously discovered that its optical spectrum had drastically changed since the last observations in the 1990s. <BR /> Aims: We aim to characterize the drastic change in the spectrum and analyze the photometric behavior of the object since 1989. <BR /> Methods: Optical high-resolution spectra of U Equ from the Southern African Large Telescope were supplemented by archival data and near-infrared photometry from the Nordic Optical Telescope. New spectral line observations with the Effelsberg 100 m radio telescope and Atacam Large Millimeter Array are presented. Radiative transfer modeling of multiple epoch spectral energy distributions was performed. <BR /> Results: No circumstellar molecular features	2024	Outflows of asymptotic giant branch and red supergiant stars drive local galactic chemical evolution. The Nearby Evolved Stars Survey (NESS) is a global project targeting a volume-limited sample of evolved stars within 2 kpc to constrain the physics driving mass loss. NESS includes ongoing JCMT (515 hr) and APEX (56 hr) surveys to observe CO(2-1), CO(3-2) and dust continuum from ~500 sources, and at the Nobeyama observatory (190 hr) for CO(1-0). We propose 12CO and 13CO(2-1) and (3-2) observations of the 280 NESS sources visible to the ACA that do not have archival data (total sample 301 sources). Combining the high resolution and large field-of-view of the ACA with data from the JCMT and APEX, we will thoroughly probe their inner shells, revealing the mass-loss history, geometry and the 12C/13C and dust-to-gas ratios. The large, volume-limited sample will robustly constrain the onset of mass-loss variations and asymmetry. All NESS data, including reduced data, catalogues, codes and model results will be publ	IRAS_215_a_06_7M	Kraemer, Kathleen; Kaminski, Tomasz; Shinnaga, Hiroko; Zijlstra, Albert; Do, Hoai; Haswell, Carole; Srinivasan, Sundar; Menten, Karl; Wouterloot, Jan; Dharmawardena, Thavisha; Pham, Tuan Anh; Kim, Hyosun; Lagadec, Eric; Feng, Siyi; Peeters, Els; McDonald, Iain; Cami, Jan; Hirano, Naomi; Wallström, Sofia; Kuan, Yi-Jehng; Hora, Joseph; Toala, Jesus; Lee, Chin-Fei; Jones, Olivia; Young, Ken; Matsuura, Mikako; Greaves, Jane; Marshall, Jonathan; Kemper, Ciska; Antoniou, Vallia; Imai, Hiroshi; Goldman, Steven; Trejo, Alfonso; Boyer, Martha; Patel, Nimesh; Friberg, Per; van Loon, Jacco; Liu, Tie; Liu, Sheng-Yuan;	22.828130444796148	0.6503334384452819	1.8	uid://A001/X14ed/X1dd	uid://A001/X14ed/X1de	uid://A002/Xf138ff/X155d	The Nearby Evolved Stars Survey: quantifying the gas and dust return to the Galactic interstellar medium	S	TARGET	T	30.035648394160216	T	2024A&A...682A.133K	Asymptotic Giant Branch (AGB) stars;null	Stars and stellar evolution	pscicluna	Scicluna, Peter	564.453125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00120.S	ALMA	JAO	ALMA	uid://A001/X14ed/X1de.source.IRAS_21543-1421.spw.16	cube	2		IRAS_21543-1421	329.2575833333389	-14.113372222222292	0.012282740404305971	Circle ICRS 329.257583 -14.113372 0.006141			2048	1	2	5.312298230431473	59487.086715	59487.090215	302.4	302.4	0.0012976198702855457	0.0013032583807676833	407514.5351238324	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14ed/X1de	application/x-votable+xml; content=datalink		2019.2.00120.S	Public	41.70500322347198	-47.410232808154696	6	3.1840889563832366E-9	1.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N604:CM11	F	2022-11-04T19:43:08.000	5.312298230431473	[218.00..220.00GHz,1128.91kHz,17.5mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [219.89..220.89GHz,564.45kHz,22.8mJy/beam@10km/s,2mJy/beam@native, XX YY] U [230.03..231.03GHz,564.45kHz,22.2mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [231.50..233.50GHz,1128.91kHz,16.5mJy/beam@10km/s,1mJy/beam@native, XX YY]	230.53279551258123	735.6607732013813	ALMA	A radical transition in the post-main-sequence system U Equulei	Kamiński, Tomek	Kamiński, Tomek; Schmidt, Mirek R.; Djupvik, Anlaug Amanda; Menten, Karl M.; Kraus, Alex; Iłkiewicz, Krystian; Steinmetz, Thomas; Mobeen, Muhammad Zain; Szczerba, Ryszard	Context. U Equ is an unusual maser-hosting infrared source discovered in the 1990s. It was tentatively classified as a post-asymptotic giant branch (post-AGB) star with a unique optical spectrum displaying rare emission and absorption features from molecular gas at a temperature of about 500 K. In 2022, we serendipitously discovered that its optical spectrum had drastically changed since the last observations in the 1990s. <BR /> Aims: We aim to characterize the drastic change in the spectrum and analyze the photometric behavior of the object since 1989. <BR /> Methods: Optical high-resolution spectra of U Equ from the Southern African Large Telescope were supplemented by archival data and near-infrared photometry from the Nordic Optical Telescope. New spectral line observations with the Effelsberg 100 m radio telescope and Atacam Large Millimeter Array are presented. Radiative transfer modeling of multiple epoch spectral energy distributions was performed. <BR /> Results: No circumstellar molecular features	2024	Outflows of asymptotic giant branch and red supergiant stars drive local galactic chemical evolution. The Nearby Evolved Stars Survey (NESS) is a global project targeting a volume-limited sample of evolved stars within 2 kpc to constrain the physics driving mass loss. NESS includes ongoing JCMT (515 hr) and APEX (56 hr) surveys to observe CO(2-1), CO(3-2) and dust continuum from ~500 sources, and at the Nobeyama observatory (190 hr) for CO(1-0). We propose 12CO and 13CO(2-1) and (3-2) observations of the 280 NESS sources visible to the ACA that do not have archival data (total sample 301 sources). Combining the high resolution and large field-of-view of the ACA with data from the JCMT and APEX, we will thoroughly probe their inner shells, revealing the mass-loss history, geometry and the 12C/13C and dust-to-gas ratios. The large, volume-limited sample will robustly constrain the onset of mass-loss variations and asymmetry. All NESS data, including reduced data, catalogues, codes and model results will be publ	IRAS_215_a_06_7M	Kraemer, Kathleen; Kaminski, Tomasz; Shinnaga, Hiroko; Zijlstra, Albert; Do, Hoai; Haswell, Carole; Srinivasan, Sundar; Menten, Karl; Wouterloot, Jan; Dharmawardena, Thavisha; Pham, Tuan Anh; Kim, Hyosun; Lagadec, Eric; Feng, Siyi; Peeters, Els; McDonald, Iain; Cami, Jan; Hirano, Naomi; Wallström, Sofia; Kuan, Yi-Jehng; Hora, Joseph; Toala, Jesus; Lee, Chin-Fei; Jones, Olivia; Young, Ken; Matsuura, Mikako; Greaves, Jane; Marshall, Jonathan; Kemper, Ciska; Antoniou, Vallia; Imai, Hiroshi; Goldman, Steven; Trejo, Alfonso; Boyer, Martha; Patel, Nimesh; Friberg, Per; van Loon, Jacco; Liu, Tie; Liu, Sheng-Yuan;	22.223722138467267	0.6503334384452819	1.8	uid://A001/X14ed/X1dd	uid://A001/X14ed/X1de	uid://A002/Xf138ff/X155d	The Nearby Evolved Stars Survey: quantifying the gas and dust return to the Galactic interstellar medium	S	TARGET	T	30.035648394160216	T	2024A&A...682A.133K	Asymptotic Giant Branch (AGB) stars;null	Stars and stellar evolution	pscicluna	Scicluna, Peter	564.453125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00120.S	ALMA	JAO	ALMA	uid://A001/X14ed/X1de.source.IRAS_21543-1421.spw.22	cube	2		IRAS_21543-1421	329.2575833333389	-14.113372222222292	0.012282740404305971	Circle ICRS 329.257583 -14.113372 0.006141			2048	1	2	5.312298230431473	59487.086715	59487.090215	302.4	302.4	0.0013626953021969991	0.0013751915122301183	194869.95087182106	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14ed/X1de	application/x-votable+xml; content=datalink		2019.2.00120.S	Public	41.70500322347198	-47.410232808154696	6	7.056658755738825E-9	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N604:CM11	F	2022-11-04T19:43:08.000	5.312298230431473	[218.00..220.00GHz,1128.91kHz,17.5mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [219.89..220.89GHz,564.45kHz,22.8mJy/beam@10km/s,2mJy/beam@native, XX YY] U [230.03..231.03GHz,564.45kHz,22.2mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [231.50..233.50GHz,1128.91kHz,16.5mJy/beam@10km/s,1mJy/beam@native, XX YY]	219.00007096742186	735.6607732013813	ALMA	A radical transition in the post-main-sequence system U Equulei	Kamiński, Tomek	Kamiński, Tomek; Schmidt, Mirek R.; Djupvik, Anlaug Amanda; Menten, Karl M.; Kraus, Alex; Iłkiewicz, Krystian; Steinmetz, Thomas; Mobeen, Muhammad Zain; Szczerba, Ryszard	Context. U Equ is an unusual maser-hosting infrared source discovered in the 1990s. It was tentatively classified as a post-asymptotic giant branch (post-AGB) star with a unique optical spectrum displaying rare emission and absorption features from molecular gas at a temperature of about 500 K. In 2022, we serendipitously discovered that its optical spectrum had drastically changed since the last observations in the 1990s. <BR /> Aims: We aim to characterize the drastic change in the spectrum and analyze the photometric behavior of the object since 1989. <BR /> Methods: Optical high-resolution spectra of U Equ from the Southern African Large Telescope were supplemented by archival data and near-infrared photometry from the Nordic Optical Telescope. New spectral line observations with the Effelsberg 100 m radio telescope and Atacam Large Millimeter Array are presented. Radiative transfer modeling of multiple epoch spectral energy distributions was performed. <BR /> Results: No circumstellar molecular features	2024	Outflows of asymptotic giant branch and red supergiant stars drive local galactic chemical evolution. The Nearby Evolved Stars Survey (NESS) is a global project targeting a volume-limited sample of evolved stars within 2 kpc to constrain the physics driving mass loss. NESS includes ongoing JCMT (515 hr) and APEX (56 hr) surveys to observe CO(2-1), CO(3-2) and dust continuum from ~500 sources, and at the Nobeyama observatory (190 hr) for CO(1-0). We propose 12CO and 13CO(2-1) and (3-2) observations of the 280 NESS sources visible to the ACA that do not have archival data (total sample 301 sources). Combining the high resolution and large field-of-view of the ACA with data from the JCMT and APEX, we will thoroughly probe their inner shells, revealing the mass-loss history, geometry and the 12C/13C and dust-to-gas ratios. The large, volume-limited sample will robustly constrain the onset of mass-loss variations and asymmetry. All NESS data, including reduced data, catalogues, codes and model results will be publ	IRAS_215_a_06_7M	Kraemer, Kathleen; Kaminski, Tomasz; Shinnaga, Hiroko; Zijlstra, Albert; Do, Hoai; Haswell, Carole; Srinivasan, Sundar; Menten, Karl; Wouterloot, Jan; Dharmawardena, Thavisha; Pham, Tuan Anh; Kim, Hyosun; Lagadec, Eric; Feng, Siyi; Peeters, Els; McDonald, Iain; Cami, Jan; Hirano, Naomi; Wallström, Sofia; Kuan, Yi-Jehng; Hora, Joseph; Toala, Jesus; Lee, Chin-Fei; Jones, Olivia; Young, Ken; Matsuura, Mikako; Greaves, Jane; Marshall, Jonathan; Kemper, Ciska; Antoniou, Vallia; Imai, Hiroshi; Goldman, Steven; Trejo, Alfonso; Boyer, Martha; Patel, Nimesh; Friberg, Per; van Loon, Jacco; Liu, Tie; Liu, Sheng-Yuan;	17.517449744269666	0.6503334384452819	1.8	uid://A001/X14ed/X1dd	uid://A001/X14ed/X1de	uid://A002/Xf138ff/X155d	The Nearby Evolved Stars Survey: quantifying the gas and dust return to the Galactic interstellar medium	S	TARGET	T	30.035648394160216	T	2024A&A...682A.133K	Asymptotic Giant Branch (AGB) stars;null	Stars and stellar evolution	pscicluna	Scicluna, Peter	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00120.S	ALMA	JAO	ALMA	uid://A001/X14ed/X1de.source.IRAS_21543-1421.spw.18	cube	2		IRAS_21543-1421	329.2575833333389	-14.113372222222292	0.012282740404305971	Circle ICRS 329.257583 -14.113372 0.006141			2048	1	2	5.312298230431473	59487.086715	59487.090215	302.4	302.4	0.001283906535528862	0.0012949936214467616	205057.66375568783	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14ed/X1de	application/x-votable+xml; content=datalink		2019.2.00120.S	Public	41.70500322347198	-47.410232808154696	6	6.26092084806635E-9	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N604:CM11	F	2022-11-04T19:43:08.000	5.312298230431473	[218.00..220.00GHz,1128.91kHz,17.5mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [219.89..220.89GHz,564.45kHz,22.8mJy/beam@10km/s,2mJy/beam@native, XX YY] U [230.03..231.03GHz,564.45kHz,22.2mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [231.50..233.50GHz,1128.91kHz,16.5mJy/beam@10km/s,1mJy/beam@native, XX YY]	232.50066371905282	735.6607732013813	ALMA	A radical transition in the post-main-sequence system U Equulei	Kamiński, Tomek	Kamiński, Tomek; Schmidt, Mirek R.; Djupvik, Anlaug Amanda; Menten, Karl M.; Kraus, Alex; Iłkiewicz, Krystian; Steinmetz, Thomas; Mobeen, Muhammad Zain; Szczerba, Ryszard	Context. U Equ is an unusual maser-hosting infrared source discovered in the 1990s. It was tentatively classified as a post-asymptotic giant branch (post-AGB) star with a unique optical spectrum displaying rare emission and absorption features from molecular gas at a temperature of about 500 K. In 2022, we serendipitously discovered that its optical spectrum had drastically changed since the last observations in the 1990s. <BR /> Aims: We aim to characterize the drastic change in the spectrum and analyze the photometric behavior of the object since 1989. <BR /> Methods: Optical high-resolution spectra of U Equ from the Southern African Large Telescope were supplemented by archival data and near-infrared photometry from the Nordic Optical Telescope. New spectral line observations with the Effelsberg 100 m radio telescope and Atacam Large Millimeter Array are presented. Radiative transfer modeling of multiple epoch spectral energy distributions was performed. <BR /> Results: No circumstellar molecular features	2024	Outflows of asymptotic giant branch and red supergiant stars drive local galactic chemical evolution. The Nearby Evolved Stars Survey (NESS) is a global project targeting a volume-limited sample of evolved stars within 2 kpc to constrain the physics driving mass loss. NESS includes ongoing JCMT (515 hr) and APEX (56 hr) surveys to observe CO(2-1), CO(3-2) and dust continuum from ~500 sources, and at the Nobeyama observatory (190 hr) for CO(1-0). We propose 12CO and 13CO(2-1) and (3-2) observations of the 280 NESS sources visible to the ACA that do not have archival data (total sample 301 sources). Combining the high resolution and large field-of-view of the ACA with data from the JCMT and APEX, we will thoroughly probe their inner shells, revealing the mass-loss history, geometry and the 12C/13C and dust-to-gas ratios. The large, volume-limited sample will robustly constrain the onset of mass-loss variations and asymmetry. All NESS data, including reduced data, catalogues, codes and model results will be publ	IRAS_215_a_06_7M	Kraemer, Kathleen; Kaminski, Tomasz; Shinnaga, Hiroko; Zijlstra, Albert; Do, Hoai; Haswell, Carole; Srinivasan, Sundar; Menten, Karl; Wouterloot, Jan; Dharmawardena, Thavisha; Pham, Tuan Anh; Kim, Hyosun; Lagadec, Eric; Feng, Siyi; Peeters, Els; McDonald, Iain; Cami, Jan; Hirano, Naomi; Wallström, Sofia; Kuan, Yi-Jehng; Hora, Joseph; Toala, Jesus; Lee, Chin-Fei; Jones, Olivia; Young, Ken; Matsuura, Mikako; Greaves, Jane; Marshall, Jonathan; Kemper, Ciska; Antoniou, Vallia; Imai, Hiroshi; Goldman, Steven; Trejo, Alfonso; Boyer, Martha; Patel, Nimesh; Friberg, Per; van Loon, Jacco; Liu, Tie; Liu, Sheng-Yuan;	16.494175711225548	0.6503334384452819	1.8	uid://A001/X14ed/X1dd	uid://A001/X14ed/X1de	uid://A002/Xf138ff/X155d	The Nearby Evolved Stars Survey: quantifying the gas and dust return to the Galactic interstellar medium	S	TARGET	T	30.035648394160216	T	2024A&A...682A.133K	Asymptotic Giant Branch (AGB) stars;null	Stars and stellar evolution	pscicluna	Scicluna, Peter	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00869.L	ALMA	JAO	ALMA	uid://A001/X1590/X18e8.source.ad3a-22755.spw.31	cube	2		ad3a-22755	243.43989166665915	-51.82186111111131	0.0188014607347378	Circle ICRS 243.439892 -51.821861 0.009401			3840	1	2	3.3835396062184175	59643.402306	59643.402726	36.288	36.288	0.0034082285853065286	0.0034449320294098044	298527.7315427542	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X18e8	application/x-votable+xml; content=datalink		2021.1.00869.L	Public	331.4554250377973	-0.5231128907039242	3	1.1540802030481397E-8	9.375E8	A001:DA57 A003:DV18 A005:DV13 A006:DV17 A008:DV24 A009:DV11 A010:DV15 A011:DV25 A013:DA43 A015:DV21 A016:DA61 A017:DV16 A019:DV14 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A028:PM03 A030:DA41 A031:DA59 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A038:DV22 A039:DV23 A040:DA50 A041:DV05 A042:DA60 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A049:DA44 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A072:DA53	F	2023-03-22T03:31:24.000	3.3835396062184175	[84.10..85.04GHz,294.68kHz,4.4mJy/beam@10km/s,243.6uJy/beam@native, XX YY] U [84.93..85.87GHz,294.68kHz,4.4mJy/beam@10km/s,243.6uJy/beam@native, XX YY] U [86.08..87.01GHz,294.68kHz,4.5mJy/beam@10km/s,248.7uJy/beam@native, XX YY] U [87.02..87.96GHz,294.68kHz,4.5mJy/beam@10km/s,248.7uJy/beam@native, XX YY]	87.49278593978073	1004.2365459674712	ALMA						A radio survey of red giant SiO sources in the inner Galaxy and Bulge is not hindered by extinction. Extremely accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<<1 min) per source. Our aim to collect 20000 SiO maser velocities yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy and Plane. Large samples reveal dynamical structures and minority populations, and their velocity structure may be compared with kinematics of molecular gas, complex orbits in the bar, or stellar streams resulting from recently captured systems. From existing data we collected ~12000 stellar velocities, almost exclusively in the northern Bulge. ALMA is the only instrument that can efficiently add measurements to the undersampled southern Bulge region (-11070% detection rate). We propose to use ALMA to survey 6000 sources in ~120h to obtain 4200+ data points in the undersampled Southern Bulge as part of this larger NSF-	ad3a-229_b_03_TM1	Habing, Harm; Quiroga Nunez, Luis Henry; Stroh, Michael; Lewis, Megan; van Langevelde, Huib; Claussen, Mark; Pihlstrom, Ylva;	4.4579476554027675	0.12305379779327583	5.4306846	uid://A001/X1590/X18e7	uid://A001/X1590/X18e8	uid://A002/Xf5e73e/X208d	Bulge symmetry or not? The hidden dynamics of the Far Side	L	TARGET	T	30.76370182901878	T		Spiral galaxies;Galactic centres/nuclei	Local Universe	lsjouwerman	Sjouwerman, Lorant	294.677734375	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00869.L	ALMA	JAO	ALMA	uid://A001/X1590/X18e8.source.ad3a-22755.spw.29	cube	2		ad3a-22755	243.43989166665915	-51.82186111111131	0.0188014607347378	Circle ICRS 243.439892 -51.821861 0.009401			3840	1	2	3.3835396062184175	59643.402306	59643.402726	36.288	36.288	0.003445340037655819	0.0034828515436770365	295312.14249696926	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X18e8	application/x-votable+xml; content=datalink		2021.1.00869.L	Public	331.4554250377973	-0.5231128907039242	3	1.1794883979769123E-8	9.375E8	A001:DA57 A003:DV18 A005:DV13 A006:DV17 A008:DV24 A009:DV11 A010:DV15 A011:DV25 A013:DA43 A015:DV21 A016:DA61 A017:DV16 A019:DV14 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A028:PM03 A030:DA41 A031:DA59 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A038:DV22 A039:DV23 A040:DA50 A041:DV05 A042:DA60 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A049:DA44 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A072:DA53	F	2023-03-22T03:31:24.000	3.3835396062184175	[84.10..85.04GHz,294.68kHz,4.4mJy/beam@10km/s,243.6uJy/beam@native, XX YY] U [84.93..85.87GHz,294.68kHz,4.4mJy/beam@10km/s,243.6uJy/beam@native, XX YY] U [86.08..87.01GHz,294.68kHz,4.5mJy/beam@10km/s,248.7uJy/beam@native, XX YY] U [87.02..87.96GHz,294.68kHz,4.5mJy/beam@10km/s,248.7uJy/beam@native, XX YY]	86.54531074679875	1004.2365459674712	ALMA						A radio survey of red giant SiO sources in the inner Galaxy and Bulge is not hindered by extinction. Extremely accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<<1 min) per source. Our aim to collect 20000 SiO maser velocities yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy and Plane. Large samples reveal dynamical structures and minority populations, and their velocity structure may be compared with kinematics of molecular gas, complex orbits in the bar, or stellar streams resulting from recently captured systems. From existing data we collected ~12000 stellar velocities, almost exclusively in the northern Bulge. ALMA is the only instrument that can efficiently add measurements to the undersampled southern Bulge region (-11070% detection rate). We propose to use ALMA to survey 6000 sources in ~120h to obtain 4200+ data points in the undersampled Southern Bulge as part of this larger NSF-	ad3a-229_b_03_TM1	Habing, Harm; Quiroga Nunez, Luis Henry; Stroh, Michael; Lewis, Megan; van Langevelde, Huib; Claussen, Mark; Pihlstrom, Ylva;	4.481471869269032	0.12305379779327583	5.4306846	uid://A001/X1590/X18e7	uid://A001/X1590/X18e8	uid://A002/Xf5e73e/X208d	Bulge symmetry or not? The hidden dynamics of the Far Side	L	TARGET	T	30.76370182901878	T		Spiral galaxies;Galactic centres/nuclei	Local Universe	lsjouwerman	Sjouwerman, Lorant	294.677734375	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00869.L	ALMA	JAO	ALMA	uid://A001/X1590/X18e8.source.ad3a-22755.spw.25	cube	2		ad3a-22755	243.43989166665915	-51.82186111111131	0.0188014607347378	Circle ICRS 243.439892 -51.821861 0.009401			3840	1	2	3.3835396062184175	59643.402306	59643.402726	36.288	36.288	0.0035255014244695354	0.003564788720202428	288597.4576804544	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X18e8	application/x-votable+xml; content=datalink		2021.1.00869.L	Public	331.4554250377973	-0.5231128907039242	3	1.2353252220431992E-8	9.375E8	A001:DA57 A003:DV18 A005:DV13 A006:DV17 A008:DV24 A009:DV11 A010:DV15 A011:DV25 A013:DA43 A015:DV21 A016:DA61 A017:DV16 A019:DV14 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A028:PM03 A030:DA41 A031:DA59 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A038:DV22 A039:DV23 A040:DA50 A041:DV05 A042:DA60 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A049:DA44 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A072:DA53	F	2023-03-22T03:31:24.000	3.3835396062184175	[84.10..85.04GHz,294.68kHz,4.4mJy/beam@10km/s,243.6uJy/beam@native, XX YY] U [84.93..85.87GHz,294.68kHz,4.4mJy/beam@10km/s,243.6uJy/beam@native, XX YY] U [86.08..87.01GHz,294.68kHz,4.5mJy/beam@10km/s,248.7uJy/beam@native, XX YY] U [87.02..87.96GHz,294.68kHz,4.5mJy/beam@10km/s,248.7uJy/beam@native, XX YY]	84.56682493852055	1004.2365459674712	ALMA						A radio survey of red giant SiO sources in the inner Galaxy and Bulge is not hindered by extinction. Extremely accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<<1 min) per source. Our aim to collect 20000 SiO maser velocities yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy and Plane. Large samples reveal dynamical structures and minority populations, and their velocity structure may be compared with kinematics of molecular gas, complex orbits in the bar, or stellar streams resulting from recently captured systems. From existing data we collected ~12000 stellar velocities, almost exclusively in the northern Bulge. ALMA is the only instrument that can efficiently add measurements to the undersampled southern Bulge region (-11070% detection rate). We propose to use ALMA to survey 6000 sources in ~120h to obtain 4200+ data points in the undersampled Southern Bulge as part of this larger NSF-	ad3a-229_b_03_TM1	Habing, Harm; Quiroga Nunez, Luis Henry; Stroh, Michael; Lewis, Megan; van Langevelde, Huib; Claussen, Mark; Pihlstrom, Ylva;	4.440382210619936	0.12305379779327583	5.4306846	uid://A001/X1590/X18e7	uid://A001/X1590/X18e8	uid://A002/Xf5e73e/X208d	Bulge symmetry or not? The hidden dynamics of the Far Side	L	TARGET	T	30.76370182901878	T		Spiral galaxies;Galactic centres/nuclei	Local Universe	lsjouwerman	Sjouwerman, Lorant	294.677734375	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00869.L	ALMA	JAO	ALMA	uid://A001/X1590/X18e8.source.ad3a-22755.spw.27	cube	2		ad3a-22755	243.43989166665915	-51.82186111111131	0.0188014607347378	Circle ICRS 243.439892 -51.821861 0.009401			3840	1	2	3.3835396062184175	59643.402306	59643.402726	36.288	36.288	0.0034913524352269947	0.003529878163139243	291420.23528901563	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X18e8	application/x-votable+xml; content=datalink		2021.1.00869.L	Public	331.4554250377973	-0.5231128907039242	3	1.2113789585096903E-8	9.375E8	A001:DA57 A003:DV18 A005:DV13 A006:DV17 A008:DV24 A009:DV11 A010:DV15 A011:DV25 A013:DA43 A015:DV21 A016:DA61 A017:DV16 A019:DV14 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A028:PM03 A030:DA41 A031:DA59 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A038:DV22 A039:DV23 A040:DA50 A041:DV05 A042:DA60 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A049:DA44 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A072:DA53	F	2023-03-22T03:31:24.000	3.3835396062184175	[84.10..85.04GHz,294.68kHz,4.4mJy/beam@10km/s,243.6uJy/beam@native, XX YY] U [84.93..85.87GHz,294.68kHz,4.4mJy/beam@10km/s,243.6uJy/beam@native, XX YY] U [86.08..87.01GHz,294.68kHz,4.5mJy/beam@10km/s,248.7uJy/beam@native, XX YY] U [87.02..87.96GHz,294.68kHz,4.5mJy/beam@10km/s,248.7uJy/beam@native, XX YY]	85.39855801178825	1004.2365459674712	ALMA						A radio survey of red giant SiO sources in the inner Galaxy and Bulge is not hindered by extinction. Extremely accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<<1 min) per source. Our aim to collect 20000 SiO maser velocities yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy and Plane. Large samples reveal dynamical structures and minority populations, and their velocity structure may be compared with kinematics of molecular gas, complex orbits in the bar, or stellar streams resulting from recently captured systems. From existing data we collected ~12000 stellar velocities, almost exclusively in the northern Bulge. ALMA is the only instrument that can efficiently add measurements to the undersampled southern Bulge region (-11070% detection rate). We propose to use ALMA to survey 6000 sources in ~120h to obtain 4200+ data points in the undersampled Southern Bulge as part of this larger NSF-	ad3a-229_b_03_TM1	Habing, Harm; Quiroga Nunez, Luis Henry; Stroh, Michael; Lewis, Megan; van Langevelde, Huib; Claussen, Mark; Pihlstrom, Ylva;	4.419391924075262	0.12305379779327583	5.4306846	uid://A001/X1590/X18e7	uid://A001/X1590/X18e8	uid://A002/Xf5e73e/X208d	Bulge symmetry or not? The hidden dynamics of the Far Side	L	TARGET	T	30.76370182901878	T		Spiral galaxies;Galactic centres/nuclei	Local Universe	lsjouwerman	Sjouwerman, Lorant	294.677734375	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2013.1.01142.S	ALMA	JAO	ALMA	uid://A001/X130/X16.source.m33-2.spw.21	image	2	ari_l	m33-2	23.4945625	30.812383888888892	0.017209832374936656	Circle ICRS 23.494563 30.812384 0.008605			128	1	2	0.5691330755082806	56884.419374	57251.283574	72.576	72.576	0.00299857541029807	0.0030592917564787802	3199.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X130/X16	application/x-votable+xml; content=datalink		2013.1.01142.S	Public	133.608108502197	-31.175892959651787	3	9.562362216247847E-7	2.0E9	A007:DV23 A011:DV04 A011:DV22 A019:DA63 A021:DA59 A029:DA49 A031:DV11 A033:DV18 A058:DA46 A060:DA55 A062:DV05 A063:DA54 A064:DA50 A064:DA56 A069:DA53 A072:DV01 A073:DA63 A074:DA47 A075:DA61 A076:DV13 A077:DV16 A077:DV19 A078:DV04 A078:DV15 A079:DA41 A079:DA43 A080:DA55 A080:DV24 A081:DA42 A082:DA42 A082:DA51 A083:DV14 A083:DV25 A084:DV06 A085:DA64 A086:DV07 A086:DV14 A087:DV02 A087:DV23 A088:DV20 A089:DA60 A089:DV15 A090:DA54 A090:DA60 A091:DA43 A091:DA58 A092:DV12 A093:DV21 A093:DV24 A094:DV02 A096:DV10 A097:DA62 A097:DV13 A101:DA47 A101:DA62 A103:DA65 A103:DV03 A104:DA44 A105:DA52 A110:DV22 A112:DV07 A113:DA57 A115:DV11 A135:DV10 A136:DV17 A137:DA41 A138:DV17 T701:PM03 T702:PM02	F	2016-11-26T00:13:13.000	0.5691330755082806	[86.00..87.98GHz,31250.00kHz,5.6mJy/beam@10km/s,214.1uJy/beam@native, XX YY] U [87.93..89.92GHz,31250.00kHz,5.5mJy/beam@10km/s,213uJy/beam@native, XX YY] U [97.99..99.98GHz,31250.00kHz,5.3mJy/beam@10km/s,213.5uJy/beam@native, XX YY] U [99.99..101.98GHz,31250.00kHz,5.2mJy/beam@10km/s,212.8uJy/beam@native, XX YY]	98.98618389508091	91860.10108419709	ALMA						We propose 100GHz-band continuum observations at 8pc resolution toward the 75 giant molecular clouds (GMCs) in the nearest spiral galaxy, M33, for the purpose of searching for obscured young clusters. Radio emission at around 100GHz from star-forming galaxies is expected to be strongly dominated by the free-free bremsstrahlung component due to ionizing radiation from massive, short-lived stars. Many studies on external galaxies have widely used the 24micron dust emission as the tracer for obscured star formation. However, the spatial resolution of 24micron data is limited to, for example in case of Spitzer, 6 arcsec. This is not comparable that of the molecular gas images anymore, which can be resolved at sub-arcsec resolution in the ALMA era. With the 100GHz-band continuum data, we aim to obtain a catalog of the obscured star clusters in the GMCs, including size, cluster mass and accurate star formation efficiencies out of a parental GMC. We also check the validity of the star formation rate (SFR) from the t	m33-1_a_03_TE	Espada, Daniel; Tosaki, Tomoka; Komugi, Shinya; Onodera, Sachiko; Kuno, Nario; Hirota, Akihiko;	5.254201753301263	0.10667990643204601	1.6067636	uid://A001/X130/X15	uid://A001/X130/X16	uid://A002/X8952b5/X2e	Embedded young cluster survey in the Giant Molecular Clouds in the Nearby Spiral Galaxy M33	S	TARGET	T	9.452822073460863	T		Starbursts, star formation;Giant Molecular Clouds (GMC) properties	Active galaxies	rmiura	Miura, Rie	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2013.1.01142.S	ALMA	JAO	ALMA	uid://A001/X130/X16.source.m33-2.spw.19	image	2	ari_l	m33-2	23.4945625	30.812383888888892	0.017209832374936656	Circle ICRS 23.494563 30.812384 0.008605			128	1	2	0.5691330755082806	56884.419374	57251.283574	72.576	72.576	0.0033341151659466006	0.0034093504633376866	2877.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X130/X16	application/x-votable+xml; content=datalink		2013.1.01142.S	Public	133.608108502197	-31.175892959651787	3	1.1848996262358913E-6	2.0E9	A007:DV23 A011:DV04 A011:DV22 A019:DA63 A021:DA59 A029:DA49 A031:DV11 A033:DV18 A058:DA46 A060:DA55 A062:DV05 A063:DA54 A064:DA50 A064:DA56 A069:DA53 A072:DV01 A073:DA63 A074:DA47 A075:DA61 A076:DV13 A077:DV16 A077:DV19 A078:DV04 A078:DV15 A079:DA41 A079:DA43 A080:DA55 A080:DV24 A081:DA42 A082:DA42 A082:DA51 A083:DV14 A083:DV25 A084:DV06 A085:DA64 A086:DV07 A086:DV14 A087:DV02 A087:DV23 A088:DV20 A089:DA60 A089:DV15 A090:DA54 A090:DA60 A091:DA43 A091:DA58 A092:DV12 A093:DV21 A093:DV24 A094:DV02 A096:DV10 A097:DA62 A097:DV13 A101:DA47 A101:DA62 A103:DA65 A103:DV03 A104:DA44 A105:DA52 A110:DV22 A112:DV07 A113:DA57 A115:DV11 A135:DV10 A136:DV17 A137:DA41 A138:DV17 T701:PM03 T702:PM02	F	2016-11-26T00:13:13.000	0.5691330755082806	[86.00..87.98GHz,31250.00kHz,5.6mJy/beam@10km/s,214.1uJy/beam@native, XX YY] U [87.93..89.92GHz,31250.00kHz,5.5mJy/beam@10km/s,213uJy/beam@native, XX YY] U [97.99..99.98GHz,31250.00kHz,5.3mJy/beam@10km/s,213.5uJy/beam@native, XX YY] U [99.99..101.98GHz,31250.00kHz,5.2mJy/beam@10km/s,212.8uJy/beam@native, XX YY]	88.924536833798	91860.10108419709	ALMA						We propose 100GHz-band continuum observations at 8pc resolution toward the 75 giant molecular clouds (GMCs) in the nearest spiral galaxy, M33, for the purpose of searching for obscured young clusters. Radio emission at around 100GHz from star-forming galaxies is expected to be strongly dominated by the free-free bremsstrahlung component due to ionizing radiation from massive, short-lived stars. Many studies on external galaxies have widely used the 24micron dust emission as the tracer for obscured star formation. However, the spatial resolution of 24micron data is limited to, for example in case of Spitzer, 6 arcsec. This is not comparable that of the molecular gas images anymore, which can be resolved at sub-arcsec resolution in the ALMA era. With the 100GHz-band continuum data, we aim to obtain a catalog of the obscured star clusters in the GMCs, including size, cluster mass and accurate star formation efficiencies out of a parental GMC. We also check the validity of the star formation rate (SFR) from the t	m33-1_a_03_TE	Espada, Daniel; Tosaki, Tomoka; Komugi, Shinya; Onodera, Sachiko; Kuno, Nario; Hirota, Akihiko;	5.531991796568913	0.10667990643204601	1.6067636	uid://A001/X130/X15	uid://A001/X130/X16	uid://A002/X8952b5/X2e	Embedded young cluster survey in the Giant Molecular Clouds in the Nearby Spiral Galaxy M33	S	TARGET	T	9.452822073460863	T		Starbursts, star formation;Giant Molecular Clouds (GMC) properties	Active galaxies	rmiura	Miura, Rie	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2013.1.01142.S	ALMA	JAO	ALMA	uid://A001/X130/X16.source.m33-2.spw.23	image	2	ari_l	m33-2	23.4945625	30.812383888888892	0.017209832374936656	Circle ICRS 23.494563 30.812384 0.008605			128	1	2	0.5691330755082806	56884.419374	57251.283574	72.576	72.576	0.0029397721825694116	0.0029981073821261418	3263.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X130/X16	application/x-votable+xml; content=datalink		2013.1.01142.S	Public	133.608108502197	-31.175892959651787	3	9.187348246193239E-7	2.0E9	A007:DV23 A011:DV04 A011:DV22 A019:DA63 A021:DA59 A029:DA49 A031:DV11 A033:DV18 A058:DA46 A060:DA55 A062:DV05 A063:DA54 A064:DA50 A064:DA56 A069:DA53 A072:DV01 A073:DA63 A074:DA47 A075:DA61 A076:DV13 A077:DV16 A077:DV19 A078:DV04 A078:DV15 A079:DA41 A079:DA43 A080:DA55 A080:DV24 A081:DA42 A082:DA42 A082:DA51 A083:DV14 A083:DV25 A084:DV06 A085:DA64 A086:DV07 A086:DV14 A087:DV02 A087:DV23 A088:DV20 A089:DA60 A089:DV15 A090:DA54 A090:DA60 A091:DA43 A091:DA58 A092:DV12 A093:DV21 A093:DV24 A094:DV02 A096:DV10 A097:DA62 A097:DV13 A101:DA47 A101:DA62 A103:DA65 A103:DV03 A104:DA44 A105:DA52 A110:DV22 A112:DV07 A113:DA57 A115:DV11 A135:DV10 A136:DV17 A137:DA41 A138:DV17 T701:PM03 T702:PM02	F	2016-11-26T00:13:13.000	0.5691330755082806	[86.00..87.98GHz,31250.00kHz,5.6mJy/beam@10km/s,214.1uJy/beam@native, XX YY] U [87.93..89.92GHz,31250.00kHz,5.5mJy/beam@10km/s,213uJy/beam@native, XX YY] U [97.99..99.98GHz,31250.00kHz,5.3mJy/beam@10km/s,213.5uJy/beam@native, XX YY] U [99.99..101.98GHz,31250.00kHz,5.2mJy/beam@10km/s,212.8uJy/beam@native, XX YY]	100.9860143668887	91860.10108419709	ALMA						We propose 100GHz-band continuum observations at 8pc resolution toward the 75 giant molecular clouds (GMCs) in the nearest spiral galaxy, M33, for the purpose of searching for obscured young clusters. Radio emission at around 100GHz from star-forming galaxies is expected to be strongly dominated by the free-free bremsstrahlung component due to ionizing radiation from massive, short-lived stars. Many studies on external galaxies have widely used the 24micron dust emission as the tracer for obscured star formation. However, the spatial resolution of 24micron data is limited to, for example in case of Spitzer, 6 arcsec. This is not comparable that of the molecular gas images anymore, which can be resolved at sub-arcsec resolution in the ALMA era. With the 100GHz-band continuum data, we aim to obtain a catalog of the obscured star clusters in the GMCs, including size, cluster mass and accurate star formation efficiencies out of a parental GMC. We also check the validity of the star formation rate (SFR) from the t	m33-1_a_03_TE	Espada, Daniel; Tosaki, Tomoka; Komugi, Shinya; Onodera, Sachiko; Kuno, Nario; Hirota, Akihiko;	5.186332024053825	0.10667990643204601	1.6067636	uid://A001/X130/X15	uid://A001/X130/X16	uid://A002/X8952b5/X2e	Embedded young cluster survey in the Giant Molecular Clouds in the Nearby Spiral Galaxy M33	S	TARGET	T	9.452822073460863	T		Starbursts, star formation;Giant Molecular Clouds (GMC) properties	Active galaxies	rmiura	Miura, Rie	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2013.1.01142.S	ALMA	JAO	ALMA	uid://A001/X130/X16.source.m33-2.spw.17	image	2	ari_l	m33-2	23.4945625	30.812383888888892	0.017209832374936656	Circle ICRS 23.494563 30.812384 0.008605			128	1	2	0.5691330755082806	56884.419374	57251.283574	72.576	72.576	0.003407533575153572	0.003486157825490473	2815.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X130/X16	application/x-votable+xml; content=datalink		2013.1.01142.S	Public	133.608108502197	-31.175892959651787	3	1.2382732955796993E-6	2.0E9	A007:DV23 A011:DV04 A011:DV22 A019:DA63 A021:DA59 A029:DA49 A031:DV11 A033:DV18 A058:DA46 A060:DA55 A062:DV05 A063:DA54 A064:DA50 A064:DA56 A069:DA53 A072:DV01 A073:DA63 A074:DA47 A075:DA61 A076:DV13 A077:DV16 A077:DV19 A078:DV04 A078:DV15 A079:DA41 A079:DA43 A080:DA55 A080:DV24 A081:DA42 A082:DA42 A082:DA51 A083:DV14 A083:DV25 A084:DV06 A085:DA64 A086:DV07 A086:DV14 A087:DV02 A087:DV23 A088:DV20 A089:DA60 A089:DV15 A090:DA54 A090:DA60 A091:DA43 A091:DA58 A092:DV12 A093:DV21 A093:DV24 A094:DV02 A096:DV10 A097:DA62 A097:DV13 A101:DA47 A101:DA62 A103:DA65 A103:DV03 A104:DA44 A105:DA52 A110:DV22 A112:DV07 A113:DA57 A115:DV11 A135:DV10 A136:DV17 A137:DA41 A138:DV17 T701:PM03 T702:PM02	F	2016-11-26T00:13:13.000	0.5691330755082806	[86.00..87.98GHz,31250.00kHz,5.6mJy/beam@10km/s,214.1uJy/beam@native, XX YY] U [87.93..89.92GHz,31250.00kHz,5.5mJy/beam@10km/s,213uJy/beam@native, XX YY] U [97.99..99.98GHz,31250.00kHz,5.3mJy/beam@10km/s,213.5uJy/beam@native, XX YY] U [99.99..101.98GHz,31250.00kHz,5.2mJy/beam@10km/s,212.8uJy/beam@native, XX YY]	86.9872010642342	91860.10108419709	ALMA						We propose 100GHz-band continuum observations at 8pc resolution toward the 75 giant molecular clouds (GMCs) in the nearest spiral galaxy, M33, for the purpose of searching for obscured young clusters. Radio emission at around 100GHz from star-forming galaxies is expected to be strongly dominated by the free-free bremsstrahlung component due to ionizing radiation from massive, short-lived stars. Many studies on external galaxies have widely used the 24micron dust emission as the tracer for obscured star formation. However, the spatial resolution of 24micron data is limited to, for example in case of Spitzer, 6 arcsec. This is not comparable that of the molecular gas images anymore, which can be resolved at sub-arcsec resolution in the ALMA era. With the 100GHz-band continuum data, we aim to obtain a catalog of the obscured star clusters in the GMCs, including size, cluster mass and accurate star formation efficiencies out of a parental GMC. We also check the validity of the star formation rate (SFR) from the t	m33-1_a_03_TE	Espada, Daniel; Tosaki, Tomoka; Komugi, Shinya; Onodera, Sachiko; Kuno, Nario; Hirota, Akihiko;	5.620246212396848	0.10667990643204601	1.6067636	uid://A001/X130/X15	uid://A001/X130/X16	uid://A002/X8952b5/X2e	Embedded young cluster survey in the Giant Molecular Clouds in the Nearby Spiral Galaxy M33	S	TARGET	T	9.452822073460863	T		Starbursts, star formation;Giant Molecular Clouds (GMC) properties	Active galaxies	rmiura	Miura, Rie	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00478.S	ALMA	JAO	ALMA	uid://A001/X133d/X1d0e.source.ALMA_3mm_ID8.spw.29	cube	2		ALMA_3mm_ID8	150.09313999994433	2.52740830000167	0.01117065701276468	Circle ICRS 150.093140 2.527408 0.005585			240	1	2	1.6267198448429323	58566.999847	58567.027424	756	756	0.0019880950795759206	0.002013023074369828	19062.280258547697	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X1d0e	application/x-votable+xml; content=datalink		2018.1.00478.S	Public	236.44791675385477	42.28646686997679	4	1.042864986770104E-7	1.875E9	A001:DA44 A002:DA51 A003:DV12 A005:DA58 A006:DV25 A007:DV05 A010:DV13 A011:DV21 A015:DA64 A016:DV11 A017:DV14 A018:DA54 A019:DA61 A023:DA42 A024:DA49 A025:DA46 A026:DV19 A027:DV06 A030:DA62 A031:DA59 A033:DA53 A034:DA50 A035:DA43 A036:DA45 A038:DV24 A039:DA56 A040:DA55 A041:DA57 A042:DV08 A043:DA60 A044:DV03 A046:DA52 A048:DV02 A049:DA47 A058:DA41 A060:DV17 A062:DV10 A066:DV04 A068:DA65 A069:DV16 A072:DV20 A074:DV09 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2020-07-05T21:41:25.000	1.6267198448429323	[136.94..138.80GHz,7812.01kHz,809.8uJy/beam@10km/s,40.1uJy/beam@native, XX YY] U [138.81..140.67GHz,7812.01kHz,785.4uJy/beam@10km/s,39.2uJy/beam@native, XX YY] U [148.93..150.79GHz,7812.01kHz,760.9uJy/beam@10km/s,39.3uJy/beam@native, XX YY] U [150.79..152.66GHz,7812.01kHz,756.7uJy/beam@10km/s,39.3uJy/beam@native, XX YY]	149.86015593223672	15532.445883934306	ALMA	A<SUP>3</SUP>COSMOS and A<SUP>3</SUP>GOODSS: Continuum source catalogues and multi-band number counts A<SUP>3</SUP>COSMOS: Measuring the cosmic dust-attenuated star formation rate density at 4 < z < 5 A<SUP>3</SUP>COSMOS: The dust content of massive quiescent galaxies and its evolution with cosmic time ALMACAL. XI. Over-densities as signposts for proto-clusters? A cautionary tale CO in the ALMA Radio-source Catalogue (ARC): The molecular gas content of radio galaxies as a function of redshift The Evolution of the IR Luminosity Function and Dust-obscured Star Formation over the Past 13 Billion Years XLSSC 122 caught in the act of growing up: Spatially resolved SZ observations of a z = 1.98 galaxy cluster	Adscheid, Sylvia Audibert, A. Chen, Jianhang Magnelli, Benjamin Zavala, J. A. van Marrewijk, J.	Adscheid, Sylvia; Magnelli, Benjamin; Ciesla, Laure; Liu, Daizhong; Schinnerer, Eva; Bertoldi, Frank Adscheid, Sylvia; Magnelli, Benjamin; Liu, Daizhong; Bertoldi, Frank; Delvecchio, Ivan; Gruppioni, Carlotta; Schinnerer, Eva; Traina, Alberto; Béthermin, Matthieu; Gkogkou, Athanasia Audibert, A.; Dasyra, K. M.; Papachristou, M.; Fernández-Ontiveros, J. A.; Ruffa, I.; Bisigello, L.; Combes, F.; Salomé, P.; Gruppioni, C. Chen, Jianhang; Ivison, R. J.; Zwaan, Martin A.; Klitsch, Anne; Péroux, Céline; Lovell, Christopher C.; Lagos, Claudia del P.; Biggs, Andrew D.; Bollo, Victoria Magnelli, Benjamin; Adscheid, Sylvia; Wang, Tsan-Ming; Ciesla, Laure; Daddi, Emanuele; Delvecchio, Ivan; Elbaz, David; Fudamoto, Yoshinobu; Fukushima, Shuma; Franco, Maximilien; Gómez-Guijarro, Carlos; Gruppioni, Carlotta; Jiménez-Andrade, Eric F.; Liu, Daizhong; Oesch, Pascal; Schinnerer, Eva; Traina, Alberto Zavala, J. A.; Casey, C. M.; Manning, S. M.; Aravena, M.; Bethermin, M.; Caputi, K. I.; Clements, D. L.; Cunha, E. da; Drew, P.;	Aims. We study the dust content of massive (log(M<SUB>*</SUB>/M<SUB>⊙</SUB>)≥10.8) quiescent galaxies (QGs) at redshifts z = 0.5 − 3 to place constraints on the evolution of their cold interstellar medium (ISM) and thereby obtain insights into the processes of galaxy quenching throughout cosmic time. Methods. We used a robust sample of 458 colour-selected QGs covered by the A<SUP>3</SUP>COSMOS+A<SUP>3</SUP>GOODSS database to perform a stacking analysis in the uv domain and measured their mean dust masses from their stacked sub-millimetre luminosities. We used the CIGALE spectral energy distribution fitting code to obtain star formation histories and infer the time since quenching for all the QGs in our sample. We used this information to gain insight into the time evolution of the dust content after quenching. Results. Most QGs in our sample quenched around a redshift of z ∼ 1.3, following the peak of cosmic star formation. The majority of QGs observed at z &gt; 1 are recently quenched (i.e. quenched for no l	2021	At z>4, the largest submm/mm surveys are only sensitive to the most extreme dusty star-forming galaxies (SFR>1000 M_sun/yr). Less extreme sources can be detected in the deepest single-dish telescope surveys, however, the identified population of DSFGs are overwhelmed by the more abundant low-z population (not to mention their large positional uncertainties). Recent deep pencil-beam surveys from ALMA have also failed to detect high-z sources. We have analyzed, for the first time, the potential of 3mm observations to detect high-z DSFGs. This wavelength naturally filters out z<2 galaxies due to a very negative K-correction. We find 14 serendipitously-detected 3mm sources within ~160 sq. arcmin of ALMA archival observations. Three of them already have spectroscopic redshifts (z=2.5-4.5), which confirms their high-z nature. Here, we request 19h of observations (including overheads) to conduct a blind redshift survey for the remaining sources using an optimized band 3 + band 4 spectral setup. This work will reveal	ALMA_3mm_d_04_TM1	Champagne, Jaclyn; Staguhn, Johannes; Casey, Caitlin; da Cunha, Elisabete; Drew, Patrick; Manning, Sinclaire; Spilker, Justin; Hung, Chao-Ling; Hodge, Jacqueline; Finkelstein, Steven;	0.7608839298570271	0.019730578586167606	2.1842108	uid://A001/X133d/X1d0d	uid://A001/X133d/X1d0e	uid://A002/Xda0496/Xadc	On the nature of 3mm-selected sources: the highest redshift dusty star-forming galaxies?	S	TARGET	T	17.04038593462587	T	2021ApJ...909..165Z 2022A&A...668A..67A 2023A&A...675L..10C 2024A&A...685A...1A 2024A&A...688A..55M 2024A&A...689A..41V 2025A&A...702A.186A	Sub-mm Galaxies (SMG);null	Galaxy evolution	zavala	Zavala, Jorge	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00478.S	ALMA	JAO	ALMA	uid://A001/X133d/X1d0e.source.ALMA_3mm_ID8.spw.31	cube	2		ALMA_3mm_ID8	150.09313999994433	2.52740830000167	0.01117065701276468	Circle ICRS 150.093140 2.527408 0.005585			240	1	2	1.6267198448429323	58566.999847	58567.027424	756	756	0.001963801926507609	0.0019881207115074614	19301.046354205213	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X1d0e	application/x-votable+xml; content=datalink		2018.1.00478.S	Public	236.44791675385477	42.28646686997679	4	1.0173786382262252E-7	1.875E9	A001:DA44 A002:DA51 A003:DV12 A005:DA58 A006:DV25 A007:DV05 A010:DV13 A011:DV21 A015:DA64 A016:DV11 A017:DV14 A018:DA54 A019:DA61 A023:DA42 A024:DA49 A025:DA46 A026:DV19 A027:DV06 A030:DA62 A031:DA59 A033:DA53 A034:DA50 A035:DA43 A036:DA45 A038:DV24 A039:DA56 A040:DA55 A041:DA57 A042:DV08 A043:DA60 A044:DV03 A046:DA52 A048:DV02 A049:DA47 A058:DA41 A060:DV17 A062:DV10 A066:DV04 A068:DA65 A069:DV16 A072:DV20 A074:DV09 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2020-07-05T21:41:25.000	1.6267198448429323	[136.94..138.80GHz,7812.01kHz,809.8uJy/beam@10km/s,40.1uJy/beam@native, XX YY] U [138.81..140.67GHz,7812.01kHz,785.4uJy/beam@10km/s,39.2uJy/beam@native, XX YY] U [148.93..150.79GHz,7812.01kHz,760.9uJy/beam@10km/s,39.3uJy/beam@native, XX YY] U [150.79..152.66GHz,7812.01kHz,756.7uJy/beam@10km/s,39.3uJy/beam@native, XX YY]	151.72554641796165	15532.445883934306	ALMA	A<SUP>3</SUP>COSMOS and A<SUP>3</SUP>GOODSS: Continuum source catalogues and multi-band number counts A<SUP>3</SUP>COSMOS: Measuring the cosmic dust-attenuated star formation rate density at 4 < z < 5 A<SUP>3</SUP>COSMOS: The dust content of massive quiescent galaxies and its evolution with cosmic time ALMACAL. XI. Over-densities as signposts for proto-clusters? A cautionary tale CO in the ALMA Radio-source Catalogue (ARC): The molecular gas content of radio galaxies as a function of redshift The Evolution of the IR Luminosity Function and Dust-obscured Star Formation over the Past 13 Billion Years XLSSC 122 caught in the act of growing up: Spatially resolved SZ observations of a z = 1.98 galaxy cluster	Adscheid, Sylvia Audibert, A. Chen, Jianhang Magnelli, Benjamin Zavala, J. A. van Marrewijk, J.	Adscheid, Sylvia; Magnelli, Benjamin; Ciesla, Laure; Liu, Daizhong; Schinnerer, Eva; Bertoldi, Frank Adscheid, Sylvia; Magnelli, Benjamin; Liu, Daizhong; Bertoldi, Frank; Delvecchio, Ivan; Gruppioni, Carlotta; Schinnerer, Eva; Traina, Alberto; Béthermin, Matthieu; Gkogkou, Athanasia Audibert, A.; Dasyra, K. M.; Papachristou, M.; Fernández-Ontiveros, J. A.; Ruffa, I.; Bisigello, L.; Combes, F.; Salomé, P.; Gruppioni, C. Chen, Jianhang; Ivison, R. J.; Zwaan, Martin A.; Klitsch, Anne; Péroux, Céline; Lovell, Christopher C.; Lagos, Claudia del P.; Biggs, Andrew D.; Bollo, Victoria Magnelli, Benjamin; Adscheid, Sylvia; Wang, Tsan-Ming; Ciesla, Laure; Daddi, Emanuele; Delvecchio, Ivan; Elbaz, David; Fudamoto, Yoshinobu; Fukushima, Shuma; Franco, Maximilien; Gómez-Guijarro, Carlos; Gruppioni, Carlotta; Jiménez-Andrade, Eric F.; Liu, Daizhong; Oesch, Pascal; Schinnerer, Eva; Traina, Alberto Zavala, J. A.; Casey, C. M.; Manning, S. M.; Aravena, M.; Bethermin, M.; Caputi, K. I.; Clements, D. L.; Cunha, E. da; Drew, P.;	Aims. We study the dust content of massive (log(M<SUB>*</SUB>/M<SUB>⊙</SUB>)≥10.8) quiescent galaxies (QGs) at redshifts z = 0.5 − 3 to place constraints on the evolution of their cold interstellar medium (ISM) and thereby obtain insights into the processes of galaxy quenching throughout cosmic time. Methods. We used a robust sample of 458 colour-selected QGs covered by the A<SUP>3</SUP>COSMOS+A<SUP>3</SUP>GOODSS database to perform a stacking analysis in the uv domain and measured their mean dust masses from their stacked sub-millimetre luminosities. We used the CIGALE spectral energy distribution fitting code to obtain star formation histories and infer the time since quenching for all the QGs in our sample. We used this information to gain insight into the time evolution of the dust content after quenching. Results. Most QGs in our sample quenched around a redshift of z ∼ 1.3, following the peak of cosmic star formation. The majority of QGs observed at z &gt; 1 are recently quenched (i.e. quenched for no l	2021	At z>4, the largest submm/mm surveys are only sensitive to the most extreme dusty star-forming galaxies (SFR>1000 M_sun/yr). Less extreme sources can be detected in the deepest single-dish telescope surveys, however, the identified population of DSFGs are overwhelmed by the more abundant low-z population (not to mention their large positional uncertainties). Recent deep pencil-beam surveys from ALMA have also failed to detect high-z sources. We have analyzed, for the first time, the potential of 3mm observations to detect high-z DSFGs. This wavelength naturally filters out z<2 galaxies due to a very negative K-correction. We find 14 serendipitously-detected 3mm sources within ~160 sq. arcmin of ALMA archival observations. Three of them already have spectroscopic redshifts (z=2.5-4.5), which confirms their high-z nature. Here, we request 19h of observations (including overheads) to conduct a blind redshift survey for the remaining sources using an optimized band 3 + band 4 spectral setup. This work will reveal	ALMA_3mm_d_04_TM1	Champagne, Jaclyn; Staguhn, Johannes; Casey, Caitlin; da Cunha, Elisabete; Drew, Patrick; Manning, Sinclaire; Spilker, Justin; Hung, Chao-Ling; Hodge, Jacqueline; Finkelstein, Steven;	0.7566594288335727	0.019730578586167606	2.1842108	uid://A001/X133d/X1d0d	uid://A001/X133d/X1d0e	uid://A002/Xda0496/Xadc	On the nature of 3mm-selected sources: the highest redshift dusty star-forming galaxies?	S	TARGET	T	17.04038593462587	T	2021ApJ...909..165Z 2022A&A...668A..67A 2023A&A...675L..10C 2024A&A...685A...1A 2024A&A...688A..55M 2024A&A...689A..41V 2025A&A...702A.186A	Sub-mm Galaxies (SMG);null	Galaxy evolution	zavala	Zavala, Jorge	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00478.S	ALMA	JAO	ALMA	uid://A001/X133d/X1d0e.source.ALMA_3mm_ID8.spw.25	cube	2		ALMA_3mm_ID8	150.09313999994433	2.52740830000167	0.01117065701276468	Circle ICRS 150.093140 2.527408 0.005585			240	1	2	1.6267198448429323	58566.999847	58567.027424	756	756	0.002159831661369295	0.0021892842518019266	17766.57444971118	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X1d0e	application/x-votable+xml; content=datalink		2018.1.00478.S	Public	236.44791675385477	42.28646686997679	4	1.2321518672403775E-7	1.875E9	A001:DA44 A002:DA51 A003:DV12 A005:DA58 A006:DV25 A007:DV05 A010:DV13 A011:DV21 A015:DA64 A016:DV11 A017:DV14 A018:DA54 A019:DA61 A023:DA42 A024:DA49 A025:DA46 A026:DV19 A027:DV06 A030:DA62 A031:DA59 A033:DA53 A034:DA50 A035:DA43 A036:DA45 A038:DV24 A039:DA56 A040:DA55 A041:DA57 A042:DV08 A043:DA60 A044:DV03 A046:DA52 A048:DV02 A049:DA47 A058:DA41 A060:DV17 A062:DV10 A066:DV04 A068:DA65 A069:DV16 A072:DV20 A074:DV09 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2020-07-05T21:41:25.000	1.6267198448429323	[136.94..138.80GHz,7812.01kHz,809.8uJy/beam@10km/s,40.1uJy/beam@native, XX YY] U [138.81..140.67GHz,7812.01kHz,785.4uJy/beam@10km/s,39.2uJy/beam@native, XX YY] U [148.93..150.79GHz,7812.01kHz,760.9uJy/beam@10km/s,39.3uJy/beam@native, XX YY] U [150.79..152.66GHz,7812.01kHz,756.7uJy/beam@10km/s,39.3uJy/beam@native, XX YY]	137.869954926861	15532.445883934306	ALMA	A<SUP>3</SUP>COSMOS and A<SUP>3</SUP>GOODSS: Continuum source catalogues and multi-band number counts A<SUP>3</SUP>COSMOS: Measuring the cosmic dust-attenuated star formation rate density at 4 < z < 5 A<SUP>3</SUP>COSMOS: The dust content of massive quiescent galaxies and its evolution with cosmic time ALMACAL. XI. Over-densities as signposts for proto-clusters? A cautionary tale CO in the ALMA Radio-source Catalogue (ARC): The molecular gas content of radio galaxies as a function of redshift The Evolution of the IR Luminosity Function and Dust-obscured Star Formation over the Past 13 Billion Years XLSSC 122 caught in the act of growing up: Spatially resolved SZ observations of a z = 1.98 galaxy cluster	Adscheid, Sylvia Audibert, A. Chen, Jianhang Magnelli, Benjamin Zavala, J. A. van Marrewijk, J.	Adscheid, Sylvia; Magnelli, Benjamin; Ciesla, Laure; Liu, Daizhong; Schinnerer, Eva; Bertoldi, Frank Adscheid, Sylvia; Magnelli, Benjamin; Liu, Daizhong; Bertoldi, Frank; Delvecchio, Ivan; Gruppioni, Carlotta; Schinnerer, Eva; Traina, Alberto; Béthermin, Matthieu; Gkogkou, Athanasia Audibert, A.; Dasyra, K. M.; Papachristou, M.; Fernández-Ontiveros, J. A.; Ruffa, I.; Bisigello, L.; Combes, F.; Salomé, P.; Gruppioni, C. Chen, Jianhang; Ivison, R. J.; Zwaan, Martin A.; Klitsch, Anne; Péroux, Céline; Lovell, Christopher C.; Lagos, Claudia del P.; Biggs, Andrew D.; Bollo, Victoria Magnelli, Benjamin; Adscheid, Sylvia; Wang, Tsan-Ming; Ciesla, Laure; Daddi, Emanuele; Delvecchio, Ivan; Elbaz, David; Fudamoto, Yoshinobu; Fukushima, Shuma; Franco, Maximilien; Gómez-Guijarro, Carlos; Gruppioni, Carlotta; Jiménez-Andrade, Eric F.; Liu, Daizhong; Oesch, Pascal; Schinnerer, Eva; Traina, Alberto Zavala, J. A.; Casey, C. M.; Manning, S. M.; Aravena, M.; Bethermin, M.; Caputi, K. I.; Clements, D. L.; Cunha, E. da; Drew, P.;	Aims. We study the dust content of massive (log(M<SUB>*</SUB>/M<SUB>⊙</SUB>)≥10.8) quiescent galaxies (QGs) at redshifts z = 0.5 − 3 to place constraints on the evolution of their cold interstellar medium (ISM) and thereby obtain insights into the processes of galaxy quenching throughout cosmic time. Methods. We used a robust sample of 458 colour-selected QGs covered by the A<SUP>3</SUP>COSMOS+A<SUP>3</SUP>GOODSS database to perform a stacking analysis in the uv domain and measured their mean dust masses from their stacked sub-millimetre luminosities. We used the CIGALE spectral energy distribution fitting code to obtain star formation histories and infer the time since quenching for all the QGs in our sample. We used this information to gain insight into the time evolution of the dust content after quenching. Results. Most QGs in our sample quenched around a redshift of z ∼ 1.3, following the peak of cosmic star formation. The majority of QGs observed at z &gt; 1 are recently quenched (i.e. quenched for no l	2021	At z>4, the largest submm/mm surveys are only sensitive to the most extreme dusty star-forming galaxies (SFR>1000 M_sun/yr). Less extreme sources can be detected in the deepest single-dish telescope surveys, however, the identified population of DSFGs are overwhelmed by the more abundant low-z population (not to mention their large positional uncertainties). Recent deep pencil-beam surveys from ALMA have also failed to detect high-z sources. We have analyzed, for the first time, the potential of 3mm observations to detect high-z DSFGs. This wavelength naturally filters out z<2 galaxies due to a very negative K-correction. We find 14 serendipitously-detected 3mm sources within ~160 sq. arcmin of ALMA archival observations. Three of them already have spectroscopic redshifts (z=2.5-4.5), which confirms their high-z nature. Here, we request 19h of observations (including overheads) to conduct a blind redshift survey for the remaining sources using an optimized band 3 + band 4 spectral setup. This work will reveal	ALMA_3mm_d_04_TM1	Champagne, Jaclyn; Staguhn, Johannes; Casey, Caitlin; da Cunha, Elisabete; Drew, Patrick; Manning, Sinclaire; Spilker, Justin; Hung, Chao-Ling; Hodge, Jacqueline; Finkelstein, Steven;	0.8098162670670584	0.019730578586167606	2.1842108	uid://A001/X133d/X1d0d	uid://A001/X133d/X1d0e	uid://A002/Xda0496/Xadc	On the nature of 3mm-selected sources: the highest redshift dusty star-forming galaxies?	S	TARGET	T	17.04038593462587	T	2021ApJ...909..165Z 2022A&A...668A..67A 2023A&A...675L..10C 2024A&A...685A...1A 2024A&A...688A..55M 2024A&A...689A..41V 2025A&A...702A.186A	Sub-mm Galaxies (SMG);null	Galaxy evolution	zavala	Zavala, Jorge	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00478.S	ALMA	JAO	ALMA	uid://A001/X133d/X1d0e.source.ALMA_3mm_ID8.spw.27	cube	2		ALMA_3mm_ID8	150.09313999994433	2.52740830000167	0.01117065701276468	Circle ICRS 150.093140 2.527408 0.005585			240	1	2	1.6267198448429323	58566.999847	58567.027424	756	756	0.0021311177413911994	0.002159787223917751	18005.954934010868	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X1d0e	application/x-votable+xml; content=datalink		2018.1.00478.S	Public	236.44791675385477	42.28646686997679	4	1.199390474963693E-7	1.875E9	A001:DA44 A002:DA51 A003:DV12 A005:DA58 A006:DV25 A007:DV05 A010:DV13 A011:DV21 A015:DA64 A016:DV11 A017:DV14 A018:DA54 A019:DA61 A023:DA42 A024:DA49 A025:DA46 A026:DV19 A027:DV06 A030:DA62 A031:DA59 A033:DA53 A034:DA50 A035:DA43 A036:DA45 A038:DV24 A039:DA56 A040:DA55 A041:DA57 A042:DV08 A043:DA60 A044:DV03 A046:DA52 A048:DV02 A049:DA47 A058:DA41 A060:DV17 A062:DV10 A066:DV04 A068:DA65 A069:DV16 A072:DV20 A074:DV09 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2020-07-05T21:41:25.000	1.6267198448429323	[136.94..138.80GHz,7812.01kHz,809.8uJy/beam@10km/s,40.1uJy/beam@native, XX YY] U [138.81..140.67GHz,7812.01kHz,785.4uJy/beam@10km/s,39.2uJy/beam@native, XX YY] U [148.93..150.79GHz,7812.01kHz,760.9uJy/beam@10km/s,39.3uJy/beam@native, XX YY] U [150.79..152.66GHz,7812.01kHz,756.7uJy/beam@10km/s,39.3uJy/beam@native, XX YY]	139.7401454019834	15532.445883934306	ALMA	A<SUP>3</SUP>COSMOS and A<SUP>3</SUP>GOODSS: Continuum source catalogues and multi-band number counts A<SUP>3</SUP>COSMOS: Measuring the cosmic dust-attenuated star formation rate density at 4 < z < 5 A<SUP>3</SUP>COSMOS: The dust content of massive quiescent galaxies and its evolution with cosmic time ALMACAL. XI. Over-densities as signposts for proto-clusters? A cautionary tale CO in the ALMA Radio-source Catalogue (ARC): The molecular gas content of radio galaxies as a function of redshift The Evolution of the IR Luminosity Function and Dust-obscured Star Formation over the Past 13 Billion Years XLSSC 122 caught in the act of growing up: Spatially resolved SZ observations of a z = 1.98 galaxy cluster	Adscheid, Sylvia Audibert, A. Chen, Jianhang Magnelli, Benjamin Zavala, J. A. van Marrewijk, J.	Adscheid, Sylvia; Magnelli, Benjamin; Ciesla, Laure; Liu, Daizhong; Schinnerer, Eva; Bertoldi, Frank Adscheid, Sylvia; Magnelli, Benjamin; Liu, Daizhong; Bertoldi, Frank; Delvecchio, Ivan; Gruppioni, Carlotta; Schinnerer, Eva; Traina, Alberto; Béthermin, Matthieu; Gkogkou, Athanasia Audibert, A.; Dasyra, K. M.; Papachristou, M.; Fernández-Ontiveros, J. A.; Ruffa, I.; Bisigello, L.; Combes, F.; Salomé, P.; Gruppioni, C. Chen, Jianhang; Ivison, R. J.; Zwaan, Martin A.; Klitsch, Anne; Péroux, Céline; Lovell, Christopher C.; Lagos, Claudia del P.; Biggs, Andrew D.; Bollo, Victoria Magnelli, Benjamin; Adscheid, Sylvia; Wang, Tsan-Ming; Ciesla, Laure; Daddi, Emanuele; Delvecchio, Ivan; Elbaz, David; Fudamoto, Yoshinobu; Fukushima, Shuma; Franco, Maximilien; Gómez-Guijarro, Carlos; Gruppioni, Carlotta; Jiménez-Andrade, Eric F.; Liu, Daizhong; Oesch, Pascal; Schinnerer, Eva; Traina, Alberto Zavala, J. A.; Casey, C. M.; Manning, S. M.; Aravena, M.; Bethermin, M.; Caputi, K. I.; Clements, D. L.; Cunha, E. da; Drew, P.;	Aims. We study the dust content of massive (log(M<SUB>*</SUB>/M<SUB>⊙</SUB>)≥10.8) quiescent galaxies (QGs) at redshifts z = 0.5 − 3 to place constraints on the evolution of their cold interstellar medium (ISM) and thereby obtain insights into the processes of galaxy quenching throughout cosmic time. Methods. We used a robust sample of 458 colour-selected QGs covered by the A<SUP>3</SUP>COSMOS+A<SUP>3</SUP>GOODSS database to perform a stacking analysis in the uv domain and measured their mean dust masses from their stacked sub-millimetre luminosities. We used the CIGALE spectral energy distribution fitting code to obtain star formation histories and infer the time since quenching for all the QGs in our sample. We used this information to gain insight into the time evolution of the dust content after quenching. Results. Most QGs in our sample quenched around a redshift of z ∼ 1.3, following the peak of cosmic star formation. The majority of QGs observed at z &gt; 1 are recently quenched (i.e. quenched for no l	2021	At z>4, the largest submm/mm surveys are only sensitive to the most extreme dusty star-forming galaxies (SFR>1000 M_sun/yr). Less extreme sources can be detected in the deepest single-dish telescope surveys, however, the identified population of DSFGs are overwhelmed by the more abundant low-z population (not to mention their large positional uncertainties). Recent deep pencil-beam surveys from ALMA have also failed to detect high-z sources. We have analyzed, for the first time, the potential of 3mm observations to detect high-z DSFGs. This wavelength naturally filters out z<2 galaxies due to a very negative K-correction. We find 14 serendipitously-detected 3mm sources within ~160 sq. arcmin of ALMA archival observations. Three of them already have spectroscopic redshifts (z=2.5-4.5), which confirms their high-z nature. Here, we request 19h of observations (including overheads) to conduct a blind redshift survey for the remaining sources using an optimized band 3 + band 4 spectral setup. This work will reveal	ALMA_3mm_d_04_TM1	Champagne, Jaclyn; Staguhn, Johannes; Casey, Caitlin; da Cunha, Elisabete; Drew, Patrick; Manning, Sinclaire; Spilker, Justin; Hung, Chao-Ling; Hodge, Jacqueline; Finkelstein, Steven;	0.7854222109954385	0.019730578586167606	2.1842108	uid://A001/X133d/X1d0d	uid://A001/X133d/X1d0e	uid://A002/Xda0496/Xadc	On the nature of 3mm-selected sources: the highest redshift dusty star-forming galaxies?	S	TARGET	T	17.04038593462587	T	2021ApJ...909..165Z 2022A&A...668A..67A 2023A&A...675L..10C 2024A&A...685A...1A 2024A&A...688A..55M 2024A&A...689A..41V 2025A&A...702A.186A	Sub-mm Galaxies (SMG);null	Galaxy evolution	zavala	Zavala, Jorge	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.01115.S	ALMA	JAO	ALMA	uid://A001/X2fb/X3c4.source.J0134-3843.spw.25	cube	2	ari_l	J0134-3843	23.63345891246174	-38.725939594451376	0.006428187432244848	Circle ICRS 23.633459 -38.725940 0.003214			960	1	2	0.6283583445855888	57492.633541	57492.642058	90.72	90.72	0.0011468083457570075	0.0011550846808820454	133887.75786494644	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X3c4	application/x-votable+xml; content=datalink		2015.1.01115.S	Public	267.8063797794596	-75.31727245588512	6	8.565338295445672E-9	1.875E9	A002:DA49 A004:DA41 A006:DA61 A008:DV08 A009:DV18 A010:DV25 A011:DV09 A014:DV22 A015:DV04 A023:DA51 A029:DV10 A030:DA65 A033:DV20 A034:DA46 A036:DV16 A037:DV19 A038:DA50 A042:DV01 A047:DA55 A048:DV15 A049:DV11 A052:DA47 A061:DA62 A062:DA56 A063:DA44 A067:DA42 A068:DA45 A069:DV14 A070:DV21 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A076:DA52 A077:DA58 A078:DV12 A080:DV23 A092:DV17	F	2017-06-22T10:14:48.000	0.6283583445855888	[241.83..243.71GHz,1938.48kHz,2.9mJy/beam@10km/s,190.2uJy/beam@native, XX YY] U [243.71..245.58GHz,1938.48kHz,2.9mJy/beam@10km/s,192.1uJy/beam@native, XX YY] U [257.85..259.73GHz,1938.48kHz,2.9mJy/beam@10km/s,193.6uJy/beam@native, XX YY] U [259.54..261.41GHz,1938.48kHz,2.8mJy/beam@10km/s,193.8uJy/beam@native, XX YY]	260.4780761487609	2239.1327092235188	ALMA	A comprehensive view of the interstellar medium in a quasar host galaxy at z ≈ 6.4 A spectral stacking analysis to search for faint outflow signatures in z ̃ 6 quasars ALMA Reveals Bright Circumgalactic Emission and a Biconical Outflow in z ∼ 6.4 Quasar PSOJ183+05 ALMA and HST Kiloparsec-scale Imaging of a Quasar-galaxy Merger at Z ≈ 6.2 ALMA multiline survey of the ISM in two quasar host-companion galaxy pairs at z > 6 An ALMA [C II] Survey of 27 Quasars at z > 5.94 Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics Dust Emission in an Accretion-rate-limited Sample of z ≳ 6 Quasars No Evidence for [C II] Halos or High-velocity Outflows in z ≳ 6 Quasar Host Galaxies Physical Properties of 15 Quasars at z ≳ 6.5 Rapidly star-forming galaxies adjacent to quasars at redshifts exceeding 6 Resolved [C II] Emission from z > 6 Quasar Host─Companion Galaxy Pairs The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies Widespread QSO	Bischetti, M. Bischetti, Manuela Decarli, R. Decarli, Roberto Fei, Qinyue Mazzucchelli, C. Neeleman, Marcel Novak, Mladen Pensabene, A. Stanley, F. Venemans, Bram P.	Bischetti, M.; Maiolino, R.; Carniani, S.; Fiore, F.; Piconcelli, E.; Fluetsch, A. Bischetti, Manuela; Feruglio, Chiara; Carniani, Stefano; D'Odorico, Valentina; Salvestrini, Francesco; Fiore, Fabrizio Decarli, R.; Walter, F.; Venemans, B. P.; Bañados, E.; Bertoldi, F.; Carilli, C.; Fan, X.; Farina, E. P.; Mazzucchelli, C.; Riechers, D.; Rix, H.-W.; Strauss, M. A.; Wang, R.; Yang, Y. Decarli, Roberto; Dotti, Massimo; Bañados, Eduardo; Farina, Emanuele Paolo; Walter, Fabian; Carilli, Chris; Fan, Xiaohui; Mazzucchelli, Chiara; Neeleman, Marcel; Novak, Mladen; Riechers, Dominik; Strauss, Michael A.; Venemans, Bram P.; Yang, Yujin; Wang, Ran Decarli, Roberto; Pensabene, Antonio; Diaz-Santos, Tanio; Ferkinhoff, Carl; Strauss, Michael A.; Venemans, Bram P.; Walter, Fabian; Bañados, Eduardo; Bertoldi, Frank; Fan, Xiaohui; Farina, Emanuele Paolo; Riechers, Dominik A.; Rix, Hans-Walter; Wang, Ran Decarli, Roberto; Walter, Fabian; Venemans, Bram P.; Bañados, Eduardo; Bertoldi, Frank; Carilli, Chris; Fan, Xiaohui; Farin	<BR /> Aims: Outflows in quasars during the early epochs of galaxy evolution are an important part of the feedback mechanisms that potentially affect the evolution of the host galaxy. However, systematic millimetre (mm) observations of outflows are only now becoming possible with the advent of sensitive mm telescopes. In this study we used spectral stacking methods to search for a faint high-velocity outflow signal in a sample of [C II] detected, z ̃ 6 quasars. <BR /> Methods: We searched for broad emission line signatures from high-velocity outflows for a sample of 26 z ̃ 6 quasars observed with the Atacama Large Millimeter Array (ALMA), with a detection of the [C II] line. The observed emission lines of the sources are dominated by the host galaxy, and outflow emission is not detected for the individual sources. We used a spectral line stacking analysis developed for interferometric data to search for outflow emission. We stacked both extracted spectra and the full spectral cubes. We also investigated the p	2017	Optically-selected quasars have been detected well into the epoch of reionization, indicating the existence of supermassive black holes (SMBH) within one Gyr of the Big Bang. FIR continuum and line observations of selected sources have revealed that quasar hosts often show intense star formation and massive, enriched gas reservoirs. We propose to observe an accretion-rate-limited sample (35 quasars total, the majority recently discovered by us using Pan-STARRS1) in [CII] and continuum emission, spanning a factor of ~20 in quasar bolometric luminosity, ~40 in SMBH mass, and ~100 in FIR luminosity. This critical five-fold increase in sample size was simply inconceivable pre-ALMA. We will study the fraction of high-z quasars associated with massive starbursts, will reveal any correlation between SMBH accretion (+ Eddington ratios) and star formation, and will constrain ISM masses. [CII] observations will provide first insights on the host dynamics, feedback, and on cosmic reionization through precise redshift me	J0142-33_a_06_TE	Rix, Hans-Walter; Decarli, Roberto; Banados, Eduardo; Riechers, Dominik; Fan, Xiaohui; Bertoldi, Frank; Strauss, Michael; Venemans, Bram; Carilli, Chris; Farina, Emanuele Paolo; Wang, Ran; Yang, Yujin;	2.8465925579986333	0.09619857095426596	1.394456	uid://A001/X2fb/X3c3	uid://A001/X2fb/X3c4	uid://A002/Xb1c200/X4077	The first Gigayear of the Universe: A census of dust and gas in z>6 quasars	S	PHASE WVR	F	6.009079146277565	T	2017ApJ...849...91M 2017Natur.545..457D 2018ApJ...854...97D 2018ApJ...866..159V 2019A&A...630A..59B 2019A&A...631A..78S 2019ApJ...880..157D 2019ApJ...882...10N 2020A&A...637A..84P 2020ApJ...904..131N 2021A&A...652A..66P 2023A&A...673A.157D 2025ApJ...980...84F 2025ApJ...990L..31B	High-z Active Galactic Nuclei (AGN);null	Active galaxies	walter	Walter, Fabian	1938.4765625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.01115.S	ALMA	JAO	ALMA	uid://A001/X2fb/X3c4.source.J0134-3843.spw.31	cube	2	ari_l	J0134-3843	23.63345891246174	-38.725939594451376	0.006428187432244848	Circle ICRS 23.633459 -38.725940 0.003214			960	1	2	0.6283583445855888	57492.633541	57492.642058	90.72	90.72	0.0012301378693824448	0.0012396656501305514	125718.9961521001	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X3c4	application/x-votable+xml; content=datalink		2015.1.01115.S	Public	267.8063797794596	-75.31727245588512	6	9.860483424056123E-9	1.875E9	A002:DA49 A004:DA41 A006:DA61 A008:DV08 A009:DV18 A010:DV25 A011:DV09 A014:DV22 A015:DV04 A023:DA51 A029:DV10 A030:DA65 A033:DV20 A034:DA46 A036:DV16 A037:DV19 A038:DA50 A042:DV01 A047:DA55 A048:DV15 A049:DV11 A052:DA47 A061:DA62 A062:DA56 A063:DA44 A067:DA42 A068:DA45 A069:DV14 A070:DV21 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A076:DA52 A077:DA58 A078:DV12 A080:DV23 A092:DV17	F	2017-06-22T10:14:48.000	0.6283583445855888	[241.83..243.71GHz,1938.48kHz,2.9mJy/beam@10km/s,190.2uJy/beam@native, XX YY] U [243.71..245.58GHz,1938.48kHz,2.9mJy/beam@10km/s,192.1uJy/beam@native, XX YY] U [257.85..259.73GHz,1938.48kHz,2.9mJy/beam@10km/s,193.6uJy/beam@native, XX YY] U [259.54..261.41GHz,1938.48kHz,2.8mJy/beam@10km/s,193.8uJy/beam@native, XX YY]	242.76985370087186	2239.1327092235188	ALMA	A comprehensive view of the interstellar medium in a quasar host galaxy at z ≈ 6.4 A spectral stacking analysis to search for faint outflow signatures in z ̃ 6 quasars ALMA Reveals Bright Circumgalactic Emission and a Biconical Outflow in z ∼ 6.4 Quasar PSOJ183+05 ALMA and HST Kiloparsec-scale Imaging of a Quasar-galaxy Merger at Z ≈ 6.2 ALMA multiline survey of the ISM in two quasar host-companion galaxy pairs at z > 6 An ALMA [C II] Survey of 27 Quasars at z > 5.94 Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics Dust Emission in an Accretion-rate-limited Sample of z ≳ 6 Quasars No Evidence for [C II] Halos or High-velocity Outflows in z ≳ 6 Quasar Host Galaxies Physical Properties of 15 Quasars at z ≳ 6.5 Rapidly star-forming galaxies adjacent to quasars at redshifts exceeding 6 Resolved [C II] Emission from z > 6 Quasar Host─Companion Galaxy Pairs The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies Widespread QSO	Bischetti, M. Bischetti, Manuela Decarli, R. Decarli, Roberto Fei, Qinyue Mazzucchelli, C. Neeleman, Marcel Novak, Mladen Pensabene, A. Stanley, F. Venemans, Bram P.	Bischetti, M.; Maiolino, R.; Carniani, S.; Fiore, F.; Piconcelli, E.; Fluetsch, A. Bischetti, Manuela; Feruglio, Chiara; Carniani, Stefano; D'Odorico, Valentina; Salvestrini, Francesco; Fiore, Fabrizio Decarli, R.; Walter, F.; Venemans, B. P.; Bañados, E.; Bertoldi, F.; Carilli, C.; Fan, X.; Farina, E. P.; Mazzucchelli, C.; Riechers, D.; Rix, H.-W.; Strauss, M. A.; Wang, R.; Yang, Y. Decarli, Roberto; Dotti, Massimo; Bañados, Eduardo; Farina, Emanuele Paolo; Walter, Fabian; Carilli, Chris; Fan, Xiaohui; Mazzucchelli, Chiara; Neeleman, Marcel; Novak, Mladen; Riechers, Dominik; Strauss, Michael A.; Venemans, Bram P.; Yang, Yujin; Wang, Ran Decarli, Roberto; Pensabene, Antonio; Diaz-Santos, Tanio; Ferkinhoff, Carl; Strauss, Michael A.; Venemans, Bram P.; Walter, Fabian; Bañados, Eduardo; Bertoldi, Frank; Fan, Xiaohui; Farina, Emanuele Paolo; Riechers, Dominik A.; Rix, Hans-Walter; Wang, Ran Decarli, Roberto; Walter, Fabian; Venemans, Bram P.; Bañados, Eduardo; Bertoldi, Frank; Carilli, Chris; Fan, Xiaohui; Farin	<BR /> Aims: Outflows in quasars during the early epochs of galaxy evolution are an important part of the feedback mechanisms that potentially affect the evolution of the host galaxy. However, systematic millimetre (mm) observations of outflows are only now becoming possible with the advent of sensitive mm telescopes. In this study we used spectral stacking methods to search for a faint high-velocity outflow signal in a sample of [C II] detected, z ̃ 6 quasars. <BR /> Methods: We searched for broad emission line signatures from high-velocity outflows for a sample of 26 z ̃ 6 quasars observed with the Atacama Large Millimeter Array (ALMA), with a detection of the [C II] line. The observed emission lines of the sources are dominated by the host galaxy, and outflow emission is not detected for the individual sources. We used a spectral line stacking analysis developed for interferometric data to search for outflow emission. We stacked both extracted spectra and the full spectral cubes. We also investigated the p	2017	Optically-selected quasars have been detected well into the epoch of reionization, indicating the existence of supermassive black holes (SMBH) within one Gyr of the Big Bang. FIR continuum and line observations of selected sources have revealed that quasar hosts often show intense star formation and massive, enriched gas reservoirs. We propose to observe an accretion-rate-limited sample (35 quasars total, the majority recently discovered by us using Pan-STARRS1) in [CII] and continuum emission, spanning a factor of ~20 in quasar bolometric luminosity, ~40 in SMBH mass, and ~100 in FIR luminosity. This critical five-fold increase in sample size was simply inconceivable pre-ALMA. We will study the fraction of high-z quasars associated with massive starbursts, will reveal any correlation between SMBH accretion (+ Eddington ratios) and star formation, and will constrain ISM masses. [CII] observations will provide first insights on the host dynamics, feedback, and on cosmic reionization through precise redshift me	J0142-33_a_06_TE	Rix, Hans-Walter; Decarli, Roberto; Banados, Eduardo; Riechers, Dominik; Fan, Xiaohui; Bertoldi, Frank; Strauss, Michael; Venemans, Bram; Carilli, Chris; Farina, Emanuele Paolo; Wang, Ran; Yang, Yujin;	2.8942621783441758	0.09619857095426596	1.394456	uid://A001/X2fb/X3c3	uid://A001/X2fb/X3c4	uid://A002/Xb1c200/X4077	The first Gigayear of the Universe: A census of dust and gas in z>6 quasars	S	PHASE WVR	F	6.009079146277565	T	2017ApJ...849...91M 2017Natur.545..457D 2018ApJ...854...97D 2018ApJ...866..159V 2019A&A...630A..59B 2019A&A...631A..78S 2019ApJ...880..157D 2019ApJ...882...10N 2020A&A...637A..84P 2020ApJ...904..131N 2021A&A...652A..66P 2023A&A...673A.157D 2025ApJ...980...84F 2025ApJ...990L..31B	High-z Active Galactic Nuclei (AGN);null	Active galaxies	walter	Walter, Fabian	1938.4765625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.01115.S	ALMA	JAO	ALMA	uid://A001/X2fb/X3c4.source.J0134-3843.spw.27	cube	2	ari_l	J0134-3843	23.63345891246174	-38.725939594451376	0.006428187432244848	Circle ICRS 23.633459 -38.725940 0.003214			960	1	2	0.6283583445855888	57492.633541	57492.642058	90.72	90.72	0.0011542637223960566	0.0011626484092389221	133016.7373373695	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X3c4	application/x-votable+xml; content=datalink		2015.1.01115.S	Public	267.8063797794596	-75.31727245588512	6	8.677473570790232E-9	1.875E9	A002:DA49 A004:DA41 A006:DA61 A008:DV08 A009:DV18 A010:DV25 A011:DV09 A014:DV22 A015:DV04 A023:DA51 A029:DV10 A030:DA65 A033:DV20 A034:DA46 A036:DV16 A037:DV19 A038:DA50 A042:DV01 A047:DA55 A048:DV15 A049:DV11 A052:DA47 A061:DA62 A062:DA56 A063:DA44 A067:DA42 A068:DA45 A069:DV14 A070:DV21 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A076:DA52 A077:DA58 A078:DV12 A080:DV23 A092:DV17	F	2017-06-22T10:14:48.000	0.6283583445855888	[241.83..243.71GHz,1938.48kHz,2.9mJy/beam@10km/s,190.2uJy/beam@native, XX YY] U [243.71..245.58GHz,1938.48kHz,2.9mJy/beam@10km/s,192.1uJy/beam@native, XX YY] U [257.85..259.73GHz,1938.48kHz,2.9mJy/beam@10km/s,193.6uJy/beam@native, XX YY] U [259.54..261.41GHz,1938.48kHz,2.8mJy/beam@10km/s,193.8uJy/beam@native, XX YY]	258.78960206025226	2239.1327092235188	ALMA	A comprehensive view of the interstellar medium in a quasar host galaxy at z ≈ 6.4 A spectral stacking analysis to search for faint outflow signatures in z ̃ 6 quasars ALMA Reveals Bright Circumgalactic Emission and a Biconical Outflow in z ∼ 6.4 Quasar PSOJ183+05 ALMA and HST Kiloparsec-scale Imaging of a Quasar-galaxy Merger at Z ≈ 6.2 ALMA multiline survey of the ISM in two quasar host-companion galaxy pairs at z > 6 An ALMA [C II] Survey of 27 Quasars at z > 5.94 Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics Dust Emission in an Accretion-rate-limited Sample of z ≳ 6 Quasars No Evidence for [C II] Halos or High-velocity Outflows in z ≳ 6 Quasar Host Galaxies Physical Properties of 15 Quasars at z ≳ 6.5 Rapidly star-forming galaxies adjacent to quasars at redshifts exceeding 6 Resolved [C II] Emission from z > 6 Quasar Host─Companion Galaxy Pairs The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies Widespread QSO	Bischetti, M. Bischetti, Manuela Decarli, R. Decarli, Roberto Fei, Qinyue Mazzucchelli, C. Neeleman, Marcel Novak, Mladen Pensabene, A. Stanley, F. Venemans, Bram P.	Bischetti, M.; Maiolino, R.; Carniani, S.; Fiore, F.; Piconcelli, E.; Fluetsch, A. Bischetti, Manuela; Feruglio, Chiara; Carniani, Stefano; D'Odorico, Valentina; Salvestrini, Francesco; Fiore, Fabrizio Decarli, R.; Walter, F.; Venemans, B. P.; Bañados, E.; Bertoldi, F.; Carilli, C.; Fan, X.; Farina, E. P.; Mazzucchelli, C.; Riechers, D.; Rix, H.-W.; Strauss, M. A.; Wang, R.; Yang, Y. Decarli, Roberto; Dotti, Massimo; Bañados, Eduardo; Farina, Emanuele Paolo; Walter, Fabian; Carilli, Chris; Fan, Xiaohui; Mazzucchelli, Chiara; Neeleman, Marcel; Novak, Mladen; Riechers, Dominik; Strauss, Michael A.; Venemans, Bram P.; Yang, Yujin; Wang, Ran Decarli, Roberto; Pensabene, Antonio; Diaz-Santos, Tanio; Ferkinhoff, Carl; Strauss, Michael A.; Venemans, Bram P.; Walter, Fabian; Bañados, Eduardo; Bertoldi, Frank; Fan, Xiaohui; Farina, Emanuele Paolo; Riechers, Dominik A.; Rix, Hans-Walter; Wang, Ran Decarli, Roberto; Walter, Fabian; Venemans, Bram P.; Bañados, Eduardo; Bertoldi, Frank; Carilli, Chris; Fan, Xiaohui; Farin	<BR /> Aims: Outflows in quasars during the early epochs of galaxy evolution are an important part of the feedback mechanisms that potentially affect the evolution of the host galaxy. However, systematic millimetre (mm) observations of outflows are only now becoming possible with the advent of sensitive mm telescopes. In this study we used spectral stacking methods to search for a faint high-velocity outflow signal in a sample of [C II] detected, z ̃ 6 quasars. <BR /> Methods: We searched for broad emission line signatures from high-velocity outflows for a sample of 26 z ̃ 6 quasars observed with the Atacama Large Millimeter Array (ALMA), with a detection of the [C II] line. The observed emission lines of the sources are dominated by the host galaxy, and outflow emission is not detected for the individual sources. We used a spectral line stacking analysis developed for interferometric data to search for outflow emission. We stacked both extracted spectra and the full spectral cubes. We also investigated the p	2017	Optically-selected quasars have been detected well into the epoch of reionization, indicating the existence of supermassive black holes (SMBH) within one Gyr of the Big Bang. FIR continuum and line observations of selected sources have revealed that quasar hosts often show intense star formation and massive, enriched gas reservoirs. We propose to observe an accretion-rate-limited sample (35 quasars total, the majority recently discovered by us using Pan-STARRS1) in [CII] and continuum emission, spanning a factor of ~20 in quasar bolometric luminosity, ~40 in SMBH mass, and ~100 in FIR luminosity. This critical five-fold increase in sample size was simply inconceivable pre-ALMA. We will study the fraction of high-z quasars associated with massive starbursts, will reveal any correlation between SMBH accretion (+ Eddington ratios) and star formation, and will constrain ISM masses. [CII] observations will provide first insights on the host dynamics, feedback, and on cosmic reionization through precise redshift me	J0142-33_a_06_TE	Rix, Hans-Walter; Decarli, Roberto; Banados, Eduardo; Riechers, Dominik; Fan, Xiaohui; Bertoldi, Frank; Strauss, Michael; Venemans, Bram; Carilli, Chris; Farina, Emanuele Paolo; Wang, Ran; Yang, Yujin;	2.8531154112976957	0.09619857095426596	1.394456	uid://A001/X2fb/X3c3	uid://A001/X2fb/X3c4	uid://A002/Xb1c200/X4077	The first Gigayear of the Universe: A census of dust and gas in z>6 quasars	S	PHASE WVR	F	6.009079146277565	T	2017ApJ...849...91M 2017Natur.545..457D 2018ApJ...854...97D 2018ApJ...866..159V 2019A&A...630A..59B 2019A&A...631A..78S 2019ApJ...880..157D 2019ApJ...882...10N 2020A&A...637A..84P 2020ApJ...904..131N 2021A&A...652A..66P 2023A&A...673A.157D 2025ApJ...980...84F 2025ApJ...990L..31B	High-z Active Galactic Nuclei (AGN);null	Active galaxies	walter	Walter, Fabian	1938.4765625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.01115.S	ALMA	JAO	ALMA	uid://A001/X2fb/X3c4.source.J0134-3843.spw.29	cube	2	ari_l	J0134-3843	23.63345891246174	-38.725939594451376	0.006428187432244848	Circle ICRS 23.633459 -38.725940 0.003214			960	1	2	0.6283583445855888	57492.633541	57492.642058	90.72	90.72	0.001220745719315479	0.0012301280106997773	126686.25056016055	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X3c4	application/x-votable+xml; content=datalink		2015.1.01115.S	Public	267.8063797794596	-75.31727245588512	6	9.709913685085728E-9	1.875E9	A002:DA49 A004:DA41 A006:DA61 A008:DV08 A009:DV18 A010:DV25 A011:DV09 A014:DV22 A015:DV04 A023:DA51 A029:DV10 A030:DA65 A033:DV20 A034:DA46 A036:DV16 A037:DV19 A038:DA50 A042:DV01 A047:DA55 A048:DV15 A049:DV11 A052:DA47 A061:DA62 A062:DA56 A063:DA44 A067:DA42 A068:DA45 A069:DV14 A070:DV21 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A076:DA52 A077:DA58 A078:DV12 A080:DV23 A092:DV17	F	2017-06-22T10:14:48.000	0.6283583445855888	[241.83..243.71GHz,1938.48kHz,2.9mJy/beam@10km/s,190.2uJy/beam@native, XX YY] U [243.71..245.58GHz,1938.48kHz,2.9mJy/beam@10km/s,192.1uJy/beam@native, XX YY] U [257.85..259.73GHz,1938.48kHz,2.9mJy/beam@10km/s,193.6uJy/beam@native, XX YY] U [259.54..261.41GHz,1938.48kHz,2.8mJy/beam@10km/s,193.8uJy/beam@native, XX YY]	244.64487725462112	2239.1327092235188	ALMA	A comprehensive view of the interstellar medium in a quasar host galaxy at z ≈ 6.4 A spectral stacking analysis to search for faint outflow signatures in z ̃ 6 quasars ALMA Reveals Bright Circumgalactic Emission and a Biconical Outflow in z ∼ 6.4 Quasar PSOJ183+05 ALMA and HST Kiloparsec-scale Imaging of a Quasar-galaxy Merger at Z ≈ 6.2 ALMA multiline survey of the ISM in two quasar host-companion galaxy pairs at z > 6 An ALMA [C II] Survey of 27 Quasars at z > 5.94 Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics Dust Emission in an Accretion-rate-limited Sample of z ≳ 6 Quasars No Evidence for [C II] Halos or High-velocity Outflows in z ≳ 6 Quasar Host Galaxies Physical Properties of 15 Quasars at z ≳ 6.5 Rapidly star-forming galaxies adjacent to quasars at redshifts exceeding 6 Resolved [C II] Emission from z > 6 Quasar Host─Companion Galaxy Pairs The ALMA view of the high-redshift relation between supermassive black holes and their host galaxies Widespread QSO	Bischetti, M. Bischetti, Manuela Decarli, R. Decarli, Roberto Fei, Qinyue Mazzucchelli, C. Neeleman, Marcel Novak, Mladen Pensabene, A. Stanley, F. Venemans, Bram P.	Bischetti, M.; Maiolino, R.; Carniani, S.; Fiore, F.; Piconcelli, E.; Fluetsch, A. Bischetti, Manuela; Feruglio, Chiara; Carniani, Stefano; D'Odorico, Valentina; Salvestrini, Francesco; Fiore, Fabrizio Decarli, R.; Walter, F.; Venemans, B. P.; Bañados, E.; Bertoldi, F.; Carilli, C.; Fan, X.; Farina, E. P.; Mazzucchelli, C.; Riechers, D.; Rix, H.-W.; Strauss, M. A.; Wang, R.; Yang, Y. Decarli, Roberto; Dotti, Massimo; Bañados, Eduardo; Farina, Emanuele Paolo; Walter, Fabian; Carilli, Chris; Fan, Xiaohui; Mazzucchelli, Chiara; Neeleman, Marcel; Novak, Mladen; Riechers, Dominik; Strauss, Michael A.; Venemans, Bram P.; Yang, Yujin; Wang, Ran Decarli, Roberto; Pensabene, Antonio; Diaz-Santos, Tanio; Ferkinhoff, Carl; Strauss, Michael A.; Venemans, Bram P.; Walter, Fabian; Bañados, Eduardo; Bertoldi, Frank; Fan, Xiaohui; Farina, Emanuele Paolo; Riechers, Dominik A.; Rix, Hans-Walter; Wang, Ran Decarli, Roberto; Walter, Fabian; Venemans, Bram P.; Bañados, Eduardo; Bertoldi, Frank; Carilli, Chris; Fan, Xiaohui; Farin	<BR /> Aims: Outflows in quasars during the early epochs of galaxy evolution are an important part of the feedback mechanisms that potentially affect the evolution of the host galaxy. However, systematic millimetre (mm) observations of outflows are only now becoming possible with the advent of sensitive mm telescopes. In this study we used spectral stacking methods to search for a faint high-velocity outflow signal in a sample of [C II] detected, z ̃ 6 quasars. <BR /> Methods: We searched for broad emission line signatures from high-velocity outflows for a sample of 26 z ̃ 6 quasars observed with the Atacama Large Millimeter Array (ALMA), with a detection of the [C II] line. The observed emission lines of the sources are dominated by the host galaxy, and outflow emission is not detected for the individual sources. We used a spectral line stacking analysis developed for interferometric data to search for outflow emission. We stacked both extracted spectra and the full spectral cubes. We also investigated the p	2017	Optically-selected quasars have been detected well into the epoch of reionization, indicating the existence of supermassive black holes (SMBH) within one Gyr of the Big Bang. FIR continuum and line observations of selected sources have revealed that quasar hosts often show intense star formation and massive, enriched gas reservoirs. We propose to observe an accretion-rate-limited sample (35 quasars total, the majority recently discovered by us using Pan-STARRS1) in [CII] and continuum emission, spanning a factor of ~20 in quasar bolometric luminosity, ~40 in SMBH mass, and ~100 in FIR luminosity. This critical five-fold increase in sample size was simply inconceivable pre-ALMA. We will study the fraction of high-z quasars associated with massive starbursts, will reveal any correlation between SMBH accretion (+ Eddington ratios) and star formation, and will constrain ISM masses. [CII] observations will provide first insights on the host dynamics, feedback, and on cosmic reionization through precise redshift me	J0142-33_a_06_TE	Rix, Hans-Walter; Decarli, Roberto; Banados, Eduardo; Riechers, Dominik; Fan, Xiaohui; Bertoldi, Frank; Strauss, Michael; Venemans, Bram; Carilli, Chris; Farina, Emanuele Paolo; Wang, Ran; Yang, Yujin;	2.9115790829950807	0.09619857095426596	1.394456	uid://A001/X2fb/X3c3	uid://A001/X2fb/X3c4	uid://A002/Xb1c200/X4077	The first Gigayear of the Universe: A census of dust and gas in z>6 quasars	S	PHASE WVR	F	6.009079146277565	T	2017ApJ...849...91M 2017Natur.545..457D 2018ApJ...854...97D 2018ApJ...866..159V 2019A&A...630A..59B 2019A&A...631A..78S 2019ApJ...880..157D 2019ApJ...882...10N 2020A&A...637A..84P 2020ApJ...904..131N 2021A&A...652A..66P 2023A&A...673A.157D 2025ApJ...980...84F 2025ApJ...990L..31B	High-z Active Galactic Nuclei (AGN);null	Active galaxies	walter	Walter, Fabian	1938.4765625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00235.S	ALMA	JAO	ALMA	uid://A001/X14c3/Xa67.source.J1337-6509.spw.22	image	2		J1337-6509	204.46852223296676	-65.15691606390389	0.010536265942348539	Circle ICRS 204.468522 -65.156916 0.005268			128	1	2	5.62114028768222	59415.879041	59415.892402	181.44	181.44	0.0010980870839988497	0.001106127502579142	8672.251218964842	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/Xa67	application/x-votable+xml; content=datalink		2019.2.00235.S	Public	307.78728487713704	-2.7238905921069603	6	1.2661095737084682E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11	F	2022-08-10T12:21:23.000	5.62114028768222	[253.33..255.31GHz,31250.00kHz,27.5mJy/beam@10km/s,1.8mJy/beam@native, XX YY] U [255.32..257.32GHz,976.56kHz,25.4mJy/beam@10km/s,1.7mJy/beam@native, XX YY] U [269.03..271.01GHz,31250.00kHz,28.3mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [271.03..273.01GHz,31250.00kHz,31.6mJy/beam@10km/s,2.1mJy/beam@native, XX YY]	272.02110804993725	1137.8314503373933	ALMA						The powerful and highly ionized winds of Wolf-Rayet (WR) stars emit free-free radiation and recombination lines from the radio to near-IR. Despite being bright at sub-mm wavelengths, few suitable observations have been made in the gap between radio and near-IR wavelengths to characterise the wind properties and compare with models. We propose to use ACA in Bands 3 and 6 (92 and 263GHz) to build a catalogue of mm/sub-mm spectral indices and flux densities of the winds of 57 of the brightest Galactic WR stars. This will be used to identify potential new high-frequency calibration sources for ALMA (to increase the number of phase calibrators available for high frequency bands), investigate statistical trends and compare with wind emission models, and use to select sources and plan future high spatial resolution imaging of the wind morphologies. The catalogue and images will have a strong legacy value to the evolved massive star community.	HD_11729_a_06_7M	Agliozzo, Claudia;	31.553785021538534	0.9233957582780258	1.8	uid://A001/X14c3/Xa66	uid://A001/X14c3/Xa67	uid://A002/Xee1eb6/X11ddb	A legacy survey of Wolf-Rayet star winds	S	PHASE WVR	F	29.283753429727856	T		Hypergiants;Evolved stars - Shaping/physical structure	Stars and stellar evolution	nphillip	Phillips, Neil	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00235.S	ALMA	JAO	ALMA	uid://A001/X14c3/Xa67.source.J1337-6509.spw.16	cube	2		J1337-6509	204.46852223296676	-65.15691606390389	0.010536265942348539	Circle ICRS 204.468522 -65.156916 0.005268			4096	1	2	5.62114028768222	59415.879041	59415.892402	181.44	181.44	0.0011650491568641183	0.0011741737499961625	263477.03599782253	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/Xa67	application/x-votable+xml; content=datalink		2019.2.00235.S	Public	307.78728487713704	-2.7238905921069603	6	4.456110558153674E-9	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11	F	2022-08-10T12:21:23.000	5.62114028768222	[253.33..255.31GHz,31250.00kHz,27.5mJy/beam@10km/s,1.8mJy/beam@native, XX YY] U [255.32..257.32GHz,976.56kHz,25.4mJy/beam@10km/s,1.7mJy/beam@native, XX YY] U [269.03..271.01GHz,31250.00kHz,28.3mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [271.03..273.01GHz,31250.00kHz,31.6mJy/beam@10km/s,2.1mJy/beam@native, XX YY]	256.32189104922594	1137.8314503373933	ALMA						The powerful and highly ionized winds of Wolf-Rayet (WR) stars emit free-free radiation and recombination lines from the radio to near-IR. Despite being bright at sub-mm wavelengths, few suitable observations have been made in the gap between radio and near-IR wavelengths to characterise the wind properties and compare with models. We propose to use ACA in Bands 3 and 6 (92 and 263GHz) to build a catalogue of mm/sub-mm spectral indices and flux densities of the winds of 57 of the brightest Galactic WR stars. This will be used to identify potential new high-frequency calibration sources for ALMA (to increase the number of phase calibrators available for high frequency bands), investigate statistical trends and compare with wind emission models, and use to select sources and plan future high spatial resolution imaging of the wind morphologies. The catalogue and images will have a strong legacy value to the evolved massive star community.	HD_11729_a_06_7M	Agliozzo, Claudia;	25.411752652206754	0.9233957582780258	1.8	uid://A001/X14c3/Xa66	uid://A001/X14c3/Xa67	uid://A002/Xee1eb6/X11ddb	A legacy survey of Wolf-Rayet star winds	S	PHASE WVR	F	29.283753429727856	T		Hypergiants;Evolved stars - Shaping/physical structure	Stars and stellar evolution	nphillip	Phillips, Neil	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00235.S	ALMA	JAO	ALMA	uid://A001/X14c3/Xa67.source.J1337-6509.spw.18	image	2		J1337-6509	204.46852223296676	-65.15691606390389	0.010536265942348539	Circle ICRS 204.468522 -65.156916 0.005268			128	1	2	5.62114028768222	59415.879041	59415.892402	181.44	181.44	0.0011742203497102986	0.0011834190152937296	8169.348781035155	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/Xa67	application/x-votable+xml; content=datalink		2019.2.00235.S	Public	307.78728487713704	-2.7238905921069603	6	1.4484965483104527E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11	F	2022-08-10T12:21:23.000	5.62114028768222	[253.33..255.31GHz,31250.00kHz,27.5mJy/beam@10km/s,1.8mJy/beam@native, XX YY] U [255.32..257.32GHz,976.56kHz,25.4mJy/beam@10km/s,1.7mJy/beam@native, XX YY] U [269.03..271.01GHz,31250.00kHz,28.3mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [271.03..273.01GHz,31250.00kHz,31.6mJy/beam@10km/s,2.1mJy/beam@native, XX YY]	254.31966076243984	1137.8314503373933	ALMA						The powerful and highly ionized winds of Wolf-Rayet (WR) stars emit free-free radiation and recombination lines from the radio to near-IR. Despite being bright at sub-mm wavelengths, few suitable observations have been made in the gap between radio and near-IR wavelengths to characterise the wind properties and compare with models. We propose to use ACA in Bands 3 and 6 (92 and 263GHz) to build a catalogue of mm/sub-mm spectral indices and flux densities of the winds of 57 of the brightest Galactic WR stars. This will be used to identify potential new high-frequency calibration sources for ALMA (to increase the number of phase calibrators available for high frequency bands), investigate statistical trends and compare with wind emission models, and use to select sources and plan future high spatial resolution imaging of the wind morphologies. The catalogue and images will have a strong legacy value to the evolved massive star community.	HD_11729_a_06_7M	Agliozzo, Claudia;	27.462142991346134	0.9233957582780258	1.8	uid://A001/X14c3/Xa66	uid://A001/X14c3/Xa67	uid://A002/Xee1eb6/X11ddb	A legacy survey of Wolf-Rayet star winds	S	PHASE WVR	F	29.283753429727856	T		Hypergiants;Evolved stars - Shaping/physical structure	Stars and stellar evolution	nphillip	Phillips, Neil	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00235.S	ALMA	JAO	ALMA	uid://A001/X14c3/Xa67.source.J1337-6509.spw.20	image	2		J1337-6509	204.46852223296676	-65.15691606390389	0.010536265942348539	Circle ICRS 204.468522 -65.156916 0.005268			128	1	2	5.62114028768222	59415.879041	59415.892402	181.44	181.44	0.0011061912802103637	0.001114351258875787	8608.251218964842	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/Xa67	application/x-votable+xml; content=datalink		2019.2.00235.S	Public	307.78728487713704	-2.7238905921069603	6	1.2849364751821044E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11	F	2022-08-10T12:21:23.000	5.62114028768222	[253.33..255.31GHz,31250.00kHz,27.5mJy/beam@10km/s,1.8mJy/beam@native, XX YY] U [255.32..257.32GHz,976.56kHz,25.4mJy/beam@10km/s,1.7mJy/beam@native, XX YY] U [269.03..271.01GHz,31250.00kHz,28.3mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [271.03..273.01GHz,31250.00kHz,31.6mJy/beam@10km/s,2.1mJy/beam@native, XX YY]	270.0209531238024	1137.8314503373933	ALMA						The powerful and highly ionized winds of Wolf-Rayet (WR) stars emit free-free radiation and recombination lines from the radio to near-IR. Despite being bright at sub-mm wavelengths, few suitable observations have been made in the gap between radio and near-IR wavelengths to characterise the wind properties and compare with models. We propose to use ACA in Bands 3 and 6 (92 and 263GHz) to build a catalogue of mm/sub-mm spectral indices and flux densities of the winds of 57 of the brightest Galactic WR stars. This will be used to identify potential new high-frequency calibration sources for ALMA (to increase the number of phase calibrators available for high frequency bands), investigate statistical trends and compare with wind emission models, and use to select sources and plan future high spatial resolution imaging of the wind morphologies. The catalogue and images will have a strong legacy value to the evolved massive star community.	HD_11729_a_06_7M	Agliozzo, Claudia;	28.335130560485684	0.9233957582780258	1.8	uid://A001/X14c3/Xa66	uid://A001/X14c3/Xa67	uid://A002/Xee1eb6/X11ddb	A legacy survey of Wolf-Rayet star winds	S	PHASE WVR	F	29.283753429727856	T		Hypergiants;Evolved stars - Shaping/physical structure	Stars and stellar evolution	nphillip	Phillips, Neil	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X15eb.source.J0725-0054.spw.10	image	2		J0725-0054	111.46099963296886	-0.91570636944423	0.01190093036373538	Circle ICRS 111.461000 -0.915706 0.005950			128	1	2	4.9506421149681605	60988.319961	60988.326983	604.8	604.8	0.0012337906889570882	0.0012439492949084998	7712.25	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X15eb	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	217.6971242928812	7.227169550857697	6	1.59982870715768E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N604:CM11 N605:CM04	F	2026-11-13T21:27:30.000	4.9506421149681605	[223.00..224.99GHz,31250.00kHz,15.4mJy/beam@10km/s,941.5uJy/beam@native, XX YY] U [225.00..226.99GHz,31250.00kHz,14.8mJy/beam@10km/s,908.8uJy/beam@native, XX YY] U [239.00..240.98GHz,31250.00kHz,15.6mJy/beam@10km/s,988.4uJy/beam@native, XX YY] U [241.00..242.98GHz,31250.00kHz,16.4mJy/beam@10km/s,1mJy/beam@native, XX YY]	241.99270256052523	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	FBQS_J08_a_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	16.430458769938305	0.48333882341380324	1.8	uid://A001/X3833/X15ea	uid://A001/X3833/X15eb	uid://A002/X1315235/X1f4c2	Towards resolving orbiting binary supermassive black holes with the EHT	S	BANDPASS FLUX WVR	F	31.161568715761135	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X15eb.source.J0725-0054.spw.14	image	2		J0725-0054	111.46099963296886	-0.91570636944423	0.01190093036373538	Circle ICRS 111.461000 -0.915706 0.005950			128	1	2	4.9506421149681605	60988.319961	60988.326983	604.8	604.8	0.0013324973713884252	0.001344354240624106	7199.7500000032	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X15eb	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	217.6971242928812	7.227169550857697	6	1.867279808960479E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N604:CM11 N605:CM04	F	2026-11-13T21:27:30.000	4.9506421149681605	[223.00..224.99GHz,31250.00kHz,15.4mJy/beam@10km/s,941.5uJy/beam@native, XX YY] U [225.00..226.99GHz,31250.00kHz,14.8mJy/beam@10km/s,908.8uJy/beam@native, XX YY] U [239.00..240.98GHz,31250.00kHz,15.6mJy/beam@10km/s,988.4uJy/beam@native, XX YY] U [241.00..242.98GHz,31250.00kHz,16.4mJy/beam@10km/s,1mJy/beam@native, XX YY]	223.99324534537953	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	FBQS_J08_a_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	15.403220761011534	0.48333882341380324	1.8	uid://A001/X3833/X15ea	uid://A001/X3833/X15eb	uid://A002/X1315235/X1f4c2	Towards resolving orbiting binary supermassive black holes with the EHT	S	BANDPASS FLUX WVR	F	31.161568715761135	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X15eb.source.J0725-0054.spw.17	image	2		J0725-0054	111.46099963296886	-0.91570636944423	0.01190093036373538	Circle ICRS 111.461000 -0.915706 0.005950			128	1	2	4.9506421149681605	60988.319961	60988.326983	604.8	604.8	0.001244029947762064	0.0012543585721771732	7648.2500000032	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X15eb	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	217.6971242928812	7.227169550857697	6	1.626604075773299E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N604:CM11 N605:CM04	F	2026-11-13T21:27:30.000	4.9506421149681605	[223.00..224.99GHz,31250.00kHz,15.4mJy/beam@10km/s,941.5uJy/beam@native, XX YY] U [225.00..226.99GHz,31250.00kHz,14.8mJy/beam@10km/s,908.8uJy/beam@native, XX YY] U [239.00..240.98GHz,31250.00kHz,15.6mJy/beam@10km/s,988.4uJy/beam@native, XX YY] U [241.00..242.98GHz,31250.00kHz,16.4mJy/beam@10km/s,1mJy/beam@native, XX YY]	239.99276287004236	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	FBQS_J08_a_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	15.622451540732126	0.48333882341380324	1.8	uid://A001/X3833/X15ea	uid://A001/X3833/X15eb	uid://A002/X1315235/X1f4c2	Towards resolving orbiting binary supermassive black holes with the EHT	S	BANDPASS FLUX WVR	F	31.161568715761135	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X15eb.source.J0725-0054.spw.6	image	2		J0725-0054	111.46099963296886	-0.91570636944423	0.01190093036373538	Circle ICRS 111.461000 -0.915706 0.005950			128	1	2	4.9506421149681605	60988.319961	60988.326983	604.8	604.8	0.00132075690237936	0.0013324048400622309	7263.75	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X15eb	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	217.6971242928812	7.227169550857697	6	1.8343762100202865E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N604:CM11 N605:CM04	F	2026-11-13T21:27:30.000	4.9506421149681605	[223.00..224.99GHz,31250.00kHz,15.4mJy/beam@10km/s,941.5uJy/beam@native, XX YY] U [225.00..226.99GHz,31250.00kHz,14.8mJy/beam@10km/s,908.8uJy/beam@native, XX YY] U [239.00..240.98GHz,31250.00kHz,15.6mJy/beam@10km/s,988.4uJy/beam@native, XX YY] U [241.00..242.98GHz,31250.00kHz,16.4mJy/beam@10km/s,1mJy/beam@native, XX YY]	225.9931850358624	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	FBQS_J08_a_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	14.80244023754067	0.48333882341380324	1.8	uid://A001/X3833/X15ea	uid://A001/X3833/X15eb	uid://A002/X1315235/X1f4c2	Towards resolving orbiting binary supermassive black holes with the EHT	S	BANDPASS FLUX WVR	F	31.161568715761135	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X15eb.source.WISEA_J081854.88+200621.0.spw.17	image	2		WISEA_J081854.88+200621.0	124.72869999995608	20.105850000006264	0.011901329087536815	Circle ICRS 124.728700 20.105850 0.005951			128	1	2	5.482396792869407	60988.332905	60988.355402	362.88	362.88	0.0012440716272219643	0.0012544005976829929	7648.2500000032	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X15eb	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	203.3933350242121	27.90815244616626	6	1.6267130717266133E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N604:CM11 N605:CM04	F	2026-11-13T21:27:30.000	5.482396792869407	[222.99..224.98GHz,31250.00kHz,19.9mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [224.99..226.98GHz,31250.00kHz,19.1mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [238.99..240.98GHz,31250.00kHz,20.2mJy/beam@10km/s,1.3mJy/beam@native, XX YY] U [240.99..242.98GHz,31250.00kHz,21.2mJy/beam@10km/s,1.3mJy/beam@native, XX YY]	239.9847225221094	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	FBQS_J08_a_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	20.168781366977086	0.6239861511051453	1.8	uid://A001/X3833/X15ea	uid://A001/X3833/X15eb	uid://A002/X1315235/X1f4c2	Towards resolving orbiting binary supermassive black holes with the EHT	S	TARGET	T	35.09976216338559	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X15eb.source.WISEA_J081854.88+200621.0.spw.6	image	2		WISEA_J081854.88+200621.0	124.72869999995608	20.105850000006264	0.011901329087536815	Circle ICRS 124.728700 20.105850 0.005951			128	1	2	5.482396792869407	60988.332905	60988.355402	362.88	362.88	0.0013208011524671092	0.0013324494803976202	7263.75	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X15eb	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	203.3933350242121	27.90815244616626	6	1.8344991284284756E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N604:CM11 N605:CM04	F	2026-11-13T21:27:30.000	5.482396792869407	[222.99..224.98GHz,31250.00kHz,19.9mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [224.99..226.98GHz,31250.00kHz,19.1mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [238.99..240.98GHz,31250.00kHz,20.2mJy/beam@10km/s,1.3mJy/beam@native, XX YY] U [240.99..242.98GHz,31250.00kHz,21.2mJy/beam@10km/s,1.3mJy/beam@native, XX YY]	225.98561370822551	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	FBQS_J08_a_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	19.1101423348901	0.6239861511051453	1.8	uid://A001/X3833/X15ea	uid://A001/X3833/X15eb	uid://A002/X1315235/X1f4c2	Towards resolving orbiting binary supermassive black holes with the EHT	S	TARGET	T	35.09976216338559	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X15eb.source.WISEA_J081854.88+200621.0.spw.14	image	2		WISEA_J081854.88+200621.0	124.72869999995608	20.105850000006264	0.011901329087536815	Circle ICRS 124.728700 20.105850 0.005951			128	1	2	5.482396792869407	60988.332905	60988.355402	362.88	362.88	0.0013325420148239454	0.0013443992813072221	7199.7500000032	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X15eb	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	203.3933350242121	27.90815244616626	6	1.867404932182481E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N604:CM11 N605:CM04	F	2026-11-13T21:27:30.000	5.482396792869407	[222.99..224.98GHz,31250.00kHz,19.9mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [224.99..226.98GHz,31250.00kHz,19.1mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [238.99..240.98GHz,31250.00kHz,20.2mJy/beam@10km/s,1.3mJy/beam@native, XX YY] U [240.99..242.98GHz,31250.00kHz,21.2mJy/beam@10km/s,1.3mJy/beam@native, XX YY]	223.98574102064208	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	FBQS_J08_a_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	19.88575862558275	0.6239861511051453	1.8	uid://A001/X3833/X15ea	uid://A001/X3833/X15eb	uid://A002/X1315235/X1f4c2	Towards resolving orbiting binary supermassive black holes with the EHT	S	TARGET	T	35.09976216338559	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X15eb.source.WISEA_J081854.88+200621.0.spw.10	image	2		WISEA_J081854.88+200621.0	124.72869999995608	20.105850000006264	0.011901329087536815	Circle ICRS 124.728700 20.105850 0.005951			128	1	2	5.482396792869407	60988.332905	60988.355402	362.88	362.88	0.0012338320253651369	0.0012439909716662405	7712.25	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X15eb	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	203.3933350242121	27.90815244616626	6	1.5999359089394004E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N604:CM11 N605:CM04	F	2026-11-13T21:27:30.000	5.482396792869407	[222.99..224.98GHz,31250.00kHz,19.9mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [224.99..226.98GHz,31250.00kHz,19.1mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [238.99..240.98GHz,31250.00kHz,20.2mJy/beam@10km/s,1.3mJy/beam@native, XX YY] U [240.99..242.98GHz,31250.00kHz,21.2mJy/beam@10km/s,1.3mJy/beam@native, XX YY]	241.98459520969283	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	FBQS_J08_a_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	21.211927896436936	0.6239861511051453	1.8	uid://A001/X3833/X15ea	uid://A001/X3833/X15eb	uid://A002/X1315235/X1f4c2	Towards resolving orbiting binary supermassive black holes with the EHT	S	TARGET	T	35.09976216338559	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01682.S	ALMA	JAO	ALMA	uid://A001/X3788/X8525.source.SDSS_J085837.68+182223.3.spw.21	cube	2		SDSS_J085837.68+182223.3	134.65705800001496	18.373097000000584	0.015879447837558288	Circle ICRS 134.657058 18.373097 0.007940			1920	1	2	0.3723831905607873	60795.975374	60796.002675	1844.64	1844.64	0.0027304602584227893	0.002777879999729741	95585.8970051161	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3788/X8525	application/x-votable+xml; content=datalink		2024.1.01682.S	Public	209.2073309994537	36.07011625880002	3	2.8561861919530593E-8	1.875E9	A007:DV20 A011:DV01 A015:DA52 A022:DA47 A024:DV02 A027:DV03 A042:DV04 A043:DV13 A045:DA65 A047:DA42 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DA61 A073:DA41 A074:DV14 A075:DV22 A076:DA56 A082:DA58 A083:DV08 A085:DV05 A086:DA64 A087:DA50 A088:DA54 A089:DA48 A090:DV09 A092:DA43 A093:DA57 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A108:DV24 A110:DA51 A111:DV19 A115:DV12 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A128:DA60 A134:DV10 A135:DV15	F	2026-06-06T17:54:12.000	0.3723831905607873	[93.93..95.91GHz,31250.00kHz,485.9uJy/beam@10km/s,19.3uJy/beam@native, XX YY] U [95.88..97.87GHz,31250.00kHz,474.5uJy/beam@10km/s,19.1uJy/beam@native, XX YY] U [105.98..107.86GHz,1128.91kHz,490uJy/beam@10km/s,21.4uJy/beam@native, XX YY] U [107.92..109.80GHz,1128.91kHz,533.3uJy/beam@10km/s,23.5uJy/beam@native, XX YY]	108.8584449094137	3136.3670519716316	ALMA						J0858+1822 is an exceptionally rare triple AGN system, at z~0.059, currently in its advanced merger stage since it is could be the first triple AGN detected in a cosmic void. This triple AGN system provide a unique opportunity to gain insight into the accretion activity and surroundings of the AGNs before they reach the gravitationally bound triple phase. Optical data classified this systems as a dual AGN, but a recent multiwavelength analysis searching for multiple active galactic nucleus (AGN) systems in nearby (z<0.077) triple galaxy mergers pointed the possitiblity of being a triple sytems. Recent HST observations show a triple nucleus and a preliminary study with MUSE-WFM observations also show this third nucleus. However, the available CO NOEMA observations do not have the enought resolution to resolve the system. Here, we propose spatially-resolved continumm ALMA observations of J0858+1822 to validate the AGN nature of the three nuclei confirming the detection of the first triple AGN in a cosmic void.	SDSS_J08_a_03_TM2	Koss, Michael; Sanders, David; Comerford, Julia; Droguett, Macarena; Ricci, Claudio; Urry, Meg; U, Vivian; Muller-Sanchez, Francisco; Borlaff, Alejandro; Barcos-Munoz, Loreto; Treister, Ezequiel; Privon, George; Evans, Aaron; Bauer, Franz; Yoon, Ilsang;	0.5333270815926796	0.010298098322736315	1.053873	uid://A001/X3788/X8522	uid://A001/X3788/X8525	uid://A002/X1284805/X9293	Cosmic secrets: observing the first triple AGN system in a cosmic void	S	TARGET	T	6.717620334831707	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Merging and interacting galaxies	Active galaxies	imoralc	del Moral-Castro, Ignacio	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01682.S	ALMA	JAO	ALMA	uid://A001/X3788/X8525.source.SDSS_J085837.68+182223.3.spw.5	image	2		SDSS_J085837.68+182223.3	134.65705800001496	18.373097000000584	0.015879447837558288	Circle ICRS 134.657058 18.373097 0.007940			128	1	2	0.3723831905607873	60795.975374	60796.002675	1844.64	1844.64	0.003125777018633688	0.0031918243921240067	3068.7192872186297	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3788/X8525	application/x-votable+xml; content=datalink		2024.1.01682.S	Public	209.2073309994537	36.07011625880002	3	1.039983147734789E-6	2.0E9	A007:DV20 A011:DV01 A015:DA52 A022:DA47 A024:DV02 A027:DV03 A042:DV04 A043:DV13 A045:DA65 A047:DA42 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DA61 A073:DA41 A074:DV14 A075:DV22 A076:DA56 A082:DA58 A083:DV08 A085:DV05 A086:DA64 A087:DA50 A088:DA54 A089:DA48 A090:DV09 A092:DA43 A093:DA57 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A108:DV24 A110:DA51 A111:DV19 A115:DV12 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A128:DA60 A134:DV10 A135:DV15	F	2026-06-06T17:54:12.000	0.3723831905607873	[93.93..95.91GHz,31250.00kHz,485.9uJy/beam@10km/s,19.3uJy/beam@native, XX YY] U [95.88..97.87GHz,31250.00kHz,474.5uJy/beam@10km/s,19.1uJy/beam@native, XX YY] U [105.98..107.86GHz,1128.91kHz,490uJy/beam@10km/s,21.4uJy/beam@native, XX YY] U [107.92..109.80GHz,1128.91kHz,533.3uJy/beam@10km/s,23.5uJy/beam@native, XX YY]	94.91742463144428	3136.3670519716316	ALMA						J0858+1822 is an exceptionally rare triple AGN system, at z~0.059, currently in its advanced merger stage since it is could be the first triple AGN detected in a cosmic void. This triple AGN system provide a unique opportunity to gain insight into the accretion activity and surroundings of the AGNs before they reach the gravitationally bound triple phase. Optical data classified this systems as a dual AGN, but a recent multiwavelength analysis searching for multiple active galactic nucleus (AGN) systems in nearby (z<0.077) triple galaxy mergers pointed the possitiblity of being a triple sytems. Recent HST observations show a triple nucleus and a preliminary study with MUSE-WFM observations also show this third nucleus. However, the available CO NOEMA observations do not have the enought resolution to resolve the system. Here, we propose spatially-resolved continumm ALMA observations of J0858+1822 to validate the AGN nature of the three nuclei confirming the detection of the first triple AGN in a cosmic void.	SDSS_J08_a_03_TM2	Koss, Michael; Sanders, David; Comerford, Julia; Droguett, Macarena; Ricci, Claudio; Urry, Meg; U, Vivian; Muller-Sanchez, Francisco; Borlaff, Alejandro; Barcos-Munoz, Loreto; Treister, Ezequiel; Privon, George; Evans, Aaron; Bauer, Franz; Yoon, Ilsang;	0.485936623733902	0.010298098322736315	1.053873	uid://A001/X3788/X8522	uid://A001/X3788/X8525	uid://A002/X1284805/X9293	Cosmic secrets: observing the first triple AGN system in a cosmic void	S	TARGET	T	6.717620334831707	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Merging and interacting galaxies	Active galaxies	imoralc	del Moral-Castro, Ignacio	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01682.S	ALMA	JAO	ALMA	uid://A001/X3788/X8525.source.SDSS_J085837.68+182223.3.spw.7	image	2		SDSS_J085837.68+182223.3	134.65705800001496	18.373097000000584	0.015879447837558288	Circle ICRS 134.657058 18.373097 0.007940			128	1	2	0.3723831905607873	60795.975374	60796.002675	1844.64	1844.64	0.0030632330349473795	0.0031266369479191827	3131.37528721863	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3788/X8525	application/x-votable+xml; content=datalink		2024.1.01682.S	Public	209.2073309994537	36.07011625880002	3	9.983591701914466E-7	2.0E9	A007:DV20 A011:DV01 A015:DA52 A022:DA47 A024:DV02 A027:DV03 A042:DV04 A043:DV13 A045:DA65 A047:DA42 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DA61 A073:DA41 A074:DV14 A075:DV22 A076:DA56 A082:DA58 A083:DV08 A085:DV05 A086:DA64 A087:DA50 A088:DA54 A089:DA48 A090:DV09 A092:DA43 A093:DA57 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A108:DV24 A110:DA51 A111:DV19 A115:DV12 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A128:DA60 A134:DV10 A135:DV15	F	2026-06-06T17:54:12.000	0.3723831905607873	[93.93..95.91GHz,31250.00kHz,485.9uJy/beam@10km/s,19.3uJy/beam@native, XX YY] U [95.88..97.87GHz,31250.00kHz,474.5uJy/beam@10km/s,19.1uJy/beam@native, XX YY] U [105.98..107.86GHz,1128.91kHz,490uJy/beam@10km/s,21.4uJy/beam@native, XX YY] U [107.92..109.80GHz,1128.91kHz,533.3uJy/beam@10km/s,23.5uJy/beam@native, XX YY]	96.8756749775169	3136.3670519716316	ALMA						J0858+1822 is an exceptionally rare triple AGN system, at z~0.059, currently in its advanced merger stage since it is could be the first triple AGN detected in a cosmic void. This triple AGN system provide a unique opportunity to gain insight into the accretion activity and surroundings of the AGNs before they reach the gravitationally bound triple phase. Optical data classified this systems as a dual AGN, but a recent multiwavelength analysis searching for multiple active galactic nucleus (AGN) systems in nearby (z<0.077) triple galaxy mergers pointed the possitiblity of being a triple sytems. Recent HST observations show a triple nucleus and a preliminary study with MUSE-WFM observations also show this third nucleus. However, the available CO NOEMA observations do not have the enought resolution to resolve the system. Here, we propose spatially-resolved continumm ALMA observations of J0858+1822 to validate the AGN nature of the three nuclei confirming the detection of the first triple AGN in a cosmic void.	SDSS_J08_a_03_TM2	Koss, Michael; Sanders, David; Comerford, Julia; Droguett, Macarena; Ricci, Claudio; Urry, Meg; U, Vivian; Muller-Sanchez, Francisco; Borlaff, Alejandro; Barcos-Munoz, Loreto; Treister, Ezequiel; Privon, George; Evans, Aaron; Bauer, Franz; Yoon, Ilsang;	0.4744565926534937	0.010298098322736315	1.053873	uid://A001/X3788/X8522	uid://A001/X3788/X8525	uid://A002/X1284805/X9293	Cosmic secrets: observing the first triple AGN system in a cosmic void	S	TARGET	T	6.717620334831707	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Merging and interacting galaxies	Active galaxies	imoralc	del Moral-Castro, Ignacio	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01682.S	ALMA	JAO	ALMA	uid://A001/X3788/X8525.source.SDSS_J085837.68+182223.3.spw.19	cube	2		SDSS_J085837.68+182223.3	134.65705800001496	18.373097000000584	0.015879447837558288	Circle ICRS 134.657058 18.373097 0.007940			1920	1	2	0.3723831905607873	60795.975374	60796.002675	1844.64	1844.64	0.002779559844468943	0.0028287156896696633	93868.09445587902	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3788/X8525	application/x-votable+xml; content=datalink		2024.1.01682.S	Public	209.2073309994537	36.07011625880002	3	2.960755213894357E-8	1.875E9	A007:DV20 A011:DV01 A015:DA52 A022:DA47 A024:DV02 A027:DV03 A042:DV04 A043:DV13 A045:DA65 A047:DA42 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DA61 A073:DA41 A074:DV14 A075:DV22 A076:DA56 A082:DA58 A083:DV08 A085:DV05 A086:DA64 A087:DA50 A088:DA54 A089:DA48 A090:DV09 A092:DA43 A093:DA57 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A108:DV24 A110:DA51 A111:DV19 A115:DV12 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A128:DA60 A134:DV10 A135:DV15	F	2026-06-06T17:54:12.000	0.3723831905607873	[93.93..95.91GHz,31250.00kHz,485.9uJy/beam@10km/s,19.3uJy/beam@native, XX YY] U [95.88..97.87GHz,31250.00kHz,474.5uJy/beam@10km/s,19.1uJy/beam@native, XX YY] U [105.98..107.86GHz,1128.91kHz,490uJy/beam@10km/s,21.4uJy/beam@native, XX YY] U [107.92..109.80GHz,1128.91kHz,533.3uJy/beam@10km/s,23.5uJy/beam@native, XX YY]	106.91895892810992	3136.3670519716316	ALMA						J0858+1822 is an exceptionally rare triple AGN system, at z~0.059, currently in its advanced merger stage since it is could be the first triple AGN detected in a cosmic void. This triple AGN system provide a unique opportunity to gain insight into the accretion activity and surroundings of the AGNs before they reach the gravitationally bound triple phase. Optical data classified this systems as a dual AGN, but a recent multiwavelength analysis searching for multiple active galactic nucleus (AGN) systems in nearby (z<0.077) triple galaxy mergers pointed the possitiblity of being a triple sytems. Recent HST observations show a triple nucleus and a preliminary study with MUSE-WFM observations also show this third nucleus. However, the available CO NOEMA observations do not have the enought resolution to resolve the system. Here, we propose spatially-resolved continumm ALMA observations of J0858+1822 to validate the AGN nature of the three nuclei confirming the detection of the first triple AGN in a cosmic void.	SDSS_J08_a_03_TM2	Koss, Michael; Sanders, David; Comerford, Julia; Droguett, Macarena; Ricci, Claudio; Urry, Meg; U, Vivian; Muller-Sanchez, Francisco; Borlaff, Alejandro; Barcos-Munoz, Loreto; Treister, Ezequiel; Privon, George; Evans, Aaron; Bauer, Franz; Yoon, Ilsang;	0.490019920673109	0.010298098322736315	1.053873	uid://A001/X3788/X8522	uid://A001/X3788/X8525	uid://A002/X1284805/X9293	Cosmic secrets: observing the first triple AGN system in a cosmic void	S	TARGET	T	6.717620334831707	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Merging and interacting galaxies	Active galaxies	imoralc	del Moral-Castro, Ignacio	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00357.S	ALMA	JAO	ALMA	uid://A001/X2d8/Xb4.source.J1047-6217.spw.27	cube	2		J1047-6217	161.9289679125	-62.28739823611111	0.007220075023862902	Circle ICRS 161.928968 -62.287398 0.003610			3840	1	2	0.055168674979289845	57368.203723	57373.427151	725.76	725.76	0.0012924664052860486	0.001302996989419713	235602.08660780868	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d8/Xb4	application/x-votable+xml; content=datalink		2015.1.00357.S	Public	289.08603142568177	-2.7890621558950017	6	5.48582584382661E-9	1.875E9	A001:DA59 A002:DA49 A003:DV23 A004:DA41 A005:DA54 A006:DA61 A007:DV02 A009:DV18 A014:DV22 A015:DV04 A018:DA52 A020:DV03 A025:DA57 A027:DV07 A030:DA65 A033:DV20 A035:DA62 A037:DV19 A038:DA50 A039:DA63 A047:DA55 A049:DV11 A064:DV13 A098:DV10 A101:DV12 A103:DV03 A104:DA44 A114:DA53 A115:DV11 A117:DA56 A118:DV05 A119:DV06 A122:DA58 A123:DA43 A125:DA47 A126:DV25 A128:DV15 A129:DV16 A130:DV09 A131:DA51 A132:DV24 A135:DA45 P401:DA48 P403:DV21 P404:DV01 S301:DA42 W207:DA60 W208:DV14	F	2018-03-13T00:00:00.000	0.055168674979289845	[216.10..216.16GHz,141.11kHz,2mJy/beam@10km/s,689uJy/beam@native, XX YY] U [216.93..216.99GHz,141.11kHz,2mJy/beam@10km/s,689.2uJy/beam@native, XX YY] U [217.09..217.15GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [217.22..217.28GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [219.55..219.61GHz,35.28kHz,1.9mJy/beam@10km/s,681.1uJy/beam@native, XX YY] U [230.08..231.95GHz,976.56kHz,1.9mJy/beam@10km/s,122.7uJy/beam@native, XX YY] U [231.31..231.37GHz,35.28kHz,1.9mJy/beam@10km/s,693.9uJy/beam@native, XX YY]	231.01646803504116	45.72294173220015	ALMA	Gas Kinematics of the Massive Protocluster G286.21+0.17 Revealed by ALMA Offline Correction of Atmospheric Effects on Single-dish Radio Spectroscopy The Core Mass Function in the Massive Protocluster G286.21+0.17 Revealed by ALMA	Cheng, Yu Sawada, Tsuyoshi	Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Kong, Shuo; Lim, Wanggi; Andersen, Morten; Da Rio, Nicola Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Lim, Wanggi; Andersen, Morten Sawada, Tsuyoshi; Chang, Chin-Shin; Francke, Harold; Gomez, Laura; Mangum, Jeffrey G.; Miyamoto, Yusuke; Nakazato, Takeshi; Nishie, Suminori; Phillips, Neil M.; Shimajiri, Yoshito; Sugimoto, Kanako	We present a method to mitigate the atmospheric effects (residual atmospheric lines) in single-dish radio spectroscopy caused by the elevation difference between the target and reference positions. The method is developed as a script using the Atmospheric Transmission at Microwaves (ATM) library built into the Common Astronomy Software Applications (CASA) package. We apply the method to the data taken with the Total Power Array of the Atacama Large Millimeter/submillimeter Array. The intensities of the residual atmospheric (mostly O<SUB>3</SUB>) lines are suppressed by, typically, an order of magnitude for the tested cases. The parameters for the ATM model can be optimized to minimize the residual line and, for a specific O<SUB>3</SUB> line at 231.28 GHz, a seasonal dependence of a best-fitting model parameter is demonstrated. The method will be provided as a task within the CASA package in the near future. The atmospheric removal method we developed can be used by any radio/millimeter/submillimeter observato	2018	We propose to study the kinematics of gas in a massive protocluster, G286.21+0.17, that is the target of an ongoing HST study of proper motion kinematics of young stellar objects. The unique comparisons that will be possible between ALMA-derived gas kinematics and HST-derived young stellar object (YSO) kinematics will help answer fundamental questions associated with massive star cluster formation, such as: "What is the nature of spatial and kinematic substructure in gas and YSOs and how do they compare?" "What is the level of turbulent velocity dispersion of gas in comparison to stellar motions, and the implications for global support of the protocluster and thus the timescale of star cluster formation?". The ALMA observations will identify populations of dense cores in different tracers, which can be compared in terms of their spatial, kinematic and core mass function properties, to similar approved Cycle 2 observations of cores in a massive IRDC, thus probing different evolutionary stages of the massive st	G286_a_1_06_TE	Lim, Wanggi; Kong, Shuo; Liu, Mengyao; Da Rio, Nicola; Andersen, Morten;	1.9132406278844714	0.11241979345273205	0.7534055	uid://A001/X2d8/Xb3	uid://A001/X2d8/Xb4	uid://A002/Xadabcb/X1102	Kinematics of Massive Star Cluster in Formation	S	PHASE WVR	F	7.423453235210456	T	2018ApJ...853..160C 2020ApJ...894...87C 2021PASP..133c4504S	High-mass star formation;Inter-Stellar Medium (ISM)/Molecular clouds	ISM and star formation	jtan	Tan, Jonathan	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00357.S	ALMA	JAO	ALMA	uid://A001/X2d8/Xb4.source.J1047-6217.spw.29	cube	2		J1047-6217	161.9289679125	-62.28739823611111	0.007220075023862902	Circle ICRS 161.928968 -62.287398 0.003610			1920	1	2	0.055168674979289845	57368.203723	57373.427151	725.76	725.76	0.0013651420142273142	0.0013655067716440879	6224961.377697545	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d8/Xb4	application/x-votable+xml; content=datalink		2015.1.00357.S	Public	289.08603142568177	-2.7890621558950017	6	2.1936073230582368E-10	5.859375E7	A001:DA59 A002:DA49 A003:DV23 A004:DA41 A005:DA54 A006:DA61 A007:DV02 A009:DV18 A014:DV22 A015:DV04 A018:DA52 A020:DV03 A025:DA57 A027:DV07 A030:DA65 A033:DV20 A035:DA62 A037:DV19 A038:DA50 A039:DA63 A047:DA55 A049:DV11 A064:DV13 A098:DV10 A101:DV12 A103:DV03 A104:DA44 A114:DA53 A115:DV11 A117:DA56 A118:DV05 A119:DV06 A122:DA58 A123:DA43 A125:DA47 A126:DV25 A128:DV15 A129:DV16 A130:DV09 A131:DA51 A132:DV24 A135:DA45 P401:DA48 P403:DV21 P404:DV01 S301:DA42 W207:DA60 W208:DV14	F	2018-03-13T00:00:00.000	0.055168674979289845	[216.10..216.16GHz,141.11kHz,2mJy/beam@10km/s,689uJy/beam@native, XX YY] U [216.93..216.99GHz,141.11kHz,2mJy/beam@10km/s,689.2uJy/beam@native, XX YY] U [217.09..217.15GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [217.22..217.28GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [219.55..219.61GHz,35.28kHz,1.9mJy/beam@10km/s,681.1uJy/beam@native, XX YY] U [230.08..231.95GHz,976.56kHz,1.9mJy/beam@10km/s,122.7uJy/beam@native, XX YY] U [231.31..231.37GHz,35.28kHz,1.9mJy/beam@10km/s,693.9uJy/beam@native, XX YY]	219.5759959321422	45.72294173220015	ALMA	Gas Kinematics of the Massive Protocluster G286.21+0.17 Revealed by ALMA Offline Correction of Atmospheric Effects on Single-dish Radio Spectroscopy The Core Mass Function in the Massive Protocluster G286.21+0.17 Revealed by ALMA	Cheng, Yu Sawada, Tsuyoshi	Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Kong, Shuo; Lim, Wanggi; Andersen, Morten; Da Rio, Nicola Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Lim, Wanggi; Andersen, Morten Sawada, Tsuyoshi; Chang, Chin-Shin; Francke, Harold; Gomez, Laura; Mangum, Jeffrey G.; Miyamoto, Yusuke; Nakazato, Takeshi; Nishie, Suminori; Phillips, Neil M.; Shimajiri, Yoshito; Sugimoto, Kanako	We present a method to mitigate the atmospheric effects (residual atmospheric lines) in single-dish radio spectroscopy caused by the elevation difference between the target and reference positions. The method is developed as a script using the Atmospheric Transmission at Microwaves (ATM) library built into the Common Astronomy Software Applications (CASA) package. We apply the method to the data taken with the Total Power Array of the Atacama Large Millimeter/submillimeter Array. The intensities of the residual atmospheric (mostly O<SUB>3</SUB>) lines are suppressed by, typically, an order of magnitude for the tested cases. The parameters for the ATM model can be optimized to minimize the residual line and, for a specific O<SUB>3</SUB> line at 231.28 GHz, a seasonal dependence of a best-fitting model parameter is demonstrated. The method will be provided as a task within the CASA package in the near future. The atmospheric removal method we developed can be used by any radio/millimeter/submillimeter observato	2018	We propose to study the kinematics of gas in a massive protocluster, G286.21+0.17, that is the target of an ongoing HST study of proper motion kinematics of young stellar objects. The unique comparisons that will be possible between ALMA-derived gas kinematics and HST-derived young stellar object (YSO) kinematics will help answer fundamental questions associated with massive star cluster formation, such as: "What is the nature of spatial and kinematic substructure in gas and YSOs and how do they compare?" "What is the level of turbulent velocity dispersion of gas in comparison to stellar motions, and the implications for global support of the protocluster and thus the timescale of star cluster formation?". The ALMA observations will identify populations of dense cores in different tracers, which can be compared in terms of their spatial, kinematic and core mass function properties, to similar approved Cycle 2 observations of cores in a massive IRDC, thus probing different evolutionary stages of the massive st	G286_a_1_06_TE	Lim, Wanggi; Kong, Shuo; Liu, Mengyao; Da Rio, Nicola; Andersen, Morten;	1.92651466972291	0.11241979345273205	0.7534055	uid://A001/X2d8/Xb3	uid://A001/X2d8/Xb4	uid://A002/Xadabcb/X1102	Kinematics of Massive Star Cluster in Formation	S	PHASE WVR	F	7.423453235210456	T	2018ApJ...853..160C 2020ApJ...894...87C 2021PASP..133c4504S	High-mass star formation;Inter-Stellar Medium (ISM)/Molecular clouds	ISM and star formation	jtan	Tan, Jonathan	35.2783203125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00357.S	ALMA	JAO	ALMA	uid://A001/X2d8/Xb4.source.J1047-6217.spw.25	cube	2		J1047-6217	161.9289679125	-62.28739823611111	0.007220075023862902	Circle ICRS 161.928968 -62.287398 0.003610			1920	1	2	0.055168674979289845	57368.203723	57373.427151	725.76	725.76	0.0012957403925492553	0.0012960690815066475	6556718.501532299	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d8/Xb4	application/x-votable+xml; content=datalink		2015.1.00357.S	Public	289.08603142568177	-2.7890621558950017	6	1.9762111439504036E-10	5.859375E7	A001:DA59 A002:DA49 A003:DV23 A004:DA41 A005:DA54 A006:DA61 A007:DV02 A009:DV18 A014:DV22 A015:DV04 A018:DA52 A020:DV03 A025:DA57 A027:DV07 A030:DA65 A033:DV20 A035:DA62 A037:DV19 A038:DA50 A039:DA63 A047:DA55 A049:DV11 A064:DV13 A098:DV10 A101:DV12 A103:DV03 A104:DA44 A114:DA53 A115:DV11 A117:DA56 A118:DV05 A119:DV06 A122:DA58 A123:DA43 A125:DA47 A126:DV25 A128:DV15 A129:DV16 A130:DV09 A131:DA51 A132:DV24 A135:DA45 P401:DA48 P403:DV21 P404:DV01 S301:DA42 W207:DA60 W208:DV14	F	2018-03-13T00:00:00.000	0.055168674979289845	[216.10..216.16GHz,141.11kHz,2mJy/beam@10km/s,689uJy/beam@native, XX YY] U [216.93..216.99GHz,141.11kHz,2mJy/beam@10km/s,689.2uJy/beam@native, XX YY] U [217.09..217.15GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [217.22..217.28GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [219.55..219.61GHz,35.28kHz,1.9mJy/beam@10km/s,681.1uJy/beam@native, XX YY] U [230.08..231.95GHz,976.56kHz,1.9mJy/beam@10km/s,122.7uJy/beam@native, XX YY] U [231.31..231.37GHz,35.28kHz,1.9mJy/beam@10km/s,693.9uJy/beam@native, XX YY]	231.3383493829013	45.72294173220015	ALMA	Gas Kinematics of the Massive Protocluster G286.21+0.17 Revealed by ALMA Offline Correction of Atmospheric Effects on Single-dish Radio Spectroscopy The Core Mass Function in the Massive Protocluster G286.21+0.17 Revealed by ALMA	Cheng, Yu Sawada, Tsuyoshi	Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Kong, Shuo; Lim, Wanggi; Andersen, Morten; Da Rio, Nicola Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Lim, Wanggi; Andersen, Morten Sawada, Tsuyoshi; Chang, Chin-Shin; Francke, Harold; Gomez, Laura; Mangum, Jeffrey G.; Miyamoto, Yusuke; Nakazato, Takeshi; Nishie, Suminori; Phillips, Neil M.; Shimajiri, Yoshito; Sugimoto, Kanako	We present a method to mitigate the atmospheric effects (residual atmospheric lines) in single-dish radio spectroscopy caused by the elevation difference between the target and reference positions. The method is developed as a script using the Atmospheric Transmission at Microwaves (ATM) library built into the Common Astronomy Software Applications (CASA) package. We apply the method to the data taken with the Total Power Array of the Atacama Large Millimeter/submillimeter Array. The intensities of the residual atmospheric (mostly O<SUB>3</SUB>) lines are suppressed by, typically, an order of magnitude for the tested cases. The parameters for the ATM model can be optimized to minimize the residual line and, for a specific O<SUB>3</SUB> line at 231.28 GHz, a seasonal dependence of a best-fitting model parameter is demonstrated. The method will be provided as a task within the CASA package in the near future. The atmospheric removal method we developed can be used by any radio/millimeter/submillimeter observato	2018	We propose to study the kinematics of gas in a massive protocluster, G286.21+0.17, that is the target of an ongoing HST study of proper motion kinematics of young stellar objects. The unique comparisons that will be possible between ALMA-derived gas kinematics and HST-derived young stellar object (YSO) kinematics will help answer fundamental questions associated with massive star cluster formation, such as: "What is the nature of spatial and kinematic substructure in gas and YSOs and how do they compare?" "What is the level of turbulent velocity dispersion of gas in comparison to stellar motions, and the implications for global support of the protocluster and thus the timescale of star cluster formation?". The ALMA observations will identify populations of dense cores in different tracers, which can be compared in terms of their spatial, kinematic and core mass function properties, to similar approved Cycle 2 observations of cores in a massive IRDC, thus probing different evolutionary stages of the massive st	G286_a_1_06_TE	Lim, Wanggi; Kong, Shuo; Liu, Mengyao; Da Rio, Nicola; Andersen, Morten;	1.9122216220014678	0.11241979345273205	0.7534055	uid://A001/X2d8/Xb3	uid://A001/X2d8/Xb4	uid://A002/Xadabcb/X1102	Kinematics of Massive Star Cluster in Formation	S	PHASE WVR	F	7.423453235210456	T	2018ApJ...853..160C 2020ApJ...894...87C 2021PASP..133c4504S	High-mass star formation;Inter-Stellar Medium (ISM)/Molecular clouds	ISM and star formation	jtan	Tan, Jonathan	35.2783203125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00357.S	ALMA	JAO	ALMA	uid://A001/X2d8/Xb4.source.J1047-6217.spw.33	cube	2		J1047-6217	161.9289679125	-62.28739823611111	0.007220075023862902	Circle ICRS 161.928968 -62.287398 0.003610			480	1	2	0.055168674979289845	57368.203723	57373.427151	725.76	725.76	0.001381593602755006	0.0013819665396231594	1537709.2006425904	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d8/Xb4	application/x-votable+xml; content=datalink		2015.1.00357.S	Public	289.08603142568177	-2.7890621558950017	6	8.987212883765535E-10	5.859375E7	A001:DA59 A002:DA49 A003:DV23 A004:DA41 A005:DA54 A006:DA61 A007:DV02 A009:DV18 A014:DV22 A015:DV04 A018:DA52 A020:DV03 A025:DA57 A027:DV07 A030:DA65 A033:DV20 A035:DA62 A037:DV19 A038:DA50 A039:DA63 A047:DA55 A049:DV11 A064:DV13 A098:DV10 A101:DV12 A103:DV03 A104:DA44 A114:DA53 A115:DV11 A117:DA56 A118:DV05 A119:DV06 A122:DA58 A123:DA43 A125:DA47 A126:DV25 A128:DV15 A129:DV16 A130:DV09 A131:DA51 A132:DV24 A135:DA45 P401:DA48 P403:DV21 P404:DV01 S301:DA42 W207:DA60 W208:DV14	F	2018-03-13T00:00:00.000	0.055168674979289845	[216.10..216.16GHz,141.11kHz,2mJy/beam@10km/s,689uJy/beam@native, XX YY] U [216.93..216.99GHz,141.11kHz,2mJy/beam@10km/s,689.2uJy/beam@native, XX YY] U [217.09..217.15GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [217.22..217.28GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [219.55..219.61GHz,35.28kHz,1.9mJy/beam@10km/s,681.1uJy/beam@native, XX YY] U [230.08..231.95GHz,976.56kHz,1.9mJy/beam@10km/s,122.7uJy/beam@native, XX YY] U [231.31..231.37GHz,35.28kHz,1.9mJy/beam@10km/s,693.9uJy/beam@native, XX YY]	216.96105603949215	45.72294173220015	ALMA	Gas Kinematics of the Massive Protocluster G286.21+0.17 Revealed by ALMA Offline Correction of Atmospheric Effects on Single-dish Radio Spectroscopy The Core Mass Function in the Massive Protocluster G286.21+0.17 Revealed by ALMA	Cheng, Yu Sawada, Tsuyoshi	Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Kong, Shuo; Lim, Wanggi; Andersen, Morten; Da Rio, Nicola Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Lim, Wanggi; Andersen, Morten Sawada, Tsuyoshi; Chang, Chin-Shin; Francke, Harold; Gomez, Laura; Mangum, Jeffrey G.; Miyamoto, Yusuke; Nakazato, Takeshi; Nishie, Suminori; Phillips, Neil M.; Shimajiri, Yoshito; Sugimoto, Kanako	We present a method to mitigate the atmospheric effects (residual atmospheric lines) in single-dish radio spectroscopy caused by the elevation difference between the target and reference positions. The method is developed as a script using the Atmospheric Transmission at Microwaves (ATM) library built into the Common Astronomy Software Applications (CASA) package. We apply the method to the data taken with the Total Power Array of the Atacama Large Millimeter/submillimeter Array. The intensities of the residual atmospheric (mostly O<SUB>3</SUB>) lines are suppressed by, typically, an order of magnitude for the tested cases. The parameters for the ATM model can be optimized to minimize the residual line and, for a specific O<SUB>3</SUB> line at 231.28 GHz, a seasonal dependence of a best-fitting model parameter is demonstrated. The method will be provided as a task within the CASA package in the near future. The atmospheric removal method we developed can be used by any radio/millimeter/submillimeter observato	2018	We propose to study the kinematics of gas in a massive protocluster, G286.21+0.17, that is the target of an ongoing HST study of proper motion kinematics of young stellar objects. The unique comparisons that will be possible between ALMA-derived gas kinematics and HST-derived young stellar object (YSO) kinematics will help answer fundamental questions associated with massive star cluster formation, such as: "What is the nature of spatial and kinematic substructure in gas and YSOs and how do they compare?" "What is the level of turbulent velocity dispersion of gas in comparison to stellar motions, and the implications for global support of the protocluster and thus the timescale of star cluster formation?". The ALMA observations will identify populations of dense cores in different tracers, which can be compared in terms of their spatial, kinematic and core mass function properties, to similar approved Cycle 2 observations of cores in a massive IRDC, thus probing different evolutionary stages of the massive st	G286_a_1_06_TE	Lim, Wanggi; Kong, Shuo; Liu, Mengyao; Da Rio, Nicola; Andersen, Morten;	1.9611695910485551	0.11241979345273205	0.7534055	uid://A001/X2d8/Xb3	uid://A001/X2d8/Xb4	uid://A002/Xadabcb/X1102	Kinematics of Massive Star Cluster in Formation	S	PHASE WVR	F	7.423453235210456	T	2018ApJ...853..160C 2020ApJ...894...87C 2021PASP..133c4504S	High-mass star formation;Inter-Stellar Medium (ISM)/Molecular clouds	ISM and star formation	jtan	Tan, Jonathan	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00357.S	ALMA	JAO	ALMA	uid://A001/X2d8/Xb4.source.J1047-6217.spw.31	cube	2		J1047-6217	161.9289679125	-62.28739823611111	0.007220075023862902	Circle ICRS 161.928968 -62.287398 0.003610			480	1	2	0.055168674979289845	57368.203723	57373.427151	725.76	725.76	0.0013869180476687869	0.0013872938547473206	1531805.8701927634	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d8/Xb4	application/x-votable+xml; content=datalink		2015.1.00357.S	Public	289.08603142568177	-2.7890621558950017	6	9.056626333571073E-10	5.859375E7	A001:DA59 A002:DA49 A003:DV23 A004:DA41 A005:DA54 A006:DA61 A007:DV02 A009:DV18 A014:DV22 A015:DV04 A018:DA52 A020:DV03 A025:DA57 A027:DV07 A030:DA65 A033:DV20 A035:DA62 A037:DV19 A038:DA50 A039:DA63 A047:DA55 A049:DV11 A064:DV13 A098:DV10 A101:DV12 A103:DV03 A104:DA44 A114:DA53 A115:DV11 A117:DA56 A118:DV05 A119:DV06 A122:DA58 A123:DA43 A125:DA47 A126:DV25 A128:DV15 A129:DV16 A130:DV09 A131:DA51 A132:DV24 A135:DA45 P401:DA48 P403:DV21 P404:DV01 S301:DA42 W207:DA60 W208:DV14	F	2018-03-13T00:00:00.000	0.055168674979289845	[216.10..216.16GHz,141.11kHz,2mJy/beam@10km/s,689uJy/beam@native, XX YY] U [216.93..216.99GHz,141.11kHz,2mJy/beam@10km/s,689.2uJy/beam@native, XX YY] U [217.09..217.15GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [217.22..217.28GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [219.55..219.61GHz,35.28kHz,1.9mJy/beam@10km/s,681.1uJy/beam@native, XX YY] U [230.08..231.95GHz,976.56kHz,1.9mJy/beam@10km/s,122.7uJy/beam@native, XX YY] U [231.31..231.37GHz,35.28kHz,1.9mJy/beam@10km/s,693.9uJy/beam@native, XX YY]	216.1280205310071	45.72294173220015	ALMA	Gas Kinematics of the Massive Protocluster G286.21+0.17 Revealed by ALMA Offline Correction of Atmospheric Effects on Single-dish Radio Spectroscopy The Core Mass Function in the Massive Protocluster G286.21+0.17 Revealed by ALMA	Cheng, Yu Sawada, Tsuyoshi	Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Kong, Shuo; Lim, Wanggi; Andersen, Morten; Da Rio, Nicola Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Lim, Wanggi; Andersen, Morten Sawada, Tsuyoshi; Chang, Chin-Shin; Francke, Harold; Gomez, Laura; Mangum, Jeffrey G.; Miyamoto, Yusuke; Nakazato, Takeshi; Nishie, Suminori; Phillips, Neil M.; Shimajiri, Yoshito; Sugimoto, Kanako	We present a method to mitigate the atmospheric effects (residual atmospheric lines) in single-dish radio spectroscopy caused by the elevation difference between the target and reference positions. The method is developed as a script using the Atmospheric Transmission at Microwaves (ATM) library built into the Common Astronomy Software Applications (CASA) package. We apply the method to the data taken with the Total Power Array of the Atacama Large Millimeter/submillimeter Array. The intensities of the residual atmospheric (mostly O<SUB>3</SUB>) lines are suppressed by, typically, an order of magnitude for the tested cases. The parameters for the ATM model can be optimized to minimize the residual line and, for a specific O<SUB>3</SUB> line at 231.28 GHz, a seasonal dependence of a best-fitting model parameter is demonstrated. The method will be provided as a task within the CASA package in the near future. The atmospheric removal method we developed can be used by any radio/millimeter/submillimeter observato	2018	We propose to study the kinematics of gas in a massive protocluster, G286.21+0.17, that is the target of an ongoing HST study of proper motion kinematics of young stellar objects. The unique comparisons that will be possible between ALMA-derived gas kinematics and HST-derived young stellar object (YSO) kinematics will help answer fundamental questions associated with massive star cluster formation, such as: "What is the nature of spatial and kinematic substructure in gas and YSOs and how do they compare?" "What is the level of turbulent velocity dispersion of gas in comparison to stellar motions, and the implications for global support of the protocluster and thus the timescale of star cluster formation?". The ALMA observations will identify populations of dense cores in different tracers, which can be compared in terms of their spatial, kinematic and core mass function properties, to similar approved Cycle 2 observations of cores in a massive IRDC, thus probing different evolutionary stages of the massive st	G286_a_1_06_TE	Lim, Wanggi; Kong, Shuo; Liu, Mengyao; Da Rio, Nicola; Andersen, Morten;	1.9641671547326054	0.11241979345273205	0.7534055	uid://A001/X2d8/Xb3	uid://A001/X2d8/Xb4	uid://A002/Xadabcb/X1102	Kinematics of Massive Star Cluster in Formation	S	PHASE WVR	F	7.423453235210456	T	2018ApJ...853..160C 2020ApJ...894...87C 2021PASP..133c4504S	High-mass star formation;Inter-Stellar Medium (ISM)/Molecular clouds	ISM and star formation	jtan	Tan, Jonathan	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00357.S	ALMA	JAO	ALMA	uid://A001/X2d8/Xb4.source.J1047-6217.spw.35	cube	2		J1047-6217	161.9289679125	-62.28739823611111	0.007220075023862902	Circle ICRS 161.928968 -62.287398 0.003610			480	1	2	0.055168674979289845	57368.203723	57373.427151	725.76	725.76	0.0013805794810938942	0.0013809518725344458	1538838.7421650817	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d8/Xb4	application/x-votable+xml; content=datalink		2015.1.00357.S	Public	289.08603142568177	-2.7890621558950017	6	8.974022316202505E-10	5.859375E7	A001:DA59 A002:DA49 A003:DV23 A004:DA41 A005:DA54 A006:DA61 A007:DV02 A009:DV18 A014:DV22 A015:DV04 A018:DA52 A020:DV03 A025:DA57 A027:DV07 A030:DA65 A033:DV20 A035:DA62 A037:DV19 A038:DA50 A039:DA63 A047:DA55 A049:DV11 A064:DV13 A098:DV10 A101:DV12 A103:DV03 A104:DA44 A114:DA53 A115:DV11 A117:DA56 A118:DV05 A119:DV06 A122:DA58 A123:DA43 A125:DA47 A126:DV25 A128:DV15 A129:DV16 A130:DV09 A131:DA51 A132:DV24 A135:DA45 P401:DA48 P403:DV21 P404:DV01 S301:DA42 W207:DA60 W208:DV14	F	2018-03-13T00:00:00.000	0.055168674979289845	[216.10..216.16GHz,141.11kHz,2mJy/beam@10km/s,689uJy/beam@native, XX YY] U [216.93..216.99GHz,141.11kHz,2mJy/beam@10km/s,689.2uJy/beam@native, XX YY] U [217.09..217.15GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [217.22..217.28GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [219.55..219.61GHz,35.28kHz,1.9mJy/beam@10km/s,681.1uJy/beam@native, XX YY] U [230.08..231.95GHz,976.56kHz,1.9mJy/beam@10km/s,122.7uJy/beam@native, XX YY] U [231.31..231.37GHz,35.28kHz,1.9mJy/beam@10km/s,693.9uJy/beam@native, XX YY]	217.1204488101562	45.72294173220015	ALMA	Gas Kinematics of the Massive Protocluster G286.21+0.17 Revealed by ALMA Offline Correction of Atmospheric Effects on Single-dish Radio Spectroscopy The Core Mass Function in the Massive Protocluster G286.21+0.17 Revealed by ALMA	Cheng, Yu Sawada, Tsuyoshi	Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Kong, Shuo; Lim, Wanggi; Andersen, Morten; Da Rio, Nicola Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Lim, Wanggi; Andersen, Morten Sawada, Tsuyoshi; Chang, Chin-Shin; Francke, Harold; Gomez, Laura; Mangum, Jeffrey G.; Miyamoto, Yusuke; Nakazato, Takeshi; Nishie, Suminori; Phillips, Neil M.; Shimajiri, Yoshito; Sugimoto, Kanako	We present a method to mitigate the atmospheric effects (residual atmospheric lines) in single-dish radio spectroscopy caused by the elevation difference between the target and reference positions. The method is developed as a script using the Atmospheric Transmission at Microwaves (ATM) library built into the Common Astronomy Software Applications (CASA) package. We apply the method to the data taken with the Total Power Array of the Atacama Large Millimeter/submillimeter Array. The intensities of the residual atmospheric (mostly O<SUB>3</SUB>) lines are suppressed by, typically, an order of magnitude for the tested cases. The parameters for the ATM model can be optimized to minimize the residual line and, for a specific O<SUB>3</SUB> line at 231.28 GHz, a seasonal dependence of a best-fitting model parameter is demonstrated. The method will be provided as a task within the CASA package in the near future. The atmospheric removal method we developed can be used by any radio/millimeter/submillimeter observato	2018	We propose to study the kinematics of gas in a massive protocluster, G286.21+0.17, that is the target of an ongoing HST study of proper motion kinematics of young stellar objects. The unique comparisons that will be possible between ALMA-derived gas kinematics and HST-derived young stellar object (YSO) kinematics will help answer fundamental questions associated with massive star cluster formation, such as: "What is the nature of spatial and kinematic substructure in gas and YSOs and how do they compare?" "What is the level of turbulent velocity dispersion of gas in comparison to stellar motions, and the implications for global support of the protocluster and thus the timescale of star cluster formation?". The ALMA observations will identify populations of dense cores in different tracers, which can be compared in terms of their spatial, kinematic and core mass function properties, to similar approved Cycle 2 observations of cores in a massive IRDC, thus probing different evolutionary stages of the massive st	G286_a_1_06_TE	Lim, Wanggi; Kong, Shuo; Liu, Mengyao; Da Rio, Nicola; Andersen, Morten;	1.9605985508461625	0.11241979345273205	0.7534055	uid://A001/X2d8/Xb3	uid://A001/X2d8/Xb4	uid://A002/Xadabcb/X1102	Kinematics of Massive Star Cluster in Formation	S	PHASE WVR	F	7.423453235210456	T	2018ApJ...853..160C 2020ApJ...894...87C 2021PASP..133c4504S	High-mass star formation;Inter-Stellar Medium (ISM)/Molecular clouds	ISM and star formation	jtan	Tan, Jonathan	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00357.S	ALMA	JAO	ALMA	uid://A001/X2d8/Xb4.source.J1047-6217.spw.37	cube	2		J1047-6217	161.9289679125	-62.28739823611111	0.007220075023862902	Circle ICRS 161.928968 -62.287398 0.003610			480	1	2	0.055168674979289845	57368.203723	57373.427151	725.76	725.76	0.0013797309623442683	0.0013801028977306216	1539785.1089470887	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d8/Xb4	application/x-votable+xml; content=datalink		2015.1.00357.S	Public	289.08603142568177	-2.7890621558950017	6	8.962993172664764E-10	5.859375E7	A001:DA59 A002:DA49 A003:DV23 A004:DA41 A005:DA54 A006:DA61 A007:DV02 A009:DV18 A014:DV22 A015:DV04 A018:DA52 A020:DV03 A025:DA57 A027:DV07 A030:DA65 A033:DV20 A035:DA62 A037:DV19 A038:DA50 A039:DA63 A047:DA55 A049:DV11 A064:DV13 A098:DV10 A101:DV12 A103:DV03 A104:DA44 A114:DA53 A115:DV11 A117:DA56 A118:DV05 A119:DV06 A122:DA58 A123:DA43 A125:DA47 A126:DV25 A128:DV15 A129:DV16 A130:DV09 A131:DA51 A132:DV24 A135:DA45 P401:DA48 P403:DV21 P404:DV01 S301:DA42 W207:DA60 W208:DV14	F	2018-03-13T00:00:00.000	0.055168674979289845	[216.10..216.16GHz,141.11kHz,2mJy/beam@10km/s,689uJy/beam@native, XX YY] U [216.93..216.99GHz,141.11kHz,2mJy/beam@10km/s,689.2uJy/beam@native, XX YY] U [217.09..217.15GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [217.22..217.28GHz,141.11kHz,2mJy/beam@10km/s,689.3uJy/beam@native, XX YY] U [219.55..219.61GHz,35.28kHz,1.9mJy/beam@10km/s,681.1uJy/beam@native, XX YY] U [230.08..231.95GHz,976.56kHz,1.9mJy/beam@10km/s,122.7uJy/beam@native, XX YY] U [231.31..231.37GHz,35.28kHz,1.9mJy/beam@10km/s,693.9uJy/beam@native, XX YY]	217.25399327969978	45.72294173220015	ALMA	Gas Kinematics of the Massive Protocluster G286.21+0.17 Revealed by ALMA Offline Correction of Atmospheric Effects on Single-dish Radio Spectroscopy The Core Mass Function in the Massive Protocluster G286.21+0.17 Revealed by ALMA	Cheng, Yu Sawada, Tsuyoshi	Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Kong, Shuo; Lim, Wanggi; Andersen, Morten; Da Rio, Nicola Cheng, Yu; Tan, Jonathan C.; Liu, Mengyao; Lim, Wanggi; Andersen, Morten Sawada, Tsuyoshi; Chang, Chin-Shin; Francke, Harold; Gomez, Laura; Mangum, Jeffrey G.; Miyamoto, Yusuke; Nakazato, Takeshi; Nishie, Suminori; Phillips, Neil M.; Shimajiri, Yoshito; Sugimoto, Kanako	We present a method to mitigate the atmospheric effects (residual atmospheric lines) in single-dish radio spectroscopy caused by the elevation difference between the target and reference positions. The method is developed as a script using the Atmospheric Transmission at Microwaves (ATM) library built into the Common Astronomy Software Applications (CASA) package. We apply the method to the data taken with the Total Power Array of the Atacama Large Millimeter/submillimeter Array. The intensities of the residual atmospheric (mostly O<SUB>3</SUB>) lines are suppressed by, typically, an order of magnitude for the tested cases. The parameters for the ATM model can be optimized to minimize the residual line and, for a specific O<SUB>3</SUB> line at 231.28 GHz, a seasonal dependence of a best-fitting model parameter is demonstrated. The method will be provided as a task within the CASA package in the near future. The atmospheric removal method we developed can be used by any radio/millimeter/submillimeter observato	2018	We propose to study the kinematics of gas in a massive protocluster, G286.21+0.17, that is the target of an ongoing HST study of proper motion kinematics of young stellar objects. The unique comparisons that will be possible between ALMA-derived gas kinematics and HST-derived young stellar object (YSO) kinematics will help answer fundamental questions associated with massive star cluster formation, such as: "What is the nature of spatial and kinematic substructure in gas and YSOs and how do they compare?" "What is the level of turbulent velocity dispersion of gas in comparison to stellar motions, and the implications for global support of the protocluster and thus the timescale of star cluster formation?". The ALMA observations will identify populations of dense cores in different tracers, which can be compared in terms of their spatial, kinematic and core mass function properties, to similar approved Cycle 2 observations of cores in a massive IRDC, thus probing different evolutionary stages of the massive st	G286_a_1_06_TE	Lim, Wanggi; Kong, Shuo; Liu, Mengyao; Da Rio, Nicola; Andersen, Morten;	1.9601207336158963	0.11241979345273205	0.7534055	uid://A001/X2d8/Xb3	uid://A001/X2d8/Xb4	uid://A002/Xadabcb/X1102	Kinematics of Massive Star Cluster in Formation	S	PHASE WVR	F	7.423453235210456	T	2018ApJ...853..160C 2020ApJ...894...87C 2021PASP..133c4504S	High-mass star formation;Inter-Stellar Medium (ISM)/Molecular clouds	ISM and star formation	jtan	Tan, Jonathan	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2011.0.00733.S	ALMA	JAO	ALMA	uid://A002/X327408/X12b.source.Lup_25.spw.19	cube	2		Lup_25	285.370875	-37.03011111111111	0.006986056606297946	Circle ICRS 285.370875 -37.030111 0.003493			3840	1	2	0.6601318681975129	56095.290389	56095.293729	211.68	211.68	0.0012840963497605267	0.0012944893580426747	239081.14525714755	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A002/X327408/X12b	application/x-votable+xml; content=datalink		2011.0.00733.S	Public	359.826249662643	-17.80282131755851	6	5.414712924950238E-9	1.875E9	A003:DA41 A004:DV04 A011:DV12 A021:DV08 A025:DV14 A026:DA47 A045:DV11 A046:DV09 A050:DA42 A067:DA46 A068:DA44 A069:DV16 A070:DA45 A071:DV10 A072:DV13 A074:DV15 A075:DA43 A082:DV05 A137:DV03 A138:DV17	F	2013-10-22T12:19:00.000	0.6601318681975129	[229.60..231.47GHz,976.56kHz,3.3mJy/beam@10km/s,212.6uJy/beam@native, XX YY] U [231.59..233.47GHz,976.56kHz,3.4mJy/beam@10km/s,216uJy/beam@native, XX YY]	232.52849598667376	1253.936012718834	ALMA	A ring-like concentration of mm-sized particles in Sz 91 Bridging the Gap between Protoplanetary and Debris Disks: Separate Evolution of Millimeter and Micrometer-sized Dust Gas Inside the 97 AU Cavity around the Transition Disk Sz 91 New detections of Galactic molecular absorption systems toward ALMA calibrator sources Probing the final stages of protoplanetary disk evolution with ALMA	Ando, Ryo Canovas, H. Hardy, A. Michel, Arnaud	Ando, Ryo; Kohno, Kotaro; Tamura, Yoichi; Izumi, Takuma; Umehata, Hideki; Nagai, Hiroshi Canovas, H.; Caceres, C.; Schreiber, M. R.; Hardy, A.; Cieza, L.; Ménard, F.; Hales, A. Canovas, H.; Schreiber, M. R.; Cáceres, C.; Ménard, F.; Pinte, C.; Mathews, G. S.; Cieza, L.; Casassus, S.; Hales, A.; Williams, J. P.; Román, P.; Hardy, A. Hardy, A.; Caceres, C.; Schreiber, M. R.; Cieza, L.; Alexander, R. D.; Canovas, H.; Williams, J. P.; Wahhaj, Z.; Menard, F. Michel, Arnaud; van der Marel, Nienke; Matthews, Brenda C.	Context. The evolution of a circumstellar disk from its gas-rich protoplanetary stage to its gas-poor debris stage is not understood well. It is apparent that disk clearing progresses from the inside-out on a short time scale and models of photoevaporation are frequently used to explain this. However, the photoevaporation rates predicted by recent models differ by up to two orders of magnitude, resulting in uncertain time scales for the final stages of disk clearing. Aims: Photoevaporation theories predict that the final stages of disk-clearing progress in objects that have ceased accretion but still posses considerable material at radii far from the star. Weak-line T Tauri stars (WTTS) with infrared emission in excess of what is expected from the stellar photosphere are likely in this configuration. We aim to provide observational constraints on theories of disk-clearing by measuring the dust masses and CO content of a sample of young (1.8-26.3 Myr) WTTS. Methods: We used ALMA Band 6 to obtain continuum and	2015	In recent years it has been established that the evolution of circumstellar disks is fundamentally driven by the following processes: viscous accretion, grain growth, planet formation, and photoevaporation. Despite this progress, we are still far from developing a comprehensive disk evolution theory and additional observational constraints are highly required. Transition disk objects are crucial in this context as they show clear signs of disk evolution: inner opacity holes. We have performed a detailed follow-up project of Spitzer-selected transition disk systems with the aim to distinguish between different types of transition disks (Cieza et al. 2010, Romero et al. 2011). Here we propose to observe 26 transition disks characterized by Romero et al. (2011) with ALMA's unprecedented sensitivity to address fundamental issues related to grain growth, planet formation, and photoveporation in circumstellar disks. In a complementary proposal we request identical ALMA observations for 26 Ophiuchus targets (PI: Cie	Band6_contCO-2-1	Williams, Jonathan; Cieza, Lucas; Casassus, Simon; Jordan, Andres; Romero, Gisela;	3.3584779473441833	0.15151654833016642	1.3612516		uid://A002/X327408/X12b	uid://A002/X433c46/X4d2	Towards a global understanding of circumstellar disk evolution	S	TARGET	T	5.286111959131488	T	2015A&A...583A..66H 2015ApJ...805...21C 2016MNRAS.458L..29C 2016PASJ...68....6A 2021ApJ...921...72M	Disks around low-mass stars;null	Disks and planet formation	mschreiber	Schreiber, Matthias	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2011.0.00733.S	ALMA	JAO	ALMA	uid://A002/X327408/X12b.source.Lup_25.spw.17	cube	2		Lup_25	285.370875	-37.03011111111111	0.006986056606297946	Circle ICRS 285.370875 -37.030111 0.003493			3840	1	2	0.6601318681975129	56095.290389	56095.293729	211.68	211.68	0.0012951679421199845	0.0013057416797750167	237037.38792264566	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A002/X327408/X12b	application/x-votable+xml; content=datalink		2011.0.00733.S	Public	359.826249662643	-17.80282131755851	6	5.508872156301579E-9	1.875E9	A003:DA41 A004:DV04 A011:DV12 A021:DV08 A025:DV14 A026:DA47 A045:DV11 A046:DV09 A050:DA42 A067:DA46 A068:DA44 A069:DV16 A070:DA45 A071:DV10 A072:DV13 A074:DV15 A075:DA43 A082:DV05 A137:DV03 A138:DV17	F	2013-10-22T12:19:00.000	0.6601318681975129	[229.60..231.47GHz,976.56kHz,3.3mJy/beam@10km/s,212.6uJy/beam@native, XX YY] U [231.59..233.47GHz,976.56kHz,3.4mJy/beam@10km/s,216uJy/beam@native, XX YY]	230.53274159996585	1253.936012718834	ALMA	A ring-like concentration of mm-sized particles in Sz 91 Bridging the Gap between Protoplanetary and Debris Disks: Separate Evolution of Millimeter and Micrometer-sized Dust Gas Inside the 97 AU Cavity around the Transition Disk Sz 91 New detections of Galactic molecular absorption systems toward ALMA calibrator sources Probing the final stages of protoplanetary disk evolution with ALMA	Ando, Ryo Canovas, H. Hardy, A. Michel, Arnaud	Ando, Ryo; Kohno, Kotaro; Tamura, Yoichi; Izumi, Takuma; Umehata, Hideki; Nagai, Hiroshi Canovas, H.; Caceres, C.; Schreiber, M. R.; Hardy, A.; Cieza, L.; Ménard, F.; Hales, A. Canovas, H.; Schreiber, M. R.; Cáceres, C.; Ménard, F.; Pinte, C.; Mathews, G. S.; Cieza, L.; Casassus, S.; Hales, A.; Williams, J. P.; Román, P.; Hardy, A. Hardy, A.; Caceres, C.; Schreiber, M. R.; Cieza, L.; Alexander, R. D.; Canovas, H.; Williams, J. P.; Wahhaj, Z.; Menard, F. Michel, Arnaud; van der Marel, Nienke; Matthews, Brenda C.	Context. The evolution of a circumstellar disk from its gas-rich protoplanetary stage to its gas-poor debris stage is not understood well. It is apparent that disk clearing progresses from the inside-out on a short time scale and models of photoevaporation are frequently used to explain this. However, the photoevaporation rates predicted by recent models differ by up to two orders of magnitude, resulting in uncertain time scales for the final stages of disk clearing. Aims: Photoevaporation theories predict that the final stages of disk-clearing progress in objects that have ceased accretion but still posses considerable material at radii far from the star. Weak-line T Tauri stars (WTTS) with infrared emission in excess of what is expected from the stellar photosphere are likely in this configuration. We aim to provide observational constraints on theories of disk-clearing by measuring the dust masses and CO content of a sample of young (1.8-26.3 Myr) WTTS. Methods: We used ALMA Band 6 to obtain continuum and	2015	In recent years it has been established that the evolution of circumstellar disks is fundamentally driven by the following processes: viscous accretion, grain growth, planet formation, and photoevaporation. Despite this progress, we are still far from developing a comprehensive disk evolution theory and additional observational constraints are highly required. Transition disk objects are crucial in this context as they show clear signs of disk evolution: inner opacity holes. We have performed a detailed follow-up project of Spitzer-selected transition disk systems with the aim to distinguish between different types of transition disks (Cieza et al. 2010, Romero et al. 2011). Here we propose to observe 26 transition disks characterized by Romero et al. (2011) with ALMA's unprecedented sensitivity to address fundamental issues related to grain growth, planet formation, and photoveporation in circumstellar disks. In a complementary proposal we request identical ALMA observations for 26 Ophiuchus targets (PI: Cie	Band6_contCO-2-1	Williams, Jonathan; Cieza, Lucas; Casassus, Simon; Jordan, Andres; Romero, Gisela;	3.3195602471497203	0.15151654833016642	1.3612516		uid://A002/X327408/X12b	uid://A002/X433c46/X4d2	Towards a global understanding of circumstellar disk evolution	S	TARGET	T	5.286111959131488	T	2015A&A...583A..66H 2015ApJ...805...21C 2016MNRAS.458L..29C 2016PASJ...68....6A 2021ApJ...921...72M	Disks around low-mass stars;null	Disks and planet formation	mschreiber	Schreiber, Matthias	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2011.0.00733.S	ALMA	JAO	ALMA	uid://A002/X327408/X12b.source.Lup_3.spw.19	cube	2		Lup_3	240.10887500000004	-41.89877777777778	0.0069855827129175745	Circle ICRS 240.108875 -41.898778 0.003493			3840	1	2	0.7348184535056819	56095.260562	56095.263893	211.68	211.68	0.0012840092441451267	0.0012944015474261408	239081.14525714755	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A002/X327408/X12b	application/x-votable+xml; content=datalink		2011.0.00733.S	Public	336.4651811183028	8.346333217187835	6	5.413978344706984E-9	1.875E9	A003:DA41 A004:DV04 A011:DV12 A021:DV08 A025:DV14 A026:DA47 A045:DV11 A046:DV09 A050:DA42 A067:DA46 A068:DA44 A069:DV16 A070:DA45 A071:DV10 A072:DV13 A074:DV15 A075:DA43 A082:DV05 A137:DV03 A138:DV17	F	2013-10-22T12:19:00.000	0.7348184535056819	[229.61..231.49GHz,976.56kHz,3.3mJy/beam@10km/s,212.6uJy/beam@native, XX YY] U [231.61..233.48GHz,976.56kHz,3.4mJy/beam@10km/s,216uJy/beam@native, XX YY]	232.54427043520934	1253.936012718834	ALMA	A ring-like concentration of mm-sized particles in Sz 91 Bridging the Gap between Protoplanetary and Debris Disks: Separate Evolution of Millimeter and Micrometer-sized Dust Gas Inside the 97 AU Cavity around the Transition Disk Sz 91 New detections of Galactic molecular absorption systems toward ALMA calibrator sources Probing the final stages of protoplanetary disk evolution with ALMA	Ando, Ryo Canovas, H. Hardy, A. Michel, Arnaud	Ando, Ryo; Kohno, Kotaro; Tamura, Yoichi; Izumi, Takuma; Umehata, Hideki; Nagai, Hiroshi Canovas, H.; Caceres, C.; Schreiber, M. R.; Hardy, A.; Cieza, L.; Ménard, F.; Hales, A. Canovas, H.; Schreiber, M. R.; Cáceres, C.; Ménard, F.; Pinte, C.; Mathews, G. S.; Cieza, L.; Casassus, S.; Hales, A.; Williams, J. P.; Román, P.; Hardy, A. Hardy, A.; Caceres, C.; Schreiber, M. R.; Cieza, L.; Alexander, R. D.; Canovas, H.; Williams, J. P.; Wahhaj, Z.; Menard, F. Michel, Arnaud; van der Marel, Nienke; Matthews, Brenda C.	Context. The evolution of a circumstellar disk from its gas-rich protoplanetary stage to its gas-poor debris stage is not understood well. It is apparent that disk clearing progresses from the inside-out on a short time scale and models of photoevaporation are frequently used to explain this. However, the photoevaporation rates predicted by recent models differ by up to two orders of magnitude, resulting in uncertain time scales for the final stages of disk clearing. Aims: Photoevaporation theories predict that the final stages of disk-clearing progress in objects that have ceased accretion but still posses considerable material at radii far from the star. Weak-line T Tauri stars (WTTS) with infrared emission in excess of what is expected from the stellar photosphere are likely in this configuration. We aim to provide observational constraints on theories of disk-clearing by measuring the dust masses and CO content of a sample of young (1.8-26.3 Myr) WTTS. Methods: We used ALMA Band 6 to obtain continuum and	2015	In recent years it has been established that the evolution of circumstellar disks is fundamentally driven by the following processes: viscous accretion, grain growth, planet formation, and photoevaporation. Despite this progress, we are still far from developing a comprehensive disk evolution theory and additional observational constraints are highly required. Transition disk objects are crucial in this context as they show clear signs of disk evolution: inner opacity holes. We have performed a detailed follow-up project of Spitzer-selected transition disk systems with the aim to distinguish between different types of transition disks (Cieza et al. 2010, Romero et al. 2011). Here we propose to observe 26 transition disks characterized by Romero et al. (2011) with ALMA's unprecedented sensitivity to address fundamental issues related to grain growth, planet formation, and photoveporation in circumstellar disks. In a complementary proposal we request identical ALMA observations for 26 Ophiuchus targets (PI: Cie	Band6_contCO-2-1	Williams, Jonathan; Cieza, Lucas; Casassus, Simon; Jordan, Andres; Romero, Gisela;	3.35839109158377	0.1515177583933221	1.3612516		uid://A002/X327408/X12b	uid://A002/X433c46/X4d2	Towards a global understanding of circumstellar disk evolution	S	TARGET	T	6.689740556995593	T	2015A&A...583A..66H 2015ApJ...805...21C 2016MNRAS.458L..29C 2016PASJ...68....6A 2021ApJ...921...72M	Disks around low-mass stars;null	Disks and planet formation	mschreiber	Schreiber, Matthias	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2011.0.00733.S	ALMA	JAO	ALMA	uid://A002/X327408/X12b.source.Lup_3.spw.17	cube	2		Lup_3	240.10887500000004	-41.89877777777778	0.0069855827129175745	Circle ICRS 240.108875 -41.898778 0.003493			3840	1	2	0.7348184535056819	56095.260562	56095.263893	211.68	211.68	0.0012950800854722604	0.0013056531058665312	237037.38792264566	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A002/X327408/X12b	application/x-votable+xml; content=datalink		2011.0.00733.S	Public	336.4651811183028	8.346333217187835	6	5.508124802064205E-9	1.875E9	A003:DA41 A004:DV04 A011:DV12 A021:DV08 A025:DV14 A026:DA47 A045:DV11 A046:DV09 A050:DA42 A067:DA46 A068:DA44 A069:DV16 A070:DA45 A071:DV10 A072:DV13 A074:DV15 A075:DA43 A082:DV05 A137:DV03 A138:DV17	F	2013-10-22T12:19:00.000	0.7348184535056819	[229.61..231.49GHz,976.56kHz,3.3mJy/beam@10km/s,212.6uJy/beam@native, XX YY] U [231.61..233.48GHz,976.56kHz,3.4mJy/beam@10km/s,216uJy/beam@native, XX YY]	230.54838065896678	1253.936012718834	ALMA	A ring-like concentration of mm-sized particles in Sz 91 Bridging the Gap between Protoplanetary and Debris Disks: Separate Evolution of Millimeter and Micrometer-sized Dust Gas Inside the 97 AU Cavity around the Transition Disk Sz 91 New detections of Galactic molecular absorption systems toward ALMA calibrator sources Probing the final stages of protoplanetary disk evolution with ALMA	Ando, Ryo Canovas, H. Hardy, A. Michel, Arnaud	Ando, Ryo; Kohno, Kotaro; Tamura, Yoichi; Izumi, Takuma; Umehata, Hideki; Nagai, Hiroshi Canovas, H.; Caceres, C.; Schreiber, M. R.; Hardy, A.; Cieza, L.; Ménard, F.; Hales, A. Canovas, H.; Schreiber, M. R.; Cáceres, C.; Ménard, F.; Pinte, C.; Mathews, G. S.; Cieza, L.; Casassus, S.; Hales, A.; Williams, J. P.; Román, P.; Hardy, A. Hardy, A.; Caceres, C.; Schreiber, M. R.; Cieza, L.; Alexander, R. D.; Canovas, H.; Williams, J. P.; Wahhaj, Z.; Menard, F. Michel, Arnaud; van der Marel, Nienke; Matthews, Brenda C.	Context. The evolution of a circumstellar disk from its gas-rich protoplanetary stage to its gas-poor debris stage is not understood well. It is apparent that disk clearing progresses from the inside-out on a short time scale and models of photoevaporation are frequently used to explain this. However, the photoevaporation rates predicted by recent models differ by up to two orders of magnitude, resulting in uncertain time scales for the final stages of disk clearing. Aims: Photoevaporation theories predict that the final stages of disk-clearing progress in objects that have ceased accretion but still posses considerable material at radii far from the star. Weak-line T Tauri stars (WTTS) with infrared emission in excess of what is expected from the stellar photosphere are likely in this configuration. We aim to provide observational constraints on theories of disk-clearing by measuring the dust masses and CO content of a sample of young (1.8-26.3 Myr) WTTS. Methods: We used ALMA Band 6 to obtain continuum and	2015	In recent years it has been established that the evolution of circumstellar disks is fundamentally driven by the following processes: viscous accretion, grain growth, planet formation, and photoevaporation. Despite this progress, we are still far from developing a comprehensive disk evolution theory and additional observational constraints are highly required. Transition disk objects are crucial in this context as they show clear signs of disk evolution: inner opacity holes. We have performed a detailed follow-up project of Spitzer-selected transition disk systems with the aim to distinguish between different types of transition disks (Cieza et al. 2010, Romero et al. 2011). Here we propose to observe 26 transition disks characterized by Romero et al. (2011) with ALMA's unprecedented sensitivity to address fundamental issues related to grain growth, planet formation, and photoveporation in circumstellar disks. In a complementary proposal we request identical ALMA observations for 26 Ophiuchus targets (PI: Cie	Band6_contCO-2-1	Williams, Jonathan; Cieza, Lucas; Casassus, Simon; Jordan, Andres; Romero, Gisela;	3.3194739407811493	0.1515177583933221	1.3612516		uid://A002/X327408/X12b	uid://A002/X433c46/X4d2	Towards a global understanding of circumstellar disk evolution	S	TARGET	T	6.689740556995593	T	2015A&A...583A..66H 2015ApJ...805...21C 2016MNRAS.458L..29C 2016PASJ...68....6A 2021ApJ...921...72M	Disks around low-mass stars;null	Disks and planet formation	mschreiber	Schreiber, Matthias	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00994.S	ALMA	JAO	ALMA	uid://A001/X133d/X18c1.source.J2258-2758.spw.34	image	2		J2258-2758	344.5248453333596	-27.972571333337015	0.0061892363386811	Polygon ICRS 344.525717 -27.969574 344.526905 -27.970068 344.527804 -27.970913 344.528287 -27.971991 344.528342 -27.972766 344.528239 -27.973341 344.527916 -27.974062 344.527545 -27.974544 344.526533 -27.975283 344.525285 -27.975642 344.523974 -27.975569 344.522786 -27.975075 344.522291 -27.974690 344.521775 -27.974062 344.521369 -27.972959 344.521451 -27.971802 344.521675 -27.971254 344.522146 -27.970599 344.523157 -27.969860 344.524406 -27.969501			128	1	2	2.5900878825751574	58658.410094	58669.473811	4838.4	4838.4	6.766374783009535E-4	6.796874758366038E-4	14179.00072559873	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X18c1	application/x-votable+xml; content=datalink		2018.1.00994.S	Public	24.38675906740491	-64.92039910565444	8	4.793962533603205E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-01-03T00:00:00.000	2.5900878825751574	[439.67..441.66GHz,31250.00kHz,57.9mJy/beam@10km/s,5mJy/beam@native, XX YY] U [441.07..443.06GHz,31250.00kHz,69.8mJy/beam@10km/s,6mJy/beam@native, XX YY] U [441.15..443.14GHz,31250.00kHz,65.1mJy/beam@10km/s,5.6mJy/beam@native, XX YY] U [442.55..444.54GHz,31250.00kHz,125.4mJy/beam@10km/s,10.8mJy/beam@native, XX YY] U [451.46..453.45GHz,31250.00kHz,78.8mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [452.89..454.87GHz,31250.00kHz,46.4mJy/beam@10km/s,4mJy/beam@native, XX YY] U [452.92..454.91GHz,31250.00kHz,42.5mJy/beam@10km/s,3.7mJy/beam@native, XX YY] U [454.37..456.35GHz,31250.00kHz,32.7mJy/beam@10km/s,2.8mJy/beam@native, XX YY]	442.06806498487	20617.239175397364	ALMA	A sensitive APEX and ALMA CO(1-0), CO(2-1), CO(3-2), and [CI](1-0) spectral survey of 40 local (ultra-)luminous infrared galaxies An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs C I and CO in nearby spiral galaxies. I. Line ratio and abundance variations at ∼200 pc scales Discovery of a [C I]-faint, CO-bright Galaxy: ALMA Observations of the Merging Galaxy NGC 6052 The 300-pc scale ALMA view of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 1-0, and 609-μm dust continuum in a luminous infrared galaxy The first ground-based detection of the 752 GHz water line in local ultraluminous infrared galaxies using APEX-SEPIA	Liu, Daizhong Michiyama, Tomonari Montoya Arroyave, I. Quinatoa, Daysi Saito, T.	Liu, Daizhong; Schinnerer, Eva; Saito, Toshiki; Rosolowsky, Erik; Leroy, Adam; Usero, Antonio; Sandstrom, Karin; Klessen, Ralf S.; Glover, Simon C. O.; Ao, Yiping; Bešlić, Ivana; Bigiel, Frank; Cao, Yixian; Chastenet, Jérémy; Chevance, Mélanie; Dale, Daniel A.; Gao, Yu; Hughes, Annie; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Pety, Jérôme; Salak, Dragan; Santoro, Francesco; Schruba, Andreas; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. Michiyama, Tomonari; Ueda, Junko; Tadaki, Ken-ichi; Bolatto, Alberto; Molina, Juan; Saito, Toshiki; Yamashita, Takuji; Zhuang, Ming-Yang; Nakanishi, Kouichiro; Iono, Daisuke; Wang, Ran; Ho, Luis C. Montoya Arroyave, I.; Cicone, C.; Makroleivaditi, E.; Weiss, A.; Lundgren, A.; Severgnini, P.; De Breuck, C.; Baumschlager, B.; Schimek, A.;	We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(J<SUB>up</SUB> → J<SUB>up</SUB> − 1) with J<SUB>up</SUB> = 1, 2, 3) and neutral carbon [CI] <SUP>3</SUP>P<SUB>1</SUB>−<SUP>3</SUP>P<SUB>0</SUB> ([CI](1-0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1-0) (and CO(2-1)) arises from similar regions as the [CI](1-0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we	2020	We propose CI(2-1) and CO(4-3) observations towards ~40 local ultra/luminous infrared galaxies (U/LIRGs), which are forming stars violently (starburst) and are often observed as interacting galaxies. ULIRGs are the key population to connect the local and high-z Universe. While we have observed CI and high-J CO from galaxies in the early Universe, we have not yet known the information of these lines even in the well studied nearby galaxies. At first we check the consistency between CO and CI based gas mass. Second, we directly connect enormous starburst triggered by a galaxy merger and local physics around the newly born young massive stars. We use the line ratios of the CI(2-1) and CO(4-3) as diagnostics of the photodissociation region (PDR). We look for the evolutionary track along the merger sequence in gas density (n) - UV radiation strength (G0) plane for the first time. In addition, comparing with prior CI observations towards high-z sources, we verify whether the ISM of the galaxies in the early Univers	NGC_7771_b_08_7M	Tadaki, Ken-ichi; Ando, Misaki; Saito, Toshiki; Iono, Daisuke; Nakanishi, Kouichiro; Ueda, Junko;	69.84404464234143	1.6050616316277402	0.91	uid://A001/X133d/X18c0	uid://A001/X133d/X18c1	uid://A002/Xde0eb4/X1d9a	CI(1-0) and CO(4-3) survey for nearby ~40 U/LIRGs- Band8 ACA stand alone observation -	S	BANDPASS FLUX WVR	F	15.836007398542868	T	2020ApJ...897L..19M 2020MNRAS.497.3591S 2021ApJS..257...28M 2023A&A...672A..36L 2023A&A...673A..13M 2024MNRAS.527.6321Q	Merging and interacting galaxies;Surveys of galaxies	Galaxy evolution	tmichiyama	Michiyama, Tomonari	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00994.S	ALMA	JAO	ALMA	uid://A001/X133d/X18c1.source.J2258-2758.spw.16	image	2		J2258-2758	344.5248453333596	-27.972571333337015	0.0061892363386811	Polygon ICRS 344.525717 -27.969574 344.526905 -27.970068 344.527804 -27.970913 344.528287 -27.971991 344.528342 -27.972766 344.528239 -27.973341 344.527916 -27.974062 344.527545 -27.974544 344.526533 -27.975283 344.525285 -27.975642 344.523974 -27.975569 344.522786 -27.975075 344.522291 -27.974690 344.521775 -27.974062 344.521369 -27.972959 344.521451 -27.971802 344.521675 -27.971254 344.522146 -27.970599 344.523157 -27.969860 344.524406 -27.969501			128	1	2	2.5900878825751574	58658.410094	58669.473811	4838.4	4838.4	6.590215300961618E-4	6.619146507813154E-4	14494.510805928172	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X18c1	application/x-votable+xml; content=datalink		2018.1.00994.S	Public	24.38675906740491	-64.92039910565444	8	4.5470624167495845E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-01-03T00:00:00.000	2.5900878825751574	[439.67..441.66GHz,31250.00kHz,57.9mJy/beam@10km/s,5mJy/beam@native, XX YY] U [441.07..443.06GHz,31250.00kHz,69.8mJy/beam@10km/s,6mJy/beam@native, XX YY] U [441.15..443.14GHz,31250.00kHz,65.1mJy/beam@10km/s,5.6mJy/beam@native, XX YY] U [442.55..444.54GHz,31250.00kHz,125.4mJy/beam@10km/s,10.8mJy/beam@native, XX YY] U [451.46..453.45GHz,31250.00kHz,78.8mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [452.89..454.87GHz,31250.00kHz,46.4mJy/beam@10km/s,4mJy/beam@native, XX YY] U [452.92..454.91GHz,31250.00kHz,42.5mJy/beam@10km/s,3.7mJy/beam@native, XX YY] U [454.37..456.35GHz,31250.00kHz,32.7mJy/beam@10km/s,2.8mJy/beam@native, XX YY]	453.9112493855886	20617.239175397364	ALMA	A sensitive APEX and ALMA CO(1-0), CO(2-1), CO(3-2), and [CI](1-0) spectral survey of 40 local (ultra-)luminous infrared galaxies An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs C I and CO in nearby spiral galaxies. I. Line ratio and abundance variations at ∼200 pc scales Discovery of a [C I]-faint, CO-bright Galaxy: ALMA Observations of the Merging Galaxy NGC 6052 The 300-pc scale ALMA view of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 1-0, and 609-μm dust continuum in a luminous infrared galaxy The first ground-based detection of the 752 GHz water line in local ultraluminous infrared galaxies using APEX-SEPIA	Liu, Daizhong Michiyama, Tomonari Montoya Arroyave, I. Quinatoa, Daysi Saito, T.	Liu, Daizhong; Schinnerer, Eva; Saito, Toshiki; Rosolowsky, Erik; Leroy, Adam; Usero, Antonio; Sandstrom, Karin; Klessen, Ralf S.; Glover, Simon C. O.; Ao, Yiping; Bešlić, Ivana; Bigiel, Frank; Cao, Yixian; Chastenet, Jérémy; Chevance, Mélanie; Dale, Daniel A.; Gao, Yu; Hughes, Annie; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Pety, Jérôme; Salak, Dragan; Santoro, Francesco; Schruba, Andreas; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. Michiyama, Tomonari; Ueda, Junko; Tadaki, Ken-ichi; Bolatto, Alberto; Molina, Juan; Saito, Toshiki; Yamashita, Takuji; Zhuang, Ming-Yang; Nakanishi, Kouichiro; Iono, Daisuke; Wang, Ran; Ho, Luis C. Montoya Arroyave, I.; Cicone, C.; Makroleivaditi, E.; Weiss, A.; Lundgren, A.; Severgnini, P.; De Breuck, C.; Baumschlager, B.; Schimek, A.;	We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(J<SUB>up</SUB> → J<SUB>up</SUB> − 1) with J<SUB>up</SUB> = 1, 2, 3) and neutral carbon [CI] <SUP>3</SUP>P<SUB>1</SUB>−<SUP>3</SUP>P<SUB>0</SUB> ([CI](1-0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1-0) (and CO(2-1)) arises from similar regions as the [CI](1-0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we	2020	We propose CI(2-1) and CO(4-3) observations towards ~40 local ultra/luminous infrared galaxies (U/LIRGs), which are forming stars violently (starburst) and are often observed as interacting galaxies. ULIRGs are the key population to connect the local and high-z Universe. While we have observed CI and high-J CO from galaxies in the early Universe, we have not yet known the information of these lines even in the well studied nearby galaxies. At first we check the consistency between CO and CI based gas mass. Second, we directly connect enormous starburst triggered by a galaxy merger and local physics around the newly born young massive stars. We use the line ratios of the CI(2-1) and CO(4-3) as diagnostics of the photodissociation region (PDR). We look for the evolutionary track along the merger sequence in gas density (n) - UV radiation strength (G0) plane for the first time. In addition, comparing with prior CI observations towards high-z sources, we verify whether the ISM of the galaxies in the early Univers	NGC_7771_b_08_7M	Tadaki, Ken-ichi; Ando, Misaki; Saito, Toshiki; Iono, Daisuke; Nakanishi, Kouichiro; Ueda, Junko;	42.493671758583226	1.6050616316277402	0.91	uid://A001/X133d/X18c0	uid://A001/X133d/X18c1	uid://A002/Xde0eb4/X1d9a	CI(1-0) and CO(4-3) survey for nearby ~40 U/LIRGs- Band8 ACA stand alone observation -	S	BANDPASS FLUX WVR	F	15.836007398542868	T	2020ApJ...897L..19M 2020MNRAS.497.3591S 2021ApJS..257...28M 2023A&A...672A..36L 2023A&A...673A..13M 2024MNRAS.527.6321Q	Merging and interacting galaxies;Surveys of galaxies	Galaxy evolution	tmichiyama	Michiyama, Tomonari	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00994.S	ALMA	JAO	ALMA	uid://A001/X133d/X18c1.source.J2258-2758.spw.20	image	2		J2258-2758	344.5248453333596	-27.972571333337015	0.0061892363386811	Polygon ICRS 344.525717 -27.969574 344.526905 -27.970068 344.527804 -27.970913 344.528287 -27.971991 344.528342 -27.972766 344.528239 -27.973341 344.527916 -27.974062 344.527545 -27.974544 344.526533 -27.975283 344.525285 -27.975642 344.523974 -27.975569 344.522786 -27.975075 344.522291 -27.974690 344.521775 -27.974062 344.521369 -27.972959 344.521451 -27.971802 344.521675 -27.971254 344.522146 -27.970599 344.523157 -27.969860 344.524406 -27.969501			128	1	2	2.5900878825751574	58658.410094	58669.473811	4838.4	4838.4	6.765251112214949E-4	6.795741355384594E-4	14181.354927998484	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X18c1	application/x-votable+xml; content=datalink		2018.1.00994.S	Public	24.38675906740491	-64.92039910565444	8	4.792367137664196E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-01-03T00:00:00.000	2.5900878825751574	[439.67..441.66GHz,31250.00kHz,57.9mJy/beam@10km/s,5mJy/beam@native, XX YY] U [441.07..443.06GHz,31250.00kHz,69.8mJy/beam@10km/s,6mJy/beam@native, XX YY] U [441.15..443.14GHz,31250.00kHz,65.1mJy/beam@10km/s,5.6mJy/beam@native, XX YY] U [442.55..444.54GHz,31250.00kHz,125.4mJy/beam@10km/s,10.8mJy/beam@native, XX YY] U [451.46..453.45GHz,31250.00kHz,78.8mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [452.89..454.87GHz,31250.00kHz,46.4mJy/beam@10km/s,4mJy/beam@native, XX YY] U [452.92..454.91GHz,31250.00kHz,42.5mJy/beam@10km/s,3.7mJy/beam@native, XX YY] U [454.37..456.35GHz,31250.00kHz,32.7mJy/beam@10km/s,2.8mJy/beam@native, XX YY]	442.14164153024075	20617.239175397364	ALMA	A sensitive APEX and ALMA CO(1-0), CO(2-1), CO(3-2), and [CI](1-0) spectral survey of 40 local (ultra-)luminous infrared galaxies An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs C I and CO in nearby spiral galaxies. I. Line ratio and abundance variations at ∼200 pc scales Discovery of a [C I]-faint, CO-bright Galaxy: ALMA Observations of the Merging Galaxy NGC 6052 The 300-pc scale ALMA view of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 1-0, and 609-μm dust continuum in a luminous infrared galaxy The first ground-based detection of the 752 GHz water line in local ultraluminous infrared galaxies using APEX-SEPIA	Liu, Daizhong Michiyama, Tomonari Montoya Arroyave, I. Quinatoa, Daysi Saito, T.	Liu, Daizhong; Schinnerer, Eva; Saito, Toshiki; Rosolowsky, Erik; Leroy, Adam; Usero, Antonio; Sandstrom, Karin; Klessen, Ralf S.; Glover, Simon C. O.; Ao, Yiping; Bešlić, Ivana; Bigiel, Frank; Cao, Yixian; Chastenet, Jérémy; Chevance, Mélanie; Dale, Daniel A.; Gao, Yu; Hughes, Annie; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Pety, Jérôme; Salak, Dragan; Santoro, Francesco; Schruba, Andreas; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. Michiyama, Tomonari; Ueda, Junko; Tadaki, Ken-ichi; Bolatto, Alberto; Molina, Juan; Saito, Toshiki; Yamashita, Takuji; Zhuang, Ming-Yang; Nakanishi, Kouichiro; Iono, Daisuke; Wang, Ran; Ho, Luis C. Montoya Arroyave, I.; Cicone, C.; Makroleivaditi, E.; Weiss, A.; Lundgren, A.; Severgnini, P.; De Breuck, C.; Baumschlager, B.; Schimek, A.;	We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(J<SUB>up</SUB> → J<SUB>up</SUB> − 1) with J<SUB>up</SUB> = 1, 2, 3) and neutral carbon [CI] <SUP>3</SUP>P<SUB>1</SUB>−<SUP>3</SUP>P<SUB>0</SUB> ([CI](1-0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1-0) (and CO(2-1)) arises from similar regions as the [CI](1-0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we	2020	We propose CI(2-1) and CO(4-3) observations towards ~40 local ultra/luminous infrared galaxies (U/LIRGs), which are forming stars violently (starburst) and are often observed as interacting galaxies. ULIRGs are the key population to connect the local and high-z Universe. While we have observed CI and high-J CO from galaxies in the early Universe, we have not yet known the information of these lines even in the well studied nearby galaxies. At first we check the consistency between CO and CI based gas mass. Second, we directly connect enormous starburst triggered by a galaxy merger and local physics around the newly born young massive stars. We use the line ratios of the CI(2-1) and CO(4-3) as diagnostics of the photodissociation region (PDR). We look for the evolutionary track along the merger sequence in gas density (n) - UV radiation strength (G0) plane for the first time. In addition, comparing with prior CI observations towards high-z sources, we verify whether the ISM of the galaxies in the early Univers	NGC_7771_b_08_7M	Tadaki, Ken-ichi; Ando, Misaki; Saito, Toshiki; Iono, Daisuke; Nakanishi, Kouichiro; Ueda, Junko;	65.14173965127493	1.6050616316277402	0.91	uid://A001/X133d/X18c0	uid://A001/X133d/X18c1	uid://A002/Xde0eb4/X1d9a	CI(1-0) and CO(4-3) survey for nearby ~40 U/LIRGs- Band8 ACA stand alone observation -	S	BANDPASS FLUX WVR	F	15.836007398542868	T	2020ApJ...897L..19M 2020MNRAS.497.3591S 2021ApJS..257...28M 2023A&A...672A..36L 2023A&A...673A..13M 2024MNRAS.527.6321Q	Merging and interacting galaxies;Surveys of galaxies	Galaxy evolution	tmichiyama	Michiyama, Tomonari	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00994.S	ALMA	JAO	ALMA	uid://A001/X133d/X18c1.source.J2258-2758.spw.30	image	2		J2258-2758	344.5248453333596	-27.972571333337015	0.0061892363386811	Polygon ICRS 344.525717 -27.969574 344.526905 -27.970068 344.527804 -27.970913 344.528287 -27.971991 344.528342 -27.972766 344.528239 -27.973341 344.527916 -27.974062 344.527545 -27.974544 344.526533 -27.975283 344.525285 -27.975642 344.523974 -27.975569 344.522786 -27.975075 344.522291 -27.974690 344.521775 -27.974062 344.521369 -27.972959 344.521451 -27.971802 344.521675 -27.971254 344.522146 -27.970599 344.523157 -27.969860 344.524406 -27.969501			128	1	2	2.5900878825751574	58658.410094	58669.473811	4838.4	4838.4	6.59066884278582E-4	6.619603578267828E-4	14493.509988799773	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X18c1	application/x-votable+xml; content=datalink		2018.1.00994.S	Public	24.38675906740491	-64.92039910565444	8	4.547689356698571E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-01-03T00:00:00.000	2.5900878825751574	[439.67..441.66GHz,31250.00kHz,57.9mJy/beam@10km/s,5mJy/beam@native, XX YY] U [441.07..443.06GHz,31250.00kHz,69.8mJy/beam@10km/s,6mJy/beam@native, XX YY] U [441.15..443.14GHz,31250.00kHz,65.1mJy/beam@10km/s,5.6mJy/beam@native, XX YY] U [442.55..444.54GHz,31250.00kHz,125.4mJy/beam@10km/s,10.8mJy/beam@native, XX YY] U [451.46..453.45GHz,31250.00kHz,78.8mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [452.89..454.87GHz,31250.00kHz,46.4mJy/beam@10km/s,4mJy/beam@native, XX YY] U [452.92..454.91GHz,31250.00kHz,42.5mJy/beam@10km/s,3.7mJy/beam@native, XX YY] U [454.37..456.35GHz,31250.00kHz,32.7mJy/beam@10km/s,2.8mJy/beam@native, XX YY]	453.8799605450811	20617.239175397364	ALMA	A sensitive APEX and ALMA CO(1-0), CO(2-1), CO(3-2), and [CI](1-0) spectral survey of 40 local (ultra-)luminous infrared galaxies An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs C I and CO in nearby spiral galaxies. I. Line ratio and abundance variations at ∼200 pc scales Discovery of a [C I]-faint, CO-bright Galaxy: ALMA Observations of the Merging Galaxy NGC 6052 The 300-pc scale ALMA view of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 1-0, and 609-μm dust continuum in a luminous infrared galaxy The first ground-based detection of the 752 GHz water line in local ultraluminous infrared galaxies using APEX-SEPIA	Liu, Daizhong Michiyama, Tomonari Montoya Arroyave, I. Quinatoa, Daysi Saito, T.	Liu, Daizhong; Schinnerer, Eva; Saito, Toshiki; Rosolowsky, Erik; Leroy, Adam; Usero, Antonio; Sandstrom, Karin; Klessen, Ralf S.; Glover, Simon C. O.; Ao, Yiping; Bešlić, Ivana; Bigiel, Frank; Cao, Yixian; Chastenet, Jérémy; Chevance, Mélanie; Dale, Daniel A.; Gao, Yu; Hughes, Annie; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Pety, Jérôme; Salak, Dragan; Santoro, Francesco; Schruba, Andreas; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. Michiyama, Tomonari; Ueda, Junko; Tadaki, Ken-ichi; Bolatto, Alberto; Molina, Juan; Saito, Toshiki; Yamashita, Takuji; Zhuang, Ming-Yang; Nakanishi, Kouichiro; Iono, Daisuke; Wang, Ran; Ho, Luis C. Montoya Arroyave, I.; Cicone, C.; Makroleivaditi, E.; Weiss, A.; Lundgren, A.; Severgnini, P.; De Breuck, C.; Baumschlager, B.; Schimek, A.;	We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(J<SUB>up</SUB> → J<SUB>up</SUB> − 1) with J<SUB>up</SUB> = 1, 2, 3) and neutral carbon [CI] <SUP>3</SUP>P<SUB>1</SUB>−<SUP>3</SUP>P<SUB>0</SUB> ([CI](1-0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1-0) (and CO(2-1)) arises from similar regions as the [CI](1-0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we	2020	We propose CI(2-1) and CO(4-3) observations towards ~40 local ultra/luminous infrared galaxies (U/LIRGs), which are forming stars violently (starburst) and are often observed as interacting galaxies. ULIRGs are the key population to connect the local and high-z Universe. While we have observed CI and high-J CO from galaxies in the early Universe, we have not yet known the information of these lines even in the well studied nearby galaxies. At first we check the consistency between CO and CI based gas mass. Second, we directly connect enormous starburst triggered by a galaxy merger and local physics around the newly born young massive stars. We use the line ratios of the CI(2-1) and CO(4-3) as diagnostics of the photodissociation region (PDR). We look for the evolutionary track along the merger sequence in gas density (n) - UV radiation strength (G0) plane for the first time. In addition, comparing with prior CI observations towards high-z sources, we verify whether the ISM of the galaxies in the early Univers	NGC_7771_b_08_7M	Tadaki, Ken-ichi; Ando, Misaki; Saito, Toshiki; Iono, Daisuke; Nakanishi, Kouichiro; Ueda, Junko;	46.37334454468555	1.6050616316277402	0.91	uid://A001/X133d/X18c0	uid://A001/X133d/X18c1	uid://A002/Xde0eb4/X1d9a	CI(1-0) and CO(4-3) survey for nearby ~40 U/LIRGs- Band8 ACA stand alone observation -	S	BANDPASS FLUX WVR	F	15.836007398542868	T	2020ApJ...897L..19M 2020MNRAS.497.3591S 2021ApJS..257...28M 2023A&A...672A..36L 2023A&A...673A..13M 2024MNRAS.527.6321Q	Merging and interacting galaxies;Surveys of galaxies	Galaxy evolution	tmichiyama	Michiyama, Tomonari	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00994.S	ALMA	JAO	ALMA	uid://A001/X133d/X18c1.source.J2258-2758.spw.32	image	2		J2258-2758	344.5248453333596	-27.972571333337015	0.0061892363386811	Polygon ICRS 344.525717 -27.969574 344.526905 -27.970068 344.527804 -27.970913 344.528287 -27.971991 344.528342 -27.972766 344.528239 -27.973341 344.527916 -27.974062 344.527545 -27.974544 344.526533 -27.975283 344.525285 -27.975642 344.523974 -27.975569 344.522786 -27.975075 344.522291 -27.974690 344.521775 -27.974062 344.521369 -27.972959 344.521451 -27.971802 344.521675 -27.971254 344.522146 -27.970599 344.523157 -27.969860 344.524406 -27.969501			128	1	2	2.5900878825751574	58658.410094	58669.473811	4838.4	4838.4	6.743852501751676E-4	6.774149463975903E-4	14226.354110870087	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X18c1	application/x-votable+xml; content=datalink		2018.1.00994.S	Public	24.38675906740491	-64.92039910565444	8	4.7620303220188146E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-01-03T00:00:00.000	2.5900878825751574	[439.67..441.66GHz,31250.00kHz,57.9mJy/beam@10km/s,5mJy/beam@native, XX YY] U [441.07..443.06GHz,31250.00kHz,69.8mJy/beam@10km/s,6mJy/beam@native, XX YY] U [441.15..443.14GHz,31250.00kHz,65.1mJy/beam@10km/s,5.6mJy/beam@native, XX YY] U [442.55..444.54GHz,31250.00kHz,125.4mJy/beam@10km/s,10.8mJy/beam@native, XX YY] U [451.46..453.45GHz,31250.00kHz,78.8mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [452.89..454.87GHz,31250.00kHz,46.4mJy/beam@10km/s,4mJy/beam@native, XX YY] U [452.92..454.91GHz,31250.00kHz,42.5mJy/beam@10km/s,3.7mJy/beam@native, XX YY] U [454.37..456.35GHz,31250.00kHz,32.7mJy/beam@10km/s,2.8mJy/beam@native, XX YY]	443.5477442003127	20617.239175397364	ALMA	A sensitive APEX and ALMA CO(1-0), CO(2-1), CO(3-2), and [CI](1-0) spectral survey of 40 local (ultra-)luminous infrared galaxies An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs C I and CO in nearby spiral galaxies. I. Line ratio and abundance variations at ∼200 pc scales Discovery of a [C I]-faint, CO-bright Galaxy: ALMA Observations of the Merging Galaxy NGC 6052 The 300-pc scale ALMA view of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 1-0, and 609-μm dust continuum in a luminous infrared galaxy The first ground-based detection of the 752 GHz water line in local ultraluminous infrared galaxies using APEX-SEPIA	Liu, Daizhong Michiyama, Tomonari Montoya Arroyave, I. Quinatoa, Daysi Saito, T.	Liu, Daizhong; Schinnerer, Eva; Saito, Toshiki; Rosolowsky, Erik; Leroy, Adam; Usero, Antonio; Sandstrom, Karin; Klessen, Ralf S.; Glover, Simon C. O.; Ao, Yiping; Bešlić, Ivana; Bigiel, Frank; Cao, Yixian; Chastenet, Jérémy; Chevance, Mélanie; Dale, Daniel A.; Gao, Yu; Hughes, Annie; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Pety, Jérôme; Salak, Dragan; Santoro, Francesco; Schruba, Andreas; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. Michiyama, Tomonari; Ueda, Junko; Tadaki, Ken-ichi; Bolatto, Alberto; Molina, Juan; Saito, Toshiki; Yamashita, Takuji; Zhuang, Ming-Yang; Nakanishi, Kouichiro; Iono, Daisuke; Wang, Ran; Ho, Luis C. Montoya Arroyave, I.; Cicone, C.; Makroleivaditi, E.; Weiss, A.; Lundgren, A.; Severgnini, P.; De Breuck, C.; Baumschlager, B.; Schimek, A.;	We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(J<SUB>up</SUB> → J<SUB>up</SUB> − 1) with J<SUB>up</SUB> = 1, 2, 3) and neutral carbon [CI] <SUP>3</SUP>P<SUB>1</SUB>−<SUP>3</SUP>P<SUB>0</SUB> ([CI](1-0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1-0) (and CO(2-1)) arises from similar regions as the [CI](1-0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we	2020	We propose CI(2-1) and CO(4-3) observations towards ~40 local ultra/luminous infrared galaxies (U/LIRGs), which are forming stars violently (starburst) and are often observed as interacting galaxies. ULIRGs are the key population to connect the local and high-z Universe. While we have observed CI and high-J CO from galaxies in the early Universe, we have not yet known the information of these lines even in the well studied nearby galaxies. At first we check the consistency between CO and CI based gas mass. Second, we directly connect enormous starburst triggered by a galaxy merger and local physics around the newly born young massive stars. We use the line ratios of the CI(2-1) and CO(4-3) as diagnostics of the photodissociation region (PDR). We look for the evolutionary track along the merger sequence in gas density (n) - UV radiation strength (G0) plane for the first time. In addition, comparing with prior CI observations towards high-z sources, we verify whether the ISM of the galaxies in the early Univers	NGC_7771_b_08_7M	Tadaki, Ken-ichi; Ando, Misaki; Saito, Toshiki; Iono, Daisuke; Nakanishi, Kouichiro; Ueda, Junko;	125.39711601357558	1.6050616316277402	0.91	uid://A001/X133d/X18c0	uid://A001/X133d/X18c1	uid://A002/Xde0eb4/X1d9a	CI(1-0) and CO(4-3) survey for nearby ~40 U/LIRGs- Band8 ACA stand alone observation -	S	BANDPASS FLUX WVR	F	15.836007398542868	T	2020ApJ...897L..19M 2020MNRAS.497.3591S 2021ApJS..257...28M 2023A&A...672A..36L 2023A&A...673A..13M 2024MNRAS.527.6321Q	Merging and interacting galaxies;Surveys of galaxies	Galaxy evolution	tmichiyama	Michiyama, Tomonari	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00994.S	ALMA	JAO	ALMA	uid://A001/X133d/X18c1.source.J2258-2758.spw.18	image	2		J2258-2758	344.5248453333596	-27.972571333337015	0.0061892363386811	Polygon ICRS 344.525717 -27.969574 344.526905 -27.970068 344.527804 -27.970913 344.528287 -27.971991 344.528342 -27.972766 344.528239 -27.973341 344.527916 -27.974062 344.527545 -27.974544 344.526533 -27.975283 344.525285 -27.975642 344.523974 -27.975569 344.522786 -27.975075 344.522291 -27.974690 344.521775 -27.974062 344.521369 -27.972959 344.521451 -27.971802 344.521675 -27.971254 344.522146 -27.970599 344.523157 -27.969860 344.524406 -27.969501			128	1	2	2.5900878825751574	58658.410094	58669.473811	4838.4	4838.4	6.611403762484424E-4	6.640521508020231E-4	14447.854805928171	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X18c1	application/x-votable+xml; content=datalink		2018.1.00994.S	Public	24.38675906740491	-64.92039910565444	8	4.576412751495038E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-01-03T00:00:00.000	2.5900878825751574	[439.67..441.66GHz,31250.00kHz,57.9mJy/beam@10km/s,5mJy/beam@native, XX YY] U [441.07..443.06GHz,31250.00kHz,69.8mJy/beam@10km/s,6mJy/beam@native, XX YY] U [441.15..443.14GHz,31250.00kHz,65.1mJy/beam@10km/s,5.6mJy/beam@native, XX YY] U [442.55..444.54GHz,31250.00kHz,125.4mJy/beam@10km/s,10.8mJy/beam@native, XX YY] U [451.46..453.45GHz,31250.00kHz,78.8mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [452.89..454.87GHz,31250.00kHz,46.4mJy/beam@10km/s,4mJy/beam@native, XX YY] U [452.92..454.91GHz,31250.00kHz,42.5mJy/beam@10km/s,3.7mJy/beam@native, XX YY] U [454.37..456.35GHz,31250.00kHz,32.7mJy/beam@10km/s,2.8mJy/beam@native, XX YY]	452.4533594221625	20617.239175397364	ALMA	A sensitive APEX and ALMA CO(1-0), CO(2-1), CO(3-2), and [CI](1-0) spectral survey of 40 local (ultra-)luminous infrared galaxies An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs C I and CO in nearby spiral galaxies. I. Line ratio and abundance variations at ∼200 pc scales Discovery of a [C I]-faint, CO-bright Galaxy: ALMA Observations of the Merging Galaxy NGC 6052 The 300-pc scale ALMA view of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 1-0, and 609-μm dust continuum in a luminous infrared galaxy The first ground-based detection of the 752 GHz water line in local ultraluminous infrared galaxies using APEX-SEPIA	Liu, Daizhong Michiyama, Tomonari Montoya Arroyave, I. Quinatoa, Daysi Saito, T.	Liu, Daizhong; Schinnerer, Eva; Saito, Toshiki; Rosolowsky, Erik; Leroy, Adam; Usero, Antonio; Sandstrom, Karin; Klessen, Ralf S.; Glover, Simon C. O.; Ao, Yiping; Bešlić, Ivana; Bigiel, Frank; Cao, Yixian; Chastenet, Jérémy; Chevance, Mélanie; Dale, Daniel A.; Gao, Yu; Hughes, Annie; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Pety, Jérôme; Salak, Dragan; Santoro, Francesco; Schruba, Andreas; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. Michiyama, Tomonari; Ueda, Junko; Tadaki, Ken-ichi; Bolatto, Alberto; Molina, Juan; Saito, Toshiki; Yamashita, Takuji; Zhuang, Ming-Yang; Nakanishi, Kouichiro; Iono, Daisuke; Wang, Ran; Ho, Luis C. Montoya Arroyave, I.; Cicone, C.; Makroleivaditi, E.; Weiss, A.; Lundgren, A.; Severgnini, P.; De Breuck, C.; Baumschlager, B.; Schimek, A.;	We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(J<SUB>up</SUB> → J<SUB>up</SUB> − 1) with J<SUB>up</SUB> = 1, 2, 3) and neutral carbon [CI] <SUP>3</SUP>P<SUB>1</SUB>−<SUP>3</SUP>P<SUB>0</SUB> ([CI](1-0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1-0) (and CO(2-1)) arises from similar regions as the [CI](1-0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we	2020	We propose CI(2-1) and CO(4-3) observations towards ~40 local ultra/luminous infrared galaxies (U/LIRGs), which are forming stars violently (starburst) and are often observed as interacting galaxies. ULIRGs are the key population to connect the local and high-z Universe. While we have observed CI and high-J CO from galaxies in the early Universe, we have not yet known the information of these lines even in the well studied nearby galaxies. At first we check the consistency between CO and CI based gas mass. Second, we directly connect enormous starburst triggered by a galaxy merger and local physics around the newly born young massive stars. We use the line ratios of the CI(2-1) and CO(4-3) as diagnostics of the photodissociation region (PDR). We look for the evolutionary track along the merger sequence in gas density (n) - UV radiation strength (G0) plane for the first time. In addition, comparing with prior CI observations towards high-z sources, we verify whether the ISM of the galaxies in the early Univers	NGC_7771_b_08_7M	Tadaki, Ken-ichi; Ando, Misaki; Saito, Toshiki; Iono, Daisuke; Nakanishi, Kouichiro; Ueda, Junko;	78.76481055186969	1.6050616316277402	0.91	uid://A001/X133d/X18c0	uid://A001/X133d/X18c1	uid://A002/Xde0eb4/X1d9a	CI(1-0) and CO(4-3) survey for nearby ~40 U/LIRGs- Band8 ACA stand alone observation -	S	BANDPASS FLUX WVR	F	15.836007398542868	T	2020ApJ...897L..19M 2020MNRAS.497.3591S 2021ApJS..257...28M 2023A&A...672A..36L 2023A&A...673A..13M 2024MNRAS.527.6321Q	Merging and interacting galaxies;Surveys of galaxies	Galaxy evolution	tmichiyama	Michiyama, Tomonari	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00994.S	ALMA	JAO	ALMA	uid://A001/X133d/X18c1.source.J2258-2758.spw.22	image	2		J2258-2758	344.5248453333596	-27.972571333337015	0.0061892363386811	Polygon ICRS 344.525717 -27.969574 344.526905 -27.970068 344.527804 -27.970913 344.528287 -27.971991 344.528342 -27.972766 344.528239 -27.973341 344.527916 -27.974062 344.527545 -27.974544 344.526533 -27.975283 344.525285 -27.975642 344.523974 -27.975569 344.522786 -27.975075 344.522291 -27.974690 344.521775 -27.974062 344.521369 -27.972959 344.521451 -27.971802 344.521675 -27.971254 344.522146 -27.970599 344.523157 -27.969860 344.524406 -27.969501			128	1	2	2.5900878825751574	58658.410094	58669.473811	4838.4	4838.4	6.78791235550317E-4	6.81860744606003E-4	14134.010927998484	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X18c1	application/x-votable+xml; content=datalink		2018.1.00994.S	Public	24.38675906740491	-64.92039910565444	8	4.824599120089104E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-01-03T00:00:00.000	2.5900878825751574	[439.67..441.66GHz,31250.00kHz,57.9mJy/beam@10km/s,5mJy/beam@native, XX YY] U [441.07..443.06GHz,31250.00kHz,69.8mJy/beam@10km/s,6mJy/beam@native, XX YY] U [441.15..443.14GHz,31250.00kHz,65.1mJy/beam@10km/s,5.6mJy/beam@native, XX YY] U [442.55..444.54GHz,31250.00kHz,125.4mJy/beam@10km/s,10.8mJy/beam@native, XX YY] U [451.46..453.45GHz,31250.00kHz,78.8mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [452.89..454.87GHz,31250.00kHz,46.4mJy/beam@10km/s,4mJy/beam@native, XX YY] U [452.92..454.91GHz,31250.00kHz,42.5mJy/beam@10km/s,3.7mJy/beam@native, XX YY] U [454.37..456.35GHz,31250.00kHz,32.7mJy/beam@10km/s,2.8mJy/beam@native, XX YY]	440.66225318943907	20617.239175397364	ALMA	A sensitive APEX and ALMA CO(1-0), CO(2-1), CO(3-2), and [CI](1-0) spectral survey of 40 local (ultra-)luminous infrared galaxies An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs C I and CO in nearby spiral galaxies. I. Line ratio and abundance variations at ∼200 pc scales Discovery of a [C I]-faint, CO-bright Galaxy: ALMA Observations of the Merging Galaxy NGC 6052 The 300-pc scale ALMA view of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 1-0, and 609-μm dust continuum in a luminous infrared galaxy The first ground-based detection of the 752 GHz water line in local ultraluminous infrared galaxies using APEX-SEPIA	Liu, Daizhong Michiyama, Tomonari Montoya Arroyave, I. Quinatoa, Daysi Saito, T.	Liu, Daizhong; Schinnerer, Eva; Saito, Toshiki; Rosolowsky, Erik; Leroy, Adam; Usero, Antonio; Sandstrom, Karin; Klessen, Ralf S.; Glover, Simon C. O.; Ao, Yiping; Bešlić, Ivana; Bigiel, Frank; Cao, Yixian; Chastenet, Jérémy; Chevance, Mélanie; Dale, Daniel A.; Gao, Yu; Hughes, Annie; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Pety, Jérôme; Salak, Dragan; Santoro, Francesco; Schruba, Andreas; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. Michiyama, Tomonari; Ueda, Junko; Tadaki, Ken-ichi; Bolatto, Alberto; Molina, Juan; Saito, Toshiki; Yamashita, Takuji; Zhuang, Ming-Yang; Nakanishi, Kouichiro; Iono, Daisuke; Wang, Ran; Ho, Luis C. Montoya Arroyave, I.; Cicone, C.; Makroleivaditi, E.; Weiss, A.; Lundgren, A.; Severgnini, P.; De Breuck, C.; Baumschlager, B.; Schimek, A.;	We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(J<SUB>up</SUB> → J<SUB>up</SUB> − 1) with J<SUB>up</SUB> = 1, 2, 3) and neutral carbon [CI] <SUP>3</SUP>P<SUB>1</SUB>−<SUP>3</SUP>P<SUB>0</SUB> ([CI](1-0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1-0) (and CO(2-1)) arises from similar regions as the [CI](1-0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we	2020	We propose CI(2-1) and CO(4-3) observations towards ~40 local ultra/luminous infrared galaxies (U/LIRGs), which are forming stars violently (starburst) and are often observed as interacting galaxies. ULIRGs are the key population to connect the local and high-z Universe. While we have observed CI and high-J CO from galaxies in the early Universe, we have not yet known the information of these lines even in the well studied nearby galaxies. At first we check the consistency between CO and CI based gas mass. Second, we directly connect enormous starburst triggered by a galaxy merger and local physics around the newly born young massive stars. We use the line ratios of the CI(2-1) and CO(4-3) as diagnostics of the photodissociation region (PDR). We look for the evolutionary track along the merger sequence in gas density (n) - UV radiation strength (G0) plane for the first time. In addition, comparing with prior CI observations towards high-z sources, we verify whether the ISM of the galaxies in the early Univers	NGC_7771_b_08_7M	Tadaki, Ken-ichi; Ando, Misaki; Saito, Toshiki; Iono, Daisuke; Nakanishi, Kouichiro; Ueda, Junko;	57.93385448317043	1.6050616316277402	0.91	uid://A001/X133d/X18c0	uid://A001/X133d/X18c1	uid://A002/Xde0eb4/X1d9a	CI(1-0) and CO(4-3) survey for nearby ~40 U/LIRGs- Band8 ACA stand alone observation -	S	BANDPASS FLUX WVR	F	15.836007398542868	T	2020ApJ...897L..19M 2020MNRAS.497.3591S 2021ApJS..257...28M 2023A&A...672A..36L 2023A&A...673A..13M 2024MNRAS.527.6321Q	Merging and interacting galaxies;Surveys of galaxies	Galaxy evolution	tmichiyama	Michiyama, Tomonari	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00994.S	ALMA	JAO	ALMA	uid://A001/X133d/X18c1.source.J2258-2758.spw.28	image	2		J2258-2758	344.5248453333596	-27.972571333337015	0.0061892363386811	Polygon ICRS 344.525717 -27.969574 344.526905 -27.970068 344.527804 -27.970913 344.528287 -27.971991 344.528342 -27.972766 344.528239 -27.973341 344.527916 -27.974062 344.527545 -27.974544 344.526533 -27.975283 344.525285 -27.975642 344.523974 -27.975569 344.522786 -27.975075 344.522291 -27.974690 344.521775 -27.974062 344.521369 -27.972959 344.521451 -27.971802 344.521675 -27.971254 344.522146 -27.970599 344.523157 -27.969860 344.524406 -27.969501			128	1	2	2.5900878825751574	58658.410094	58669.473811	4838.4	4838.4	6.569299222779284E-4	6.59804635497775E-4	14540.86337407113	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133d/X18c1	application/x-votable+xml; content=datalink		2018.1.00994.S	Public	24.38675906740491	-64.92039910565444	8	4.5181820409172265E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-01-03T00:00:00.000	2.5900878825751574	[439.67..441.66GHz,31250.00kHz,57.9mJy/beam@10km/s,5mJy/beam@native, XX YY] U [441.07..443.06GHz,31250.00kHz,69.8mJy/beam@10km/s,6mJy/beam@native, XX YY] U [441.15..443.14GHz,31250.00kHz,65.1mJy/beam@10km/s,5.6mJy/beam@native, XX YY] U [442.55..444.54GHz,31250.00kHz,125.4mJy/beam@10km/s,10.8mJy/beam@native, XX YY] U [451.46..453.45GHz,31250.00kHz,78.8mJy/beam@10km/s,6.8mJy/beam@native, XX YY] U [452.89..454.87GHz,31250.00kHz,46.4mJy/beam@10km/s,4mJy/beam@native, XX YY] U [452.92..454.91GHz,31250.00kHz,42.5mJy/beam@10km/s,3.7mJy/beam@native, XX YY] U [454.37..456.35GHz,31250.00kHz,32.7mJy/beam@10km/s,2.8mJy/beam@native, XX YY]	455.3596397605238	20617.239175397364	ALMA	A sensitive APEX and ALMA CO(1-0), CO(2-1), CO(3-2), and [CI](1-0) spectral survey of 40 local (ultra-)luminous infrared galaxies An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs C I and CO in nearby spiral galaxies. I. Line ratio and abundance variations at ∼200 pc scales Discovery of a [C I]-faint, CO-bright Galaxy: ALMA Observations of the Merging Galaxy NGC 6052 The 300-pc scale ALMA view of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 1-0, and 609-μm dust continuum in a luminous infrared galaxy The first ground-based detection of the 752 GHz water line in local ultraluminous infrared galaxies using APEX-SEPIA	Liu, Daizhong Michiyama, Tomonari Montoya Arroyave, I. Quinatoa, Daysi Saito, T.	Liu, Daizhong; Schinnerer, Eva; Saito, Toshiki; Rosolowsky, Erik; Leroy, Adam; Usero, Antonio; Sandstrom, Karin; Klessen, Ralf S.; Glover, Simon C. O.; Ao, Yiping; Bešlić, Ivana; Bigiel, Frank; Cao, Yixian; Chastenet, Jérémy; Chevance, Mélanie; Dale, Daniel A.; Gao, Yu; Hughes, Annie; Kreckel, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Pety, Jérôme; Salak, Dragan; Santoro, Francesco; Schruba, Andreas; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas Michiyama, Tomonari; Saito, Toshiki; Tadaki, Ken-ichi; Ueda, Junko; Zhuang, Ming-Yang; Molina, Juan; Lee, Bumhyun; Wang, Ran; Bolatto, Alberto D.; Iono, Daisuke; Nakanishi, Kouichiro; Izumi, Takuma; Yamashita, Takuji; Ho, Luis C. Michiyama, Tomonari; Ueda, Junko; Tadaki, Ken-ichi; Bolatto, Alberto; Molina, Juan; Saito, Toshiki; Yamashita, Takuji; Zhuang, Ming-Yang; Nakanishi, Kouichiro; Iono, Daisuke; Wang, Ran; Ho, Luis C. Montoya Arroyave, I.; Cicone, C.; Makroleivaditi, E.; Weiss, A.; Lundgren, A.; Severgnini, P.; De Breuck, C.; Baumschlager, B.; Schimek, A.;	We present a high sensitivity, ground-based spectral line survey of low-J carbon monoxide (CO(J<SUB>up</SUB> → J<SUB>up</SUB> − 1) with J<SUB>up</SUB> = 1, 2, 3) and neutral carbon [CI] <SUP>3</SUP>P<SUB>1</SUB>−<SUP>3</SUP>P<SUB>0</SUB> ([CI](1-0)) in 36 local ultra-luminous infrared galaxies (ULIRGs) and 4 additional LIRGs, all of which have previous Herschel OH 119 μm observations. The study is based on new single-dish observations conducted with the Atacama Pathfinder Experiment (APEX) and complemented with archival APEX and Atacama Large Millimeter Array (ALMA and ACA) data. Our methods are optimized for a multi-tracer study of the total molecular line emission from these ULIRGs, including any extended low-surface-brightness components. We find a tight correlation between the CO and [CI] line luminosities, which suggests that the emission from CO(1-0) (and CO(2-1)) arises from similar regions as the [CI](1-0), at least when averaged over galactic scales. By using [CI] to compute molecular gas masses, we	2020	We propose CI(2-1) and CO(4-3) observations towards ~40 local ultra/luminous infrared galaxies (U/LIRGs), which are forming stars violently (starburst) and are often observed as interacting galaxies. ULIRGs are the key population to connect the local and high-z Universe. While we have observed CI and high-J CO from galaxies in the early Universe, we have not yet known the information of these lines even in the well studied nearby galaxies. At first we check the consistency between CO and CI based gas mass. Second, we directly connect enormous starburst triggered by a galaxy merger and local physics around the newly born young massive stars. We use the line ratios of the CI(2-1) and CO(4-3) as diagnostics of the photodissociation region (PDR). We look for the evolutionary track along the merger sequence in gas density (n) - UV radiation strength (G0) plane for the first time. In addition, comparing with prior CI observations towards high-z sources, we verify whether the ISM of the galaxies in the early Univers	NGC_7771_b_08_7M	Tadaki, Ken-ichi; Ando, Misaki; Saito, Toshiki; Iono, Daisuke; Nakanishi, Kouichiro; Ueda, Junko;	32.67546814976686	1.6050616316277402	0.91	uid://A001/X133d/X18c0	uid://A001/X133d/X18c1	uid://A002/Xde0eb4/X1d9a	CI(1-0) and CO(4-3) survey for nearby ~40 U/LIRGs- Band8 ACA stand alone observation -	S	BANDPASS FLUX WVR	F	15.836007398542868	T	2020ApJ...897L..19M 2020MNRAS.497.3591S 2021ApJS..257...28M 2023A&A...672A..36L 2023A&A...673A..13M 2024MNRAS.527.6321Q	Merging and interacting galaxies;Surveys of galaxies	Galaxy evolution	tmichiyama	Michiyama, Tomonari	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.01099.S	ALMA	JAO	ALMA	uid://A001/X3621/X440c.source.J1256-0547.spw.10	image	2		J1256-0547	194.04652737503682	-5.789312555561366	0.012526593247178497	Circle ICRS 194.046527 -5.789313 0.006263			128	1	2	4.707529993582289	60321.474666	60321.481672	604.8	604.8	0.001295857282719605	0.0013070674110553392	7340.409938964844	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3621/X440c	application/x-votable+xml; content=datalink		2023.1.01099.S	Public	305.10434212830796	57.0623580272927	6	1.7655681230704115E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2025-01-16T02:50:38.000	4.707529993582289	[211.36..213.35GHz,31250.00kHz,11.6mJy/beam@10km/s,690.6uJy/beam@native, XX YY] U [213.36..215.35GHz,31250.00kHz,10.6mJy/beam@10km/s,630.9uJy/beam@native, XX YY] U [227.36..229.35GHz,31250.00kHz,10.4mJy/beam@10km/s,640.5uJy/beam@native, XX YY] U [229.36..231.35GHz,31250.00kHz,11.7mJy/beam@10km/s,725.2uJy/beam@native, XX YY]	230.35473856146155	40841.37813729204	ALMA						The photon ring around the supermassive black hole (SMBH) in M87 has been imaged with the Event Horizon Telescope (EHT), and results on SgrA* are in the pipeline. With ALMA passive-phasing, the EHT can now detect sources of a few 10s of mJy. Additional SMBH photon rings are likely resolvable by the EHT, but these SMBHs are faint at centimeter radio (weak/no jets), and their 230 GHz flux (accretion inflow) is unknown. We propose to measure the 230 GHz flux of 68 SMBHs with photon ring > 8 microarcsec (piggy-backing 611 more SMBHs with photon ring > 2 microarcsec) and 124 SMBH binary (SMBHB) candidates. i.e., a total of 803 'large ring' SMBHs and SMBHB candidates. Those with nuclear flux > 10mJy will be followed up with the 12m array, VLBA, and eventually the best with EHT. Our longer term goals are to identify all SMBHs in which the EHT can resolve the photon ring and jet base, and to drive the technical requirements of the next-generation-EHT. Even only a few new EHT-feasible 'large ring' galaxies will allow	135225.8_a_06_7M	Lira, Paulina; Gurwell, Mark; Sasikumar, Silpa; Krichbaum, Thomas; Ramakrishnan, Venkatessh; Bower, Geoffrey; Reeves, Rodrigo; Cuadra, Jorge; Arratia, Vicente; Leigh, Nathan; Nagar, Neil; Nair, Dhanya; Rao, Ramprasad; Arevalo, Patricia;	11.69934669072083	0.3342836622686967	1.8	uid://A001/X3621/X440b	uid://A001/X3621/X440c	uid://A002/X11289b1/X1f239	Towards resolving orbiting binary SMBH, plus shadows, jets, and accretion flows of single SMBH: ACA fluxes	S	BANDPASS FLUX WVR	F	32.30911930509961	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	joacoh99	Hernandez-Yevenes, Joaquin	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.01099.S	ALMA	JAO	ALMA	uid://A001/X3621/X440c.source.J1256-0547.spw.17	image	2		J1256-0547	194.04652737503682	-5.789312555561366	0.012526593247178497	Circle ICRS 194.046527 -5.789313 0.006263			128	1	2	4.707529993582289	60321.474666	60321.481672	604.8	604.8	0.0013071564494368422	0.001318563782893238	7276.409938968044	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3621/X440c	application/x-votable+xml; content=datalink		2023.1.01099.S	Public	305.10434212830796	57.0623580272927	6	1.7966274530190318E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2025-01-16T02:50:38.000	4.707529993582289	[211.36..213.35GHz,31250.00kHz,11.6mJy/beam@10km/s,690.6uJy/beam@native, XX YY] U [213.36..215.35GHz,31250.00kHz,10.6mJy/beam@10km/s,630.9uJy/beam@native, XX YY] U [227.36..229.35GHz,31250.00kHz,10.4mJy/beam@10km/s,640.5uJy/beam@native, XX YY] U [229.36..231.35GHz,31250.00kHz,11.7mJy/beam@10km/s,725.2uJy/beam@native, XX YY]	228.35495784736236	40841.37813729204	ALMA						The photon ring around the supermassive black hole (SMBH) in M87 has been imaged with the Event Horizon Telescope (EHT), and results on SgrA* are in the pipeline. With ALMA passive-phasing, the EHT can now detect sources of a few 10s of mJy. Additional SMBH photon rings are likely resolvable by the EHT, but these SMBHs are faint at centimeter radio (weak/no jets), and their 230 GHz flux (accretion inflow) is unknown. We propose to measure the 230 GHz flux of 68 SMBHs with photon ring > 8 microarcsec (piggy-backing 611 more SMBHs with photon ring > 2 microarcsec) and 124 SMBH binary (SMBHB) candidates. i.e., a total of 803 'large ring' SMBHs and SMBHB candidates. Those with nuclear flux > 10mJy will be followed up with the 12m array, VLBA, and eventually the best with EHT. Our longer term goals are to identify all SMBHs in which the EHT can resolve the photon ring and jet base, and to drive the technical requirements of the next-generation-EHT. Even only a few new EHT-feasible 'large ring' galaxies will allow	135225.8_a_06_7M	Lira, Paulina; Gurwell, Mark; Sasikumar, Silpa; Krichbaum, Thomas; Ramakrishnan, Venkatessh; Bower, Geoffrey; Reeves, Rodrigo; Cuadra, Jorge; Arratia, Vicente; Leigh, Nathan; Nagar, Neil; Nair, Dhanya; Rao, Ramprasad; Arevalo, Patricia;	10.378736256635799	0.3342836622686967	1.8	uid://A001/X3621/X440b	uid://A001/X3621/X440c	uid://A002/X11289b1/X1f239	Towards resolving orbiting binary SMBH, plus shadows, jets, and accretion flows of single SMBH: ACA fluxes	S	BANDPASS FLUX WVR	F	32.30911930509961	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	joacoh99	Hernandez-Yevenes, Joaquin	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.01099.S	ALMA	JAO	ALMA	uid://A001/X3621/X440c.source.J1256-0547.spw.14	image	2		J1256-0547	194.04652737503682	-5.789312555561366	0.012526593247178497	Circle ICRS 194.046527 -5.789313 0.006263			128	1	2	4.707529993582289	60321.474666	60321.481672	604.8	604.8	0.0014051753068271356	0.0014183662031770569	6827.910061038357	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3621/X440c	application/x-votable+xml; content=datalink		2023.1.01099.S	Public	305.10434212830796	57.0623580272927	6	2.0775342986848923E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2025-01-16T02:50:38.000	4.707529993582289	[211.36..213.35GHz,31250.00kHz,11.6mJy/beam@10km/s,690.6uJy/beam@native, XX YY] U [213.36..215.35GHz,31250.00kHz,10.6mJy/beam@10km/s,630.9uJy/beam@native, XX YY] U [227.36..229.35GHz,31250.00kHz,10.4mJy/beam@10km/s,640.5uJy/beam@native, XX YY] U [229.36..231.35GHz,31250.00kHz,11.7mJy/beam@10km/s,725.2uJy/beam@native, XX YY]	212.35671594804813	40841.37813729204	ALMA						The photon ring around the supermassive black hole (SMBH) in M87 has been imaged with the Event Horizon Telescope (EHT), and results on SgrA* are in the pipeline. With ALMA passive-phasing, the EHT can now detect sources of a few 10s of mJy. Additional SMBH photon rings are likely resolvable by the EHT, but these SMBHs are faint at centimeter radio (weak/no jets), and their 230 GHz flux (accretion inflow) is unknown. We propose to measure the 230 GHz flux of 68 SMBHs with photon ring > 8 microarcsec (piggy-backing 611 more SMBHs with photon ring > 2 microarcsec) and 124 SMBH binary (SMBHB) candidates. i.e., a total of 803 'large ring' SMBHs and SMBHB candidates. Those with nuclear flux > 10mJy will be followed up with the 12m array, VLBA, and eventually the best with EHT. Our longer term goals are to identify all SMBHs in which the EHT can resolve the photon ring and jet base, and to drive the technical requirements of the next-generation-EHT. Even only a few new EHT-feasible 'large ring' galaxies will allow	135225.8_a_06_7M	Lira, Paulina; Gurwell, Mark; Sasikumar, Silpa; Krichbaum, Thomas; Ramakrishnan, Venkatessh; Bower, Geoffrey; Reeves, Rodrigo; Cuadra, Jorge; Arratia, Vicente; Leigh, Nathan; Nagar, Neil; Nair, Dhanya; Rao, Ramprasad; Arevalo, Patricia;	11.603508413418018	0.3342836622686967	1.8	uid://A001/X3621/X440b	uid://A001/X3621/X440c	uid://A002/X11289b1/X1f239	Towards resolving orbiting binary SMBH, plus shadows, jets, and accretion flows of single SMBH: ACA fluxes	S	BANDPASS FLUX WVR	F	32.30911930509961	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	joacoh99	Hernandez-Yevenes, Joaquin	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.01099.S	ALMA	JAO	ALMA	uid://A001/X3621/X440c.source.J1256-0547.spw.6	image	2		J1256-0547	194.04652737503682	-5.789312555561366	0.012526593247178497	Circle ICRS 194.046527 -5.789313 0.006263			128	1	2	4.707529993582289	60321.474666	60321.481672	604.8	604.8	0.0013921264975948612	0.001405072414991022	6891.910061035156	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3621/X440c	application/x-votable+xml; content=datalink		2023.1.01099.S	Public	305.10434212830796	57.0623580272927	6	2.038950705470846E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2025-01-16T02:50:38.000	4.707529993582289	[211.36..213.35GHz,31250.00kHz,11.6mJy/beam@10km/s,690.6uJy/beam@native, XX YY] U [213.36..215.35GHz,31250.00kHz,10.6mJy/beam@10km/s,630.9uJy/beam@native, XX YY] U [227.36..229.35GHz,31250.00kHz,10.4mJy/beam@10km/s,640.5uJy/beam@native, XX YY] U [229.36..231.35GHz,31250.00kHz,11.7mJy/beam@10km/s,725.2uJy/beam@native, XX YY]	214.35649666214726	40841.37813729204	ALMA						The photon ring around the supermassive black hole (SMBH) in M87 has been imaged with the Event Horizon Telescope (EHT), and results on SgrA* are in the pipeline. With ALMA passive-phasing, the EHT can now detect sources of a few 10s of mJy. Additional SMBH photon rings are likely resolvable by the EHT, but these SMBHs are faint at centimeter radio (weak/no jets), and their 230 GHz flux (accretion inflow) is unknown. We propose to measure the 230 GHz flux of 68 SMBHs with photon ring > 8 microarcsec (piggy-backing 611 more SMBHs with photon ring > 2 microarcsec) and 124 SMBH binary (SMBHB) candidates. i.e., a total of 803 'large ring' SMBHs and SMBHB candidates. Those with nuclear flux > 10mJy will be followed up with the 12m array, VLBA, and eventually the best with EHT. Our longer term goals are to identify all SMBHs in which the EHT can resolve the photon ring and jet base, and to drive the technical requirements of the next-generation-EHT. Even only a few new EHT-feasible 'large ring' galaxies will allow	135225.8_a_06_7M	Lira, Paulina; Gurwell, Mark; Sasikumar, Silpa; Krichbaum, Thomas; Ramakrishnan, Venkatessh; Bower, Geoffrey; Reeves, Rodrigo; Cuadra, Jorge; Arratia, Vicente; Leigh, Nathan; Nagar, Neil; Nair, Dhanya; Rao, Ramprasad; Arevalo, Patricia;	10.550878698187498	0.3342836622686967	1.8	uid://A001/X3621/X440b	uid://A001/X3621/X440c	uid://A002/X11289b1/X1f239	Towards resolving orbiting binary SMBH, plus shadows, jets, and accretion flows of single SMBH: ACA fluxes	S	BANDPASS FLUX WVR	F	32.30911930509961	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	joacoh99	Hernandez-Yevenes, Joaquin	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X161b.source.UGC_06314.spw.11	image	2		UGC_06314	169.54079000000598	30.406790000000143	0.011901749610033563	Circle ICRS 169.540790 30.406790 0.005951			128	1	2	3.491542649429291	61005.488441	61005.508248	362.88	362.88	0.0012338756216828304	0.0012440349269409404	7712.25	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X161b	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	198.27149832410475	69.33599522851904	6	1.6000489754590567E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N605:CM04 T701:PM04 T702:PM03 T703:PM01	F	2026-12-03T23:02:26.000	3.491542649429291	[222.99..224.97GHz,31250.00kHz,16.9mJy/beam@10km/s,1mJy/beam@native, XX YY] U [224.99..226.97GHz,31250.00kHz,16.2mJy/beam@10km/s,995.5uJy/beam@native, XX YY] U [238.98..240.97GHz,31250.00kHz,17.1mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [240.98..242.97GHz,31250.00kHz,17.8mJy/beam@10km/s,1.1mJy/beam@native, XX YY]	241.97604520910585	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	WISEA_J1_c_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	17.768625505472315	0.5285208182025438	0.2795362	uid://A001/X3833/X161a	uid://A001/X3833/X161b	uid://A002/X1323597/X25abd	Towards resolving orbiting binary supermassive black holes with the EHT	S	TARGET	T	30.251728112753515	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X161b.source.UGC_06314.spw.18	image	2		UGC_06314	169.54079000000598	30.406790000000143	0.011901749610033563	Circle ICRS 169.540790 30.406790 0.005951			128	1	2	3.491542649429291	61005.488441	61005.508248	362.88	362.88	0.001244115585346554	0.001254444920772236	7648.2500000032	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X161b	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	198.27149832410475	69.33599522851904	6	1.6268280305724474E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N605:CM04 T701:PM04 T702:PM03 T703:PM01	F	2026-12-03T23:02:26.000	3.491542649429291	[222.99..224.97GHz,31250.00kHz,16.9mJy/beam@10km/s,1mJy/beam@native, XX YY] U [224.99..226.97GHz,31250.00kHz,16.2mJy/beam@10km/s,995.5uJy/beam@native, XX YY] U [238.98..240.97GHz,31250.00kHz,17.1mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [240.98..242.97GHz,31250.00kHz,17.8mJy/beam@10km/s,1.1mJy/beam@native, XX YY]	239.97624318268424	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	WISEA_J1_c_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	17.144658307640682	0.5285208182025438	0.2795362	uid://A001/X3833/X161a	uid://A001/X3833/X161b	uid://A002/X1323597/X25abd	Towards resolving orbiting binary supermassive black holes with the EHT	S	TARGET	T	30.251728112753515	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X161b.source.UGC_06314.spw.15	image	2		UGC_06314	169.54079000000598	30.406790000000143	0.011901749610033563	Circle ICRS 169.540790 30.406790 0.005951			128	1	2	3.491542649429291	61005.488441	61005.508248	362.88	362.88	0.001332589098968159	0.001344446784417021	7199.7500000032	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X161b	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	198.27149832410475	69.33599522851904	6	1.8675369005790219E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N605:CM04 T701:PM04 T702:PM03 T703:PM01	F	2026-12-03T23:02:26.000	3.491542649429291	[222.99..224.97GHz,31250.00kHz,16.9mJy/beam@10km/s,1mJy/beam@native, XX YY] U [224.99..226.97GHz,31250.00kHz,16.2mJy/beam@10km/s,995.5uJy/beam@native, XX YY] U [238.98..240.97GHz,31250.00kHz,17.1mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [240.98..242.97GHz,31250.00kHz,17.8mJy/beam@10km/s,1.1mJy/beam@native, XX YY]	223.977826970512	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	WISEA_J1_c_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	16.91127010422197	0.5285208182025438	0.2795362	uid://A001/X3833/X161a	uid://A001/X3833/X161b	uid://A002/X1323597/X25abd	Towards resolving orbiting binary supermassive black holes with the EHT	S	TARGET	T	30.251728112753515	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01084.S	ALMA	JAO	ALMA	uid://A001/X3833/X161b.source.UGC_06314.spw.7	image	2		UGC_06314	169.54079000000598	30.406790000000143	0.011901749610033563	Circle ICRS 169.540790 30.406790 0.005951			128	1	2	3.491542649429291	61005.488441	61005.508248	362.88	362.88	0.0013208478217587702	0.0013324965612722152	7263.75	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X161b	application/x-votable+xml; content=datalink		2025.1.01084.S	Proprietary	198.27149832410475	69.33599522851904	6	1.834628771391425E-7	2.0E9	J501:CM10 J502:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N603:CM09 N605:CM04 T701:PM04 T702:PM03 T703:PM01	F	2026-12-03T23:02:26.000	3.491542649429291	[222.99..224.97GHz,31250.00kHz,16.9mJy/beam@10km/s,1mJy/beam@native, XX YY] U [224.99..226.97GHz,31250.00kHz,16.2mJy/beam@10km/s,995.5uJy/beam@native, XX YY] U [238.98..240.97GHz,31250.00kHz,17.1mJy/beam@10km/s,1.1mJy/beam@native, XX YY] U [240.98..242.97GHz,31250.00kHz,17.8mJy/beam@10km/s,1.1mJy/beam@native, XX YY]	225.97762899693356	38872.24324937599	ALMA						Gravitationally bound supermassive black hole binaries (SMBHB) are a highly elusive population - to date, only one confirmed candidate exists. Our understanding of SMBHB evolution, their gravitational wave (GW) emission, the interpretation of current SMBHB GW observatory findings, and predictions for future SMBHB GW observatories, are all limited by this paucity of confirmed SMBHB. We show that the unprecedented resolution of the Event Horizon Telescope (EHT), its relatively high radio frequency, its increasing sensitivity, among other factors, combine to make it a powerful (but as yet unproven) hunter of SMBHB down to sub-pc (and even milli-pc) separations, thus strong GW regimes. We propose an economical and efficient ACA program to complete 230 GHz flux measurements of all ALMA accessible SMBHB candidates with estimated separations of <=100 pc and without existing such flux measurements. A fully 230 GHz characterized SMBHB sample we will enable an optimal selection of targets for which the highest resoluti	WISEA_J1_c_06_7M	Arratia, Vicente; Nagar, Neil; Nair, Dhanya; Hernandez-Yevenes, Joaquin;	16.215557129539476	0.5285208182025438	0.2795362	uid://A001/X3833/X161a	uid://A001/X3833/X161b	uid://A002/X1323597/X25abd	Towards resolving orbiting binary supermassive black holes with the EHT	S	TARGET	T	30.251728112753515	T		Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	silpa	Sasikumar, Silpa	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.00430.S	ALMA	JAO	ALMA	uid://A001/X3645/X287.source.J1118+1234.spw.7	image	2		J1118+1234	169.73875598303619	12.57825500560264	0.006941571605586213	Circle ICRS 169.738756 12.578255 0.003471			128	1	2	1.217117368008334	60412.155704	60412.192061	211.68	211.68	0.001320635565872699	0.0013322824334721457	7263.75	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3645/X287	application/x-votable+xml; content=datalink		2023.1.00430.S	Public	242.27879635445197	63.91725217414599	6	1.8340391811894993E-7	2.0E9	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14	F	2025-05-01T17:57:03.000	1.217117368008334	[223.02..225.01GHz,31250.00kHz,1.6mJy/beam@10km/s,100.4uJy/beam@native, XX YY] U [225.02..227.01GHz,31250.00kHz,1.6mJy/beam@10km/s,97uJy/beam@native, XX YY] U [239.02..241.01GHz,31250.00kHz,1.7mJy/beam@10km/s,106.4uJy/beam@native, XX YY] U [241.02..243.01GHz,31250.00kHz,1.8mJy/beam@10km/s,113.8uJy/beam@native, XX YY]	226.01394869262742	38872.24324937599	ALMA						Using ground- and space-based imaging and rest-frame optical spectroscopy, we have identified a remarkable sample of 12 strongly-lensed massive red quiescent galaxies at z=0.7 to z=2.5 (to be combined with 6 archival targets). Using ALMA Band 6 continuum imaging, we propose to measure their total dust masses down to unprecedented dust fraction levels of 0.01%. Tension exists in the literature regarding the ISM in quiescent galaxies: stacked dust continuum (15 arcsec resolution) of statistical samples at high redshift yield moderate dust masses, whereas recent model predictions suggest dust masses should be orders of magnitude lower. Gravitationally lensed quiescent galaxies offer a unique opportunity to resolve this conflict by pushing into uncharted parameter space, and have started to point towards consensus with theoretical predictions. In this proposal, we aim to triple the number of individually observed galaxies. Such strong limits on dust mass are only possible due to the combination of strong-lensing	J1116+14_a_06_TM1	Pope, Alexandra; Narayanan, Desika; Mowla, Lamiya; Antwi-Danso, Jacqueline; Bodansky, Sarah; Valentino, Francesco; Sharon, Keren; Sukay, Ezra; Long, Arianna; Spilker, Justin; Williams, Christina; McKinney, Jed; Khullar, Gourav; Leja, Joel; Nelson, Erica; Manning, Sinclaire; Gladders, Michael; Bezanson, Rachel;	1.5795445241328334	0.051908457906862805	1.4046085	uid://A001/X3645/X286	uid://A001/X3645/X287	uid://A002/X115cf83/X788	Detecting Dust in a Sample of Lensed Quiescent Galaxies at Cosmic Noon	S	PHASE WVR	F	12.186847993401921	T		Early-type galaxies;null	Galaxy evolution	kwhitaker	Whitaker, Katherine	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.00430.S	ALMA	JAO	ALMA	uid://A001/X3645/X287.source.J1118+1234.spw.11	image	2		J1118+1234	169.73875598303619	12.57825500560264	0.006941571605586213	Circle ICRS 169.738756 12.578255 0.003471			128	1	2	1.217117368008334	60412.155704	60412.192061	211.68	211.68	0.0012336773419422973	0.0012438350146335786	7712.25	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3645/X287	application/x-votable+xml; content=datalink		2023.1.00430.S	Public	242.27879635445197	63.91725217414599	6	1.5995347715976313E-7	2.0E9	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14	F	2025-05-01T17:57:03.000	1.217117368008334	[223.02..225.01GHz,31250.00kHz,1.6mJy/beam@10km/s,100.4uJy/beam@native, XX YY] U [225.02..227.01GHz,31250.00kHz,1.6mJy/beam@10km/s,97uJy/beam@native, XX YY] U [239.02..241.01GHz,31250.00kHz,1.7mJy/beam@10km/s,106.4uJy/beam@native, XX YY] U [241.02..243.01GHz,31250.00kHz,1.8mJy/beam@10km/s,113.8uJy/beam@native, XX YY]	242.01493621068954	38872.24324937599	ALMA						Using ground- and space-based imaging and rest-frame optical spectroscopy, we have identified a remarkable sample of 12 strongly-lensed massive red quiescent galaxies at z=0.7 to z=2.5 (to be combined with 6 archival targets). Using ALMA Band 6 continuum imaging, we propose to measure their total dust masses down to unprecedented dust fraction levels of 0.01%. Tension exists in the literature regarding the ISM in quiescent galaxies: stacked dust continuum (15 arcsec resolution) of statistical samples at high redshift yield moderate dust masses, whereas recent model predictions suggest dust masses should be orders of magnitude lower. Gravitationally lensed quiescent galaxies offer a unique opportunity to resolve this conflict by pushing into uncharted parameter space, and have started to point towards consensus with theoretical predictions. In this proposal, we aim to triple the number of individually observed galaxies. Such strong limits on dust mass are only possible due to the combination of strong-lensing	J1116+14_a_06_TM1	Pope, Alexandra; Narayanan, Desika; Mowla, Lamiya; Antwi-Danso, Jacqueline; Bodansky, Sarah; Valentino, Francesco; Sharon, Keren; Sukay, Ezra; Long, Arianna; Spilker, Justin; Williams, Christina; McKinney, Jed; Khullar, Gourav; Leja, Joel; Nelson, Erica; Manning, Sinclaire; Gladders, Michael; Bezanson, Rachel;	1.7908987750828325	0.051908457906862805	1.4046085	uid://A001/X3645/X286	uid://A001/X3645/X287	uid://A002/X115cf83/X788	Detecting Dust in a Sample of Lensed Quiescent Galaxies at Cosmic Noon	S	PHASE WVR	F	12.186847993401921	T		Early-type galaxies;null	Galaxy evolution	kwhitaker	Whitaker, Katherine	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.00430.S	ALMA	JAO	ALMA	uid://A001/X3645/X287.source.J1118+1234.spw.15	image	2		J1118+1234	169.73875598303619	12.57825500560264	0.006941571605586213	Circle ICRS 169.738756 12.578255 0.003471			128	1	2	1.217117368008334	60412.155704	60412.192061	211.68	211.68	0.0013323749562975874	0.0013442307362555286	7199.7500000032	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3645/X287	application/x-votable+xml; content=datalink		2023.1.00430.S	Public	242.27879635445197	63.91725217414599	6	1.8669367347713744E-7	2.0E9	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14	F	2025-05-01T17:57:03.000	1.217117368008334	[223.02..225.01GHz,31250.00kHz,1.6mJy/beam@10km/s,100.4uJy/beam@native, XX YY] U [225.02..227.01GHz,31250.00kHz,1.6mJy/beam@10km/s,97uJy/beam@native, XX YY] U [239.02..241.01GHz,31250.00kHz,1.7mJy/beam@10km/s,106.4uJy/beam@native, XX YY] U [241.02..243.01GHz,31250.00kHz,1.8mJy/beam@10km/s,113.8uJy/beam@native, XX YY]	224.01382525296964	38872.24324937599	ALMA						Using ground- and space-based imaging and rest-frame optical spectroscopy, we have identified a remarkable sample of 12 strongly-lensed massive red quiescent galaxies at z=0.7 to z=2.5 (to be combined with 6 archival targets). Using ALMA Band 6 continuum imaging, we propose to measure their total dust masses down to unprecedented dust fraction levels of 0.01%. Tension exists in the literature regarding the ISM in quiescent galaxies: stacked dust continuum (15 arcsec resolution) of statistical samples at high redshift yield moderate dust masses, whereas recent model predictions suggest dust masses should be orders of magnitude lower. Gravitationally lensed quiescent galaxies offer a unique opportunity to resolve this conflict by pushing into uncharted parameter space, and have started to point towards consensus with theoretical predictions. In this proposal, we aim to triple the number of individually observed galaxies. Such strong limits on dust mass are only possible due to the combination of strong-lensing	J1116+14_a_06_TM1	Pope, Alexandra; Narayanan, Desika; Mowla, Lamiya; Antwi-Danso, Jacqueline; Bodansky, Sarah; Valentino, Francesco; Sharon, Keren; Sukay, Ezra; Long, Arianna; Spilker, Justin; Williams, Christina; McKinney, Jed; Khullar, Gourav; Leja, Joel; Nelson, Erica; Manning, Sinclaire; Gladders, Michael; Bezanson, Rachel;	1.6419560957216233	0.051908457906862805	1.4046085	uid://A001/X3645/X286	uid://A001/X3645/X287	uid://A002/X115cf83/X788	Detecting Dust in a Sample of Lensed Quiescent Galaxies at Cosmic Noon	S	PHASE WVR	F	12.186847993401921	T		Early-type galaxies;null	Galaxy evolution	kwhitaker	Whitaker, Katherine	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.00430.S	ALMA	JAO	ALMA	uid://A001/X3645/X287.source.J1118+1234.spw.18	image	2		J1118+1234	169.73875598303619	12.57825500560264	0.006941571605586213	Circle ICRS 169.738756 12.578255 0.003471			128	1	2	1.217117368008334	60412.155704	60412.192061	211.68	211.68	0.0012439156600776526	0.0012542433356132194	7648.2500000032	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3645/X287	application/x-votable+xml; content=datalink		2023.1.00430.S	Public	242.27879635445197	63.91725217414599	6	1.626305220790981E-7	2.0E9	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14	F	2025-05-01T17:57:03.000	1.217117368008334	[223.02..225.01GHz,31250.00kHz,1.6mJy/beam@10km/s,100.4uJy/beam@native, XX YY] U [225.02..227.01GHz,31250.00kHz,1.6mJy/beam@10km/s,97uJy/beam@native, XX YY] U [239.02..241.01GHz,31250.00kHz,1.7mJy/beam@10km/s,106.4uJy/beam@native, XX YY] U [241.02..243.01GHz,31250.00kHz,1.8mJy/beam@10km/s,113.8uJy/beam@native, XX YY]	240.01481277103176	38872.24324937599	ALMA						Using ground- and space-based imaging and rest-frame optical spectroscopy, we have identified a remarkable sample of 12 strongly-lensed massive red quiescent galaxies at z=0.7 to z=2.5 (to be combined with 6 archival targets). Using ALMA Band 6 continuum imaging, we propose to measure their total dust masses down to unprecedented dust fraction levels of 0.01%. Tension exists in the literature regarding the ISM in quiescent galaxies: stacked dust continuum (15 arcsec resolution) of statistical samples at high redshift yield moderate dust masses, whereas recent model predictions suggest dust masses should be orders of magnitude lower. Gravitationally lensed quiescent galaxies offer a unique opportunity to resolve this conflict by pushing into uncharted parameter space, and have started to point towards consensus with theoretical predictions. In this proposal, we aim to triple the number of individually observed galaxies. Such strong limits on dust mass are only possible due to the combination of strong-lensing	J1116+14_a_06_TM1	Pope, Alexandra; Narayanan, Desika; Mowla, Lamiya; Antwi-Danso, Jacqueline; Bodansky, Sarah; Valentino, Francesco; Sharon, Keren; Sukay, Ezra; Long, Arianna; Spilker, Justin; Williams, Christina; McKinney, Jed; Khullar, Gourav; Leja, Joel; Nelson, Erica; Manning, Sinclaire; Gladders, Michael; Bezanson, Rachel;	1.6822211797695654	0.051908457906862805	1.4046085	uid://A001/X3645/X286	uid://A001/X3645/X287	uid://A002/X115cf83/X788	Detecting Dust in a Sample of Lensed Quiescent Galaxies at Cosmic Noon	S	PHASE WVR	F	12.186847993401921	T		Early-type galaxies;null	Galaxy evolution	kwhitaker	Whitaker, Katherine	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01774.S	ALMA	JAO	ALMA	uid://A001/X37fb/X2b8.source.J0426+2327.spw.31	cube	2		J0426+2327	66.73222832074735	23.461009394411935	0.00716989593709565	Circle ICRS 66.732228 23.461009 0.003585			480	1	2	0.04970366979888649	60945.268253	60945.332112	326.592	326.592	0.0012940929281408447	0.0012993399082934665	102195.95862646766	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X37fb/X2b8	application/x-votable+xml; content=datalink		2024.1.01774.S	Proprietary	173.88796554914416	-17.445755967830237	6	1.2663548318812418E-8	9.375E8	A042:DV03 A072:DV09 A074:DV14 A075:DA50 A076:DA48 A082:DA64 A083:DA56 A085:DV22 A086:DV04 A087:DV05 A088:DA46 A089:DA58 A091:DA59 A092:DA54 A094:DV07 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A110:DA51 A111:DV19 A115:DV12 A116:DA57 A118:DV13 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A124:DV01 A125:DV02 A126:DA47 A127:DA65 A128:DA60 A129:DA42 A130:DA53 A131:DV20 A132:DV25 A134:DV10 A135:DV15 P401:DA52 P404:DA41 P408:DV08 P410:DA62 S301:DV21 S307:DV18 W208:DA43 W210:DV23	F	2026-11-22T01:03:47.000	0.04970366979888649	[219.53..219.58GHz,141.11kHz,1.3mJy/beam@10km/s,468.6uJy/beam@native, XX YY] U [220.36..220.42GHz,141.11kHz,1.3mJy/beam@10km/s,468.8uJy/beam@native, XX YY] U [230.50..230.56GHz,35.28kHz,1.3mJy/beam@10km/s,456.8uJy/beam@native, XX YY] U [230.73..231.66GHz,2257.81kHz,1.3mJy/beam@10km/s,114.2uJy/beam@native, XX YY]	231.1944854868674	45.88047175359646	ALMA						The usage of exoplanetary atmospheric abundances as chemical tracers of their disk formation and migration is complicated by the fact that planets are typically discovered after their progenitor disk has dissipated. The gold standard for testing where, when, and how a planet forms would be to measure its volatile composition in conjunction with that of its parent disk. The recently discovered target of this proposal, IRAS 04125+2902, presents the first opportunity to perform such an experiment. The target hosts a transiting 0.96 RJup planet as well as a transitional disk that is misaligned with the planetary orbital plane. We propose to fully characterize the IRAS 04125+2902 system with JWST and ALMA. We will use JWST observations to measure the bulk C/O and metallicity of IRAS 04125+2902 b's atmosphere, and to determine the C/O and water-enrichment in the the inner disk. With ALMA we will determine the C/O/N/H ratios in the outer disk. Our joint interdisciplinary program will measure the formation location a	IRAS_041_b_06_TM1	Mann, Andrew; Penzlin, Anna; Espaillat, Catherine; Seligman, Darryl; Thao, Pa Chia; Booth, Richard; Bergner, Jennifer; Qi, Chunhua; Welbanks, Luis; Barber, Madyson;	1.259607193801723	0.10510875114526666	0.5540856	uid://A001/X37fb/X2b7	uid://A001/X37fb/X2b8	uid://A002/X12f38f9/X6b71	Measuring the Bulk Properties of a 3 Myr Transiting Exoplanet and its Original Protoplanetary Disk	S	CHECK WVR	F	1.0071695850640119	T		Disks around low-mass stars;null	Disks and planet formation	afeinstein20	Feinstein, Adina	2257.8125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01774.S	ALMA	JAO	ALMA	uid://A001/X37fb/X2b8.source.J0426+2327.spw.25	cube	2		J0426+2327	66.73222832074735	23.461009394411935	0.00716989593709565	Circle ICRS 66.732228 23.461009 0.003585			480	1	2	0.04970366979888649	60945.268253	60945.332112	326.592	326.592	0.0013652722638000383	0.0013656358901834133	1556170.6309343239	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X37fb/X2b8	application/x-votable+xml; content=datalink		2024.1.01774.S	Proprietary	173.88796554914416	-17.445755967830237	6	8.776096234256785E-10	5.859375E7	A042:DV03 A072:DV09 A074:DV14 A075:DA50 A076:DA48 A082:DA64 A083:DA56 A085:DV22 A086:DV04 A087:DV05 A088:DA46 A089:DA58 A091:DA59 A092:DA54 A094:DV07 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A110:DA51 A111:DV19 A115:DV12 A116:DA57 A118:DV13 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A124:DV01 A125:DV02 A126:DA47 A127:DA65 A128:DA60 A129:DA42 A130:DA53 A131:DV20 A132:DV25 A134:DV10 A135:DV15 P401:DA52 P404:DA41 P408:DV08 P410:DA62 S301:DV21 S307:DV18 W208:DA43 W210:DV23	F	2026-11-22T01:03:47.000	0.04970366979888649	[219.53..219.58GHz,141.11kHz,1.3mJy/beam@10km/s,468.6uJy/beam@native, XX YY] U [220.36..220.42GHz,141.11kHz,1.3mJy/beam@10km/s,468.8uJy/beam@native, XX YY] U [230.50..230.56GHz,35.28kHz,1.3mJy/beam@10km/s,456.8uJy/beam@native, XX YY] U [230.73..231.66GHz,2257.81kHz,1.3mJy/beam@10km/s,114.2uJy/beam@native, XX YY]	219.555141668077	45.88047175359646	ALMA						The usage of exoplanetary atmospheric abundances as chemical tracers of their disk formation and migration is complicated by the fact that planets are typically discovered after their progenitor disk has dissipated. The gold standard for testing where, when, and how a planet forms would be to measure its volatile composition in conjunction with that of its parent disk. The recently discovered target of this proposal, IRAS 04125+2902, presents the first opportunity to perform such an experiment. The target hosts a transiting 0.96 RJup planet as well as a transitional disk that is misaligned with the planetary orbital plane. We propose to fully characterize the IRAS 04125+2902 system with JWST and ALMA. We will use JWST observations to measure the bulk C/O and metallicity of IRAS 04125+2902 b's atmosphere, and to determine the C/O and water-enrichment in the the inner disk. With ALMA we will determine the C/O/N/H ratios in the outer disk. Our joint interdisciplinary program will measure the formation location a	IRAS_041_b_06_TM1	Mann, Andrew; Penzlin, Anna; Espaillat, Catherine; Seligman, Darryl; Thao, Pa Chia; Booth, Richard; Bergner, Jennifer; Qi, Chunhua; Welbanks, Luis; Barber, Madyson;	1.3255592221527674	0.10510875114526666	0.5540856	uid://A001/X37fb/X2b7	uid://A001/X37fb/X2b8	uid://A002/X12f38f9/X6b71	Measuring the Bulk Properties of a 3 Myr Transiting Exoplanet and its Original Protoplanetary Disk	S	CHECK WVR	F	1.0071695850640119	T		Disks around low-mass stars;null	Disks and planet formation	afeinstein20	Feinstein, Adina	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01774.S	ALMA	JAO	ALMA	uid://A001/X37fb/X2b8.source.J0426+2327.spw.29	cube	2		J0426+2327	66.73222832074735	23.461009394411935	0.00716989593709565	Circle ICRS 66.732228 23.461009 0.003585			1920	1	2	0.04970366979888649	60945.268253	60945.332112	326.592	326.592	0.0013002693502327035	0.0013005996875503937	6534206.091211344	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X37fb/X2b8	application/x-votable+xml; content=datalink		2024.1.01774.S	Proprietary	173.88796554914416	-17.445755967830237	6	1.9900508196823555E-10	5.859375E7	A042:DV03 A072:DV09 A074:DV14 A075:DA50 A076:DA48 A082:DA64 A083:DA56 A085:DV22 A086:DV04 A087:DV05 A088:DA46 A089:DA58 A091:DA59 A092:DA54 A094:DV07 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A110:DA51 A111:DV19 A115:DV12 A116:DA57 A118:DV13 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A124:DV01 A125:DV02 A126:DA47 A127:DA65 A128:DA60 A129:DA42 A130:DA53 A131:DV20 A132:DV25 A134:DV10 A135:DV15 P401:DA52 P404:DA41 P408:DV08 P410:DA62 S301:DV21 S307:DV18 W208:DA43 W210:DV23	F	2026-11-22T01:03:47.000	0.04970366979888649	[219.53..219.58GHz,141.11kHz,1.3mJy/beam@10km/s,468.6uJy/beam@native, XX YY] U [220.36..220.42GHz,141.11kHz,1.3mJy/beam@10km/s,468.8uJy/beam@native, XX YY] U [230.50..230.56GHz,35.28kHz,1.3mJy/beam@10km/s,456.8uJy/beam@native, XX YY] U [230.73..231.66GHz,2257.81kHz,1.3mJy/beam@10km/s,114.2uJy/beam@native, XX YY]	230.53253238131188	45.88047175359646	ALMA						The usage of exoplanetary atmospheric abundances as chemical tracers of their disk formation and migration is complicated by the fact that planets are typically discovered after their progenitor disk has dissipated. The gold standard for testing where, when, and how a planet forms would be to measure its volatile composition in conjunction with that of its parent disk. The recently discovered target of this proposal, IRAS 04125+2902, presents the first opportunity to perform such an experiment. The target hosts a transiting 0.96 RJup planet as well as a transitional disk that is misaligned with the planetary orbital plane. We propose to fully characterize the IRAS 04125+2902 system with JWST and ALMA. We will use JWST observations to measure the bulk C/O and metallicity of IRAS 04125+2902 b's atmosphere, and to determine the C/O and water-enrichment in the the inner disk. With ALMA we will determine the C/O/N/H ratios in the outer disk. Our joint interdisciplinary program will measure the formation location a	IRAS_041_b_06_TM1	Mann, Andrew; Penzlin, Anna; Espaillat, Catherine; Seligman, Darryl; Thao, Pa Chia; Booth, Richard; Bergner, Jennifer; Qi, Chunhua; Welbanks, Luis; Barber, Madyson;	1.260991013701145	0.10510875114526666	0.5540856	uid://A001/X37fb/X2b7	uid://A001/X37fb/X2b8	uid://A002/X12f38f9/X6b71	Measuring the Bulk Properties of a 3 Myr Transiting Exoplanet and its Original Protoplanetary Disk	S	CHECK WVR	F	1.0071695850640119	T		Disks around low-mass stars;null	Disks and planet formation	afeinstein20	Feinstein, Adina	35.2783203125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01774.S	ALMA	JAO	ALMA	uid://A001/X37fb/X2b8.source.J0426+2327.spw.27	cube	2		J0426+2327	66.73222832074735	23.461009394411935	0.00716989593709565	Circle ICRS 66.732228 23.461009 0.003585			480	1	2	0.04970366979888649	60945.268253	60945.332112	326.592	326.592	0.0013600801515308192	0.0013604410170750968	1562111.3195156388	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X37fb/X2b8	application/x-votable+xml; content=datalink		2024.1.01774.S	Proprietary	173.88796554914416	-17.445755967830237	6	8.709463584054152E-10	5.859375E7	A042:DV03 A072:DV09 A074:DV14 A075:DA50 A076:DA48 A082:DA64 A083:DA56 A085:DV22 A086:DV04 A087:DV05 A088:DA46 A089:DA58 A091:DA59 A092:DA54 A094:DV07 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A110:DA51 A111:DV19 A115:DV12 A116:DA57 A118:DV13 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A124:DV01 A125:DV02 A126:DA47 A127:DA65 A128:DA60 A129:DA42 A130:DA53 A131:DV20 A132:DV25 A134:DV10 A135:DV15 P401:DA52 P404:DA41 P408:DV08 P410:DA62 S301:DV21 S307:DV18 W208:DA43 W210:DV23	F	2026-11-22T01:03:47.000	0.04970366979888649	[219.53..219.58GHz,141.11kHz,1.3mJy/beam@10km/s,468.6uJy/beam@native, XX YY] U [220.36..220.42GHz,141.11kHz,1.3mJy/beam@10km/s,468.8uJy/beam@native, XX YY] U [230.50..230.56GHz,35.28kHz,1.3mJy/beam@10km/s,456.8uJy/beam@native, XX YY] U [230.73..231.66GHz,2257.81kHz,1.3mJy/beam@10km/s,114.2uJy/beam@native, XX YY]	220.39340603876985	45.88047175359646	ALMA						The usage of exoplanetary atmospheric abundances as chemical tracers of their disk formation and migration is complicated by the fact that planets are typically discovered after their progenitor disk has dissipated. The gold standard for testing where, when, and how a planet forms would be to measure its volatile composition in conjunction with that of its parent disk. The recently discovered target of this proposal, IRAS 04125+2902, presents the first opportunity to perform such an experiment. The target hosts a transiting 0.96 RJup planet as well as a transitional disk that is misaligned with the planetary orbital plane. We propose to fully characterize the IRAS 04125+2902 system with JWST and ALMA. We will use JWST observations to measure the bulk C/O and metallicity of IRAS 04125+2902 b's atmosphere, and to determine the C/O and water-enrichment in the the inner disk. With ALMA we will determine the C/O/N/H ratios in the outer disk. Our joint interdisciplinary program will measure the formation location a	IRAS_041_b_06_TM1	Mann, Andrew; Penzlin, Anna; Espaillat, Catherine; Seligman, Darryl; Thao, Pa Chia; Booth, Richard; Bergner, Jennifer; Qi, Chunhua; Welbanks, Luis; Barber, Madyson;	1.3235718652211075	0.10510875114526666	0.5540856	uid://A001/X37fb/X2b7	uid://A001/X37fb/X2b8	uid://A002/X12f38f9/X6b71	Measuring the Bulk Properties of a 3 Myr Transiting Exoplanet and its Original Protoplanetary Disk	S	CHECK WVR	F	1.0071695850640119	T		Disks around low-mass stars;null	Disks and planet formation	afeinstein20	Feinstein, Adina	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.1.01709.S	ALMA	JAO	ALMA	uid://A001/X1465/X473.source.PKS_1136-135.spw.23	image	2		PKS_1136-135	174.79459441165915	-13.845455534806419	0.006942541218788679	Circle ICRS 174.794594 -13.845456 0.003471			128	1	2	0.7477207332604732	58858.453089	58858.457307	362.88	362.88	0.0012338496645666914	0.001244008756102882	7712.250000000001	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1465/X473	application/x-votable+xml; content=datalink		2019.1.01709.S	Public	277.5252034573481	45.431633590939086	6	1.5999816555128784E-7	2.0E9	A001:DA48 A002:DA44 A003:DV23 A005:DV22 A006:DV13 A007:DV21 A008:DA46 A010:DV15 A011:DV07 A015:DV25 A016:DV24 A017:DV14 A019:DA61 A022:DV01 A023:DV12 A024:DA58 A026:DV18 A027:DV17 A034:DV08 A035:DA43 A036:DA64 A040:DA65 A041:DV04 A043:DA42 A044:DA55 A045:DA57 A047:DV06 A048:DA50 A049:DA63 A050:DV19 A058:DA41 A060:DA47 A062:DV02 A066:DA54 A068:DV20 A069:DA45 A070:DA62 A072:DA53 A073:DA51 A076:DA56 A082:DA52 A083:DA59 A085:DA60 A088:DV11	F	2022-11-03T22:24:38.000	0.7477207332604732	[222.99..224.97GHz,31250.00kHz,1.3mJy/beam@10km/s,82.2uJy/beam@native, XX YY] U [224.99..226.97GHz,31250.00kHz,1.3mJy/beam@10km/s,79.4uJy/beam@native, XX YY] U [238.99..240.97GHz,31250.00kHz,1.4mJy/beam@10km/s,86.9uJy/beam@native, XX YY] U [240.99..242.97GHz,31250.00kHz,1.5mJy/beam@10km/s,93uJy/beam@native, XX YY]	241.9811357809062	38872.24324937599	ALMA	ALMA High-Level Data Products: submillimetre counterparts of SDSS quasars in the ALMA footprint Disentangling the AGN and Star formation Contributions to the Radio-X-Ray Emission of Radio-loud Quasars at 1 < Z < 2 The relativistic jet dichotomy and the end of the blazar sequence	Azadi, Mojegan Keenan, Mary Wong, A.	Azadi, Mojegan; Wilkes, Belinda; Kuraszkiewicz, Joanna; McDowell, Jonathan; Siebenmorgen, Ralf; Ashby, Matthew; Birkinshaw, Mark; Worrall, Diana; Abrams, Natasha; Barthel, Peter; Fazio, Giovanni G.; Haas, Martin; Hyman, Sóley; Martínez-Galarza, Rafael; Meyer, Eileen T. Keenan, Mary; Meyer, Eileen T.; Georganopoulos, Markos; Reddy, Karthik; French, Omar J. Wong, A.; Hatziminaoglou, E.; Borkar, A.; Popping, G.; Pérez-Fournon, I.; Poidevin, F.; Stoehr, F.; Messias, H.	Our understanding of the unification of jetted AGN has evolved greatly as jet samples have increased in size. Here, based on the largest-ever sample of over 2000 well-sampled jet spectral energy distributions, we examine the synchrotron peak frequency - peak luminosity plane, and find little evidence for the anticorrelation known as the blazar sequence. Instead, we find strong evidence for a dichotomy in jets, between those associated with efficient or 'quasar-mode' accretion (strong/type II jets) and those associated with inefficient accretion (weak/type I jets). Type II jets include those hosted by high-excitation radio galaxies, flat-spectrum radio quasars (FSRQ), and most low-frequency-peaked BL Lac objects. Type I jets include those hosted by low-excitation radio galaxies and blazars with synchrotron peak frequency above 10<SUP>15</SUP> Hz (nearly all BL Lac objects). We have derived estimates of the total jet power for over 1000 of our sources from low-frequency radio observations, and find that the jet	2021	We propose high-resolution continuum imaging in bands 3 and 6 of radio jets detected in the optical and/or X-rays, in order to accurately map the spectral energy distribution in the critical window between GHz radio and infrared. Our previous program on extremely powerful jets has revealed that the spectral energy distributions of these jets are more complex than previously understood, with multiple emission components of unclear origin, which are likely related to the unknown particle acceleration mechanism. This program compliments previous observations by selecting a sample with a range in morphology and extending down to low jet powers. These observations are critical to sampling the synchrotron spectrum of these resolved jets in a previously unexplored window, where our previous assumptions about the SED of resolved jets appear to be breaking down. For two targets, we request band 7 observations to confirm the completely unexpected turnover in the sub-mm spectrum which reveals that at least three distinc	PKS_1136_a_06_TM1	Sparks, William; Chiaberge, Marco; Georganopoulos, Markos; Perlman, Eric;	1.4632471606622652	0.04244699280278389	2.013234	uid://A001/X1465/X472	uid://A001/X1465/X473	uid://A002/Xe64b7b/X2448f	Probing the spectral evolution of jets with ALMA	S	TARGET	T	8.522737743623013	F	2021MNRAS.505.4726K 2023ApJ...945..145A 2023MNRAS.523...23W	Active Galactic Nuclei (AGN)/Quasars (QSO);Outflows, jets, feedback	Active galaxies	etmeyer	Meyer, Eileen	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.1.01709.S	ALMA	JAO	ALMA	uid://A001/X1465/X473.source.PKS_1136-135.spw.17	image	2		PKS_1136-135	174.79459441165915	-13.845455534806419	0.006942541218788679	Circle ICRS 174.794594 -13.845456 0.003471			128	1	2	0.7477207332604732	58858.453089	58858.457307	362.88	362.88	0.001332561065211216	0.0013444185012092419	7199.75	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1465/X473	application/x-votable+xml; content=datalink		2019.1.01709.S	Public	277.5252034573481	45.431633590939086	6	1.8674583264335469E-7	2.0E9	A001:DA48 A002:DA44 A003:DV23 A005:DV22 A006:DV13 A007:DV21 A008:DA46 A010:DV15 A011:DV07 A015:DV25 A016:DV24 A017:DV14 A019:DA61 A022:DV01 A023:DV12 A024:DA58 A026:DV18 A027:DV17 A034:DV08 A035:DA43 A036:DA64 A040:DA65 A041:DV04 A043:DA42 A044:DA55 A045:DA57 A047:DV06 A048:DA50 A049:DA63 A050:DV19 A058:DA41 A060:DA47 A062:DV02 A066:DA54 A068:DV20 A069:DA45 A070:DA62 A072:DA53 A073:DA51 A076:DA56 A082:DA52 A083:DA59 A085:DA60 A088:DV11	F	2022-11-03T22:24:38.000	0.7477207332604732	[222.99..224.97GHz,31250.00kHz,1.3mJy/beam@10km/s,82.2uJy/beam@native, XX YY] U [224.99..226.97GHz,31250.00kHz,1.3mJy/beam@10km/s,79.4uJy/beam@native, XX YY] U [238.99..240.97GHz,31250.00kHz,1.4mJy/beam@10km/s,86.9uJy/beam@native, XX YY] U [240.99..242.97GHz,31250.00kHz,1.5mJy/beam@10km/s,93uJy/beam@native, XX YY]	223.9825389046404	38872.24324937599	ALMA	ALMA High-Level Data Products: submillimetre counterparts of SDSS quasars in the ALMA footprint Disentangling the AGN and Star formation Contributions to the Radio-X-Ray Emission of Radio-loud Quasars at 1 < Z < 2 The relativistic jet dichotomy and the end of the blazar sequence	Azadi, Mojegan Keenan, Mary Wong, A.	Azadi, Mojegan; Wilkes, Belinda; Kuraszkiewicz, Joanna; McDowell, Jonathan; Siebenmorgen, Ralf; Ashby, Matthew; Birkinshaw, Mark; Worrall, Diana; Abrams, Natasha; Barthel, Peter; Fazio, Giovanni G.; Haas, Martin; Hyman, Sóley; Martínez-Galarza, Rafael; Meyer, Eileen T. Keenan, Mary; Meyer, Eileen T.; Georganopoulos, Markos; Reddy, Karthik; French, Omar J. Wong, A.; Hatziminaoglou, E.; Borkar, A.; Popping, G.; Pérez-Fournon, I.; Poidevin, F.; Stoehr, F.; Messias, H.	Our understanding of the unification of jetted AGN has evolved greatly as jet samples have increased in size. Here, based on the largest-ever sample of over 2000 well-sampled jet spectral energy distributions, we examine the synchrotron peak frequency - peak luminosity plane, and find little evidence for the anticorrelation known as the blazar sequence. Instead, we find strong evidence for a dichotomy in jets, between those associated with efficient or 'quasar-mode' accretion (strong/type II jets) and those associated with inefficient accretion (weak/type I jets). Type II jets include those hosted by high-excitation radio galaxies, flat-spectrum radio quasars (FSRQ), and most low-frequency-peaked BL Lac objects. Type I jets include those hosted by low-excitation radio galaxies and blazars with synchrotron peak frequency above 10<SUP>15</SUP> Hz (nearly all BL Lac objects). We have derived estimates of the total jet power for over 1000 of our sources from low-frequency radio observations, and find that the jet	2021	We propose high-resolution continuum imaging in bands 3 and 6 of radio jets detected in the optical and/or X-rays, in order to accurately map the spectral energy distribution in the critical window between GHz radio and infrared. Our previous program on extremely powerful jets has revealed that the spectral energy distributions of these jets are more complex than previously understood, with multiple emission components of unclear origin, which are likely related to the unknown particle acceleration mechanism. This program compliments previous observations by selecting a sample with a range in morphology and extending down to low jet powers. These observations are critical to sampling the synchrotron spectrum of these resolved jets in a previously unexplored window, where our previous assumptions about the SED of resolved jets appear to be breaking down. For two targets, we request band 7 observations to confirm the completely unexpected turnover in the sub-mm spectrum which reveals that at least three distinc	PKS_1136_a_06_TM1	Sparks, William; Chiaberge, Marco; Georganopoulos, Markos; Perlman, Eric;	1.3443254347516123	0.04244699280278389	2.013234	uid://A001/X1465/X472	uid://A001/X1465/X473	uid://A002/Xe64b7b/X2448f	Probing the spectral evolution of jets with ALMA	S	TARGET	T	8.522737743623013	F	2021MNRAS.505.4726K 2023ApJ...945..145A 2023MNRAS.523...23W	Active Galactic Nuclei (AGN)/Quasars (QSO);Outflows, jets, feedback	Active galaxies	etmeyer	Meyer, Eileen	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.1.01709.S	ALMA	JAO	ALMA	uid://A001/X1465/X473.source.PKS_1136-135.spw.19	image	2		PKS_1136-135	174.79459441165915	-13.845455534806419	0.006942541218788679	Circle ICRS 174.794594 -13.845456 0.003471			128	1	2	0.7477207332604732	58858.453089	58858.457307	362.88	362.88	0.0013208200350031942	0.001332468529461401	7263.75	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1465/X473	application/x-votable+xml; content=datalink		2019.1.01709.S	Public	277.5252034573481	45.431633590939086	6	1.83455158181033E-7	2.0E9	A001:DA48 A002:DA44 A003:DV23 A005:DV22 A006:DV13 A007:DV21 A008:DA46 A010:DV15 A011:DV07 A015:DV25 A016:DV24 A017:DV14 A019:DA61 A022:DV01 A023:DV12 A024:DA58 A026:DV18 A027:DV17 A034:DV08 A035:DA43 A036:DA64 A040:DA65 A041:DV04 A043:DA42 A044:DA55 A045:DA57 A047:DV06 A048:DA50 A049:DA63 A050:DV19 A058:DA41 A060:DA47 A062:DV02 A066:DA54 A068:DV20 A069:DA45 A070:DA62 A072:DA53 A073:DA51 A076:DA56 A082:DA52 A083:DA59 A085:DA60 A088:DV11	F	2022-11-03T22:24:38.000	0.7477207332604732	[222.99..224.97GHz,31250.00kHz,1.3mJy/beam@10km/s,82.2uJy/beam@native, XX YY] U [224.99..226.97GHz,31250.00kHz,1.3mJy/beam@10km/s,79.4uJy/beam@native, XX YY] U [238.99..240.97GHz,31250.00kHz,1.4mJy/beam@10km/s,86.9uJy/beam@native, XX YY] U [240.99..242.97GHz,31250.00kHz,1.5mJy/beam@10km/s,93uJy/beam@native, XX YY]	225.98238300200327	38872.24324937599	ALMA	ALMA High-Level Data Products: submillimetre counterparts of SDSS quasars in the ALMA footprint Disentangling the AGN and Star formation Contributions to the Radio-X-Ray Emission of Radio-loud Quasars at 1 < Z < 2 The relativistic jet dichotomy and the end of the blazar sequence	Azadi, Mojegan Keenan, Mary Wong, A.	Azadi, Mojegan; Wilkes, Belinda; Kuraszkiewicz, Joanna; McDowell, Jonathan; Siebenmorgen, Ralf; Ashby, Matthew; Birkinshaw, Mark; Worrall, Diana; Abrams, Natasha; Barthel, Peter; Fazio, Giovanni G.; Haas, Martin; Hyman, Sóley; Martínez-Galarza, Rafael; Meyer, Eileen T. Keenan, Mary; Meyer, Eileen T.; Georganopoulos, Markos; Reddy, Karthik; French, Omar J. Wong, A.; Hatziminaoglou, E.; Borkar, A.; Popping, G.; Pérez-Fournon, I.; Poidevin, F.; Stoehr, F.; Messias, H.	Our understanding of the unification of jetted AGN has evolved greatly as jet samples have increased in size. Here, based on the largest-ever sample of over 2000 well-sampled jet spectral energy distributions, we examine the synchrotron peak frequency - peak luminosity plane, and find little evidence for the anticorrelation known as the blazar sequence. Instead, we find strong evidence for a dichotomy in jets, between those associated with efficient or 'quasar-mode' accretion (strong/type II jets) and those associated with inefficient accretion (weak/type I jets). Type II jets include those hosted by high-excitation radio galaxies, flat-spectrum radio quasars (FSRQ), and most low-frequency-peaked BL Lac objects. Type I jets include those hosted by low-excitation radio galaxies and blazars with synchrotron peak frequency above 10<SUP>15</SUP> Hz (nearly all BL Lac objects). We have derived estimates of the total jet power for over 1000 of our sources from low-frequency radio observations, and find that the jet	2021	We propose high-resolution continuum imaging in bands 3 and 6 of radio jets detected in the optical and/or X-rays, in order to accurately map the spectral energy distribution in the critical window between GHz radio and infrared. Our previous program on extremely powerful jets has revealed that the spectral energy distributions of these jets are more complex than previously understood, with multiple emission components of unclear origin, which are likely related to the unknown particle acceleration mechanism. This program compliments previous observations by selecting a sample with a range in morphology and extending down to low jet powers. These observations are critical to sampling the synchrotron spectrum of these resolved jets in a previously unexplored window, where our previous assumptions about the SED of resolved jets appear to be breaking down. For two targets, we request band 7 observations to confirm the completely unexpected turnover in the sub-mm spectrum which reveals that at least three distinc	PKS_1136_a_06_TM1	Sparks, William; Chiaberge, Marco; Georganopoulos, Markos; Perlman, Eric;	1.2929908087923372	0.04244699280278389	2.013234	uid://A001/X1465/X472	uid://A001/X1465/X473	uid://A002/Xe64b7b/X2448f	Probing the spectral evolution of jets with ALMA	S	TARGET	T	8.522737743623013	F	2021MNRAS.505.4726K 2023ApJ...945..145A 2023MNRAS.523...23W	Active Galactic Nuclei (AGN)/Quasars (QSO);Outflows, jets, feedback	Active galaxies	etmeyer	Meyer, Eileen	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.1.01709.S	ALMA	JAO	ALMA	uid://A001/X1465/X473.source.PKS_1136-135.spw.21	image	2		PKS_1136-135	174.79459441165915	-13.845455534806419	0.006942541218788679	Circle ICRS 174.794594 -13.845456 0.003471			128	1	2	0.7477207332604732	58858.453089	58858.457307	362.88	362.88	0.0012440894128111636	0.0012544185309379824	7648.250000006399	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1465/X473	application/x-votable+xml; content=datalink		2019.1.01709.S	Public	277.5252034573481	45.431633590939086	6	1.626759583931558E-7	2.0E9	A001:DA48 A002:DA44 A003:DV23 A005:DV22 A006:DV13 A007:DV21 A008:DA46 A010:DV15 A011:DV07 A015:DV25 A016:DV24 A017:DV14 A019:DA61 A022:DV01 A023:DV12 A024:DA58 A026:DV18 A027:DV17 A034:DV08 A035:DA43 A036:DA64 A040:DA65 A041:DV04 A043:DA42 A044:DA55 A045:DA57 A047:DV06 A048:DA50 A049:DA63 A050:DV19 A058:DA41 A060:DA47 A062:DV02 A066:DA54 A068:DV20 A069:DA45 A070:DA62 A072:DA53 A073:DA51 A076:DA56 A082:DA52 A083:DA59 A085:DA60 A088:DV11	F	2022-11-03T22:24:38.000	0.7477207332604732	[222.99..224.97GHz,31250.00kHz,1.3mJy/beam@10km/s,82.2uJy/beam@native, XX YY] U [224.99..226.97GHz,31250.00kHz,1.3mJy/beam@10km/s,79.4uJy/beam@native, XX YY] U [238.99..240.97GHz,31250.00kHz,1.4mJy/beam@10km/s,86.9uJy/beam@native, XX YY] U [240.99..242.97GHz,31250.00kHz,1.5mJy/beam@10km/s,93uJy/beam@native, XX YY]	239.98129168374328	38872.24324937599	ALMA	ALMA High-Level Data Products: submillimetre counterparts of SDSS quasars in the ALMA footprint Disentangling the AGN and Star formation Contributions to the Radio-X-Ray Emission of Radio-loud Quasars at 1 < Z < 2 The relativistic jet dichotomy and the end of the blazar sequence	Azadi, Mojegan Keenan, Mary Wong, A.	Azadi, Mojegan; Wilkes, Belinda; Kuraszkiewicz, Joanna; McDowell, Jonathan; Siebenmorgen, Ralf; Ashby, Matthew; Birkinshaw, Mark; Worrall, Diana; Abrams, Natasha; Barthel, Peter; Fazio, Giovanni G.; Haas, Martin; Hyman, Sóley; Martínez-Galarza, Rafael; Meyer, Eileen T. Keenan, Mary; Meyer, Eileen T.; Georganopoulos, Markos; Reddy, Karthik; French, Omar J. Wong, A.; Hatziminaoglou, E.; Borkar, A.; Popping, G.; Pérez-Fournon, I.; Poidevin, F.; Stoehr, F.; Messias, H.	Our understanding of the unification of jetted AGN has evolved greatly as jet samples have increased in size. Here, based on the largest-ever sample of over 2000 well-sampled jet spectral energy distributions, we examine the synchrotron peak frequency - peak luminosity plane, and find little evidence for the anticorrelation known as the blazar sequence. Instead, we find strong evidence for a dichotomy in jets, between those associated with efficient or 'quasar-mode' accretion (strong/type II jets) and those associated with inefficient accretion (weak/type I jets). Type II jets include those hosted by high-excitation radio galaxies, flat-spectrum radio quasars (FSRQ), and most low-frequency-peaked BL Lac objects. Type I jets include those hosted by low-excitation radio galaxies and blazars with synchrotron peak frequency above 10<SUP>15</SUP> Hz (nearly all BL Lac objects). We have derived estimates of the total jet power for over 1000 of our sources from low-frequency radio observations, and find that the jet	2021	We propose high-resolution continuum imaging in bands 3 and 6 of radio jets detected in the optical and/or X-rays, in order to accurately map the spectral energy distribution in the critical window between GHz radio and infrared. Our previous program on extremely powerful jets has revealed that the spectral energy distributions of these jets are more complex than previously understood, with multiple emission components of unclear origin, which are likely related to the unknown particle acceleration mechanism. This program compliments previous observations by selecting a sample with a range in morphology and extending down to low jet powers. These observations are critical to sampling the synchrotron spectrum of these resolved jets in a previously unexplored window, where our previous assumptions about the SED of resolved jets appear to be breaking down. For two targets, we request band 7 observations to confirm the completely unexpected turnover in the sub-mm spectrum which reveals that at least three distinc	PKS_1136_a_06_TM1	Sparks, William; Chiaberge, Marco; Georganopoulos, Markos; Perlman, Eric;	1.3733796333603907	0.04244699280278389	2.013234	uid://A001/X1465/X472	uid://A001/X1465/X473	uid://A002/Xe64b7b/X2448f	Probing the spectral evolution of jets with ALMA	S	TARGET	T	8.522737743623013	F	2021MNRAS.505.4726K 2023ApJ...945..145A 2023MNRAS.523...23W	Active Galactic Nuclei (AGN)/Quasars (QSO);Outflows, jets, feedback	Active galaxies	etmeyer	Meyer, Eileen	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.31	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0013736319619614954	0.0013740031656910383	1787638.4745513492	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	7.68506374723663E-10	5.859375E7	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	218.21854034010187	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.0650830258340025	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	122.0703125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.27	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0013721463208535086	0.0013725167159124843	1789573.9745513492	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	7.66844701819194E-10	5.859375E7	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	218.45484086308494	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.0641997207205494	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	122.0703125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.33	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.001365261645008575	0.0013656284634748054	3111761.855069942	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	4.3879901245990373E-10	5.859375E7	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	219.55659253931884	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.0601054965432386	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.37	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0013031474413448749	0.0013034817415312264	1883848.6022304264	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	6.916523570277612E-10	5.859375E7	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	230.023100255649	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.1640010386527506	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	122.0703125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.25	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0013840243083759417	0.0013844011935764964	1774215.4745513492	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	7.801804015056249E-10	5.859375E7	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	216.5797586712815	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.071259843620758	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	122.0703125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.29	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0013817144620504958	0.0013820900807332945	1777181.4745513492	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	7.775780754631137E-10	5.859375E7	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	216.94187045178668	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.0698872813004985	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	122.0703125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.35	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0013600689384829737	0.0013604329504375433	3123642.477907312	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	4.354670069009219E-10	5.859375E7	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	220.3949679933745	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.057016487874011	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.39	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0013000944073505737	0.0013007574410438332	1633039.8808221682	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	7.960097670699568E-10	1.171875E8	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	230.5340672659155	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.1621601936437522	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.41	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			960	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0012958538590597858	0.0012961843975823697	1894454.3522304264	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	6.839308113307701E-10	5.859375E7	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	231.31793067240318	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.159351944931561	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	122.0703125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00342.S	ALMA	JAO	ALMA	uid://A001/X335d/X37c.source.J0607-0834.spw.43	cube	2		J0607-0834	91.99874682083548	-8.580549491672668	0.00718148541272227	Polygon ICRS 91.999650 -8.577072 92.000881 -8.577645 92.001813 -8.578625 92.002314 -8.579877 92.002378 -8.580549 92.002264 -8.581442 92.001929 -8.582279 92.001545 -8.582838 92.000496 -8.583696 91.999202 -8.584112 91.997844 -8.584027 91.996612 -8.583454 91.996100 -8.583008 91.995565 -8.582279 91.995144 -8.581000 91.995230 -8.579656 91.995461 -8.579021 91.995949 -8.578261 91.996997 -8.577403 91.998292 -8.576987			3840	1	2	1.027999806110033	60407.910626	60416.988903	725.76	725.76	0.0012816562736420048	0.0012920141684766757	237571.12977880333	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X335d/X37c	application/x-votable+xml; content=datalink		2022.1.00342.S	Public	215.75167716481315	-13.523809056184684	6	5.3940899507951025E-9	1.875E9	A001:DV12 A002:DA45 A003:DV07 A004:DA41 A006:DA59 A007:DV20 A008:DV17 A009:DV09 A010:DV06 A011:DV01 A013:DV18 A015:DA52 A016:DA44 A017:DV08 A019:DA57 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A027:DV03 A028:DA54 A030:DV22 A031:DA58 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A041:DA43 A042:DV04 A043:DV10 A044:DA46 A045:DA65 A047:DA42 A048:DA55 A049:DV13 A050:DA64 A058:DA63 A060:DV23 A062:DA56 A066:DA49 A068:DV21 A069:DA62 A072:DA61 A074:DV14 A082:DA58 A088:DA54	F	2025-10-31T06:27:52.000	1.027999806110033	[216.55..216.61GHz,122.07kHz,2.1mJy/beam@10km/s,727.3uJy/beam@native, XX YY] U [216.91..216.97GHz,122.07kHz,2.1mJy/beam@10km/s,727.4uJy/beam@native, XX YY] U [218.19..218.25GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [218.43..218.48GHz,122.07kHz,2.1mJy/beam@10km/s,727.9uJy/beam@native, XX YY] U [219.53..219.59GHz,70.56kHz,2.1mJy/beam@10km/s,728.3uJy/beam@native, XX YY] U [220.37..220.42GHz,70.56kHz,2.1mJy/beam@10km/s,728.6uJy/beam@native, XX YY] U [229.99..230.05GHz,122.07kHz,2.2mJy/beam@10km/s,783.1uJy/beam@native, XX YY] U [230.48..230.59GHz,141.11kHz,2.2mJy/beam@10km/s,553.9uJy/beam@native, XX YY] U [231.29..231.35GHz,122.07kHz,2.2mJy/beam@10km/s,783.6uJy/beam@native, XX YY] U [232.03..233.91GHz,976.56kHz,2.2mJy/beam@10km/s,138.6uJy/beam@native, XX YY]	232.97257406330885	95.97527889966662	ALMA						We propose to study the evolution of protostellar outflows and their impact on the dense circumstellar envelope using a sample of 78 low-mass protostars at various evolutionary stages in the Orion A cloud. We will conduct multi-line observations of the environment around these protostars that will allow us to trace the distribution of the outflowing gas (and its momentum and energy) with respect to the kinematics and structure of the infalling envelope. We will use the 12m array and ACA to obtain data with a resolution of 440 au and sensitive to structures extending out to 0.1 pc. Combining the proposed observations with radiative transfer models and MHD outflow simulations we aim to: 1) determine the importance of outflows in the removal of dense gas around protostars and its effect on the star formation efficiency; 2) establish how outflow and infall rates change over the lifetime of prototstars in order to understand their relative impact at different evolutionary stages on the core mass-loss process; and	HOPS-158_a_06_TM1	Tobin, John; Stephens, Ian; Mardones, Diego; Hsieh, Chenghan; Plunkett, Adele; Stutz, Amelia; Megeath, Tom; Hsu, Shih-Ying; Zhang, Yichen; Lee, Yueh-Ning; Álvarez-Gutiérrez, Rodrigo; Dunham, Michael; Lai, Shih-Ping; Maureira, Maria Jose; Kong, Shuo; Sheehan, Patrick; Pineda, Jaime; Sahu, Dipen; Yang, Yao-Lun; Offner, Stella; Li, Zhi-Yun; Liu, Sheng-Yuan;	2.1534860692524056	0.11963349456614726	2.3912816	uid://A001/X335d/X37b	uid://A001/X335d/X37c	uid://A002/X1158102/X15e63	Survey of Orion Protostellar Outflow-Envelope Interactions and Evolution	S	PHASE WVR	F	12.27119633675865	T		Outflows, jets and ionized winds;Low-mass star formation	ISM and star formation	harcealma	Arce, Hector	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.01528.S	ALMA	JAO	ALMA	uid://A001/X2f6/X418.source.UDS.0388.spw.19	image	2	ari_l	UDS.0388	34.24816666669578	-5.40854722222337	0.004702340442186642	Polygon ICRS 34.248315 -5.406201 34.249172 -5.406420 34.249888 -5.406938 34.250236 -5.407415 34.250413 -5.407821 34.250524 -5.408695 34.250413 -5.409274 34.250236 -5.409680 34.249672 -5.410359 34.248896 -5.410783 34.248018 -5.410894 34.247161 -5.410675 34.246445 -5.410157 34.246097 -5.409680 34.245921 -5.409274 34.245810 -5.408400 34.246030 -5.407546 34.246256 -5.407165 34.246661 -5.406736 34.247437 -5.406311			128	1	2	0.17689425449646595	57596.449613	57596.510826	40.32	40.32	8.819895401400332E-4	8.871690312147658E-4	10877.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2f6/X418	application/x-votable+xml; content=datalink		2015.1.01528.S	Public	169.9121406876789	-60.22504047464271	7	8.156411470952411E-8	2.0E9	A001:DA59 A002:DA49 A006:DA61 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A048:DV15 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A078:DV12 A079:DA64 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A134:DA44 A135:DV19 T701:PM03 T703:PM04 T704:PM01	F	2017-09-30T06:57:11.000	0.17689425449646595	[335.98..337.97GHz,31250.00kHz,7.1mJy/beam@10km/s,532.5uJy/beam@native, XX YY] U [337.92..339.90GHz,31250.00kHz,6.5mJy/beam@10km/s,486.5uJy/beam@native, XX YY] U [347.98..349.97GHz,31250.00kHz,6.9mJy/beam@10km/s,528.1uJy/beam@native, XX YY] U [349.98..351.97GHz,31250.00kHz,7.7mJy/beam@10km/s,592.7uJy/beam@native, XX YY]	338.91255702173265	26767.00116081351	ALMA	A machine-learning approach for identifying the counterparts of submillimetre galaxies and applications to the GOODS-North field An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Identifying Candidate z ∼ 4.5 [C II] Emitters An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Number Counts of Submillimeter Galaxies An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: The Far-infrared/Radio Correlation for High-redshift Dusty Star-forming Galaxies An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: halo masses for submillimetre galaxies An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: high-resolution dust continuum morphologies and the link between sub-millimetre galaxies and spheroid formation An ALMA survey of the SCUBA-2 Cosmology	Algera, H. S. B. An, Fang Xia Borsato, E. Chen, Chian-Chou Cheng, Cheng Cooke, E. A. Dudzevičiūtė, U. Gullberg, B. Koprowski, M. P. Lang, Philipp Liu, Ruihan Henry Scholtz, J. Schreiber, C. Smail, Ian Stach, S. M. Stach, Stuart M. Tan, Qing-Hua Zavala, J. A.	Algera, H. S. B.; Smail, I.; Dudzevičiūtė, U.; Swinbank, A. M.; Stach, S.; Hodge, J. A.; Thomson, A. P.; Almaini, O.; Arumugam, V.; Blain, A. W.; Calistro-Rivera, G.; Chapman, S. C.; Chen, C.-C.; da Cunha, E.; Farrah, D.; Leslie, S.; Scott, D.; van der Vlugt, D.; Wardlow, J. L.; van der Werf, P. An, Fang Xia; Simpson, J. M.; Smail, Ian; Swinbank, A. M.; Ma, Cong; Liu, Daizhong; Lang, P.; Schinnerer, E.; Karim, A.; Magnelli, B.; Leslie, S.; Bertoldi, F.; Chen, Chian-Chou; Geach, J. E.; Matsuda, Y.; Stach, S. M.; Wardlow, J. L.; Gullberg, B.; Ivison, R. J.; Ao, Y.; Coogan, R. T.; Thomson, A. P.; Chapman, S. C.; Wang, R.; Wang, Wei-Hao; Yang, Y.; Asquith, R.; Bourne, N.; Coppin, K.; Hine, N. K.; Ho, L. C.; Hwang, H. S.; Kato, Y.; Lacaille, K.; Lewis, A. J. R.; Oteo, I.; Scholtz, J.; Sawicki, M.; Smith, D. Borsato, E.; Marchetti, L.; Negrello, M.; Corsini, E. M.; Wake, D.; Amvrosiadis, A.; Baker, A. J.; Bakx, T. J. L. C.; Beelen, A.; Berta, S.; Beyer, A.; Clements, D. L.; Cooray, A.; Cox, P.; Dannerbauer, H.; de	As part of our KMOS AGN Survey at High-redshift (KASHz), we present spatially resolved VLT/KMOS and VLT/SINFONI spectroscopic data and ALMA 870 μm continuum imaging of eight z = 1.4-2.6 moderate AGN (L_{2-10 kev} = 10<SUP>42</SUP>-10<SUP>45</SUP> ergs s<SUP>-1</SUP>). We map [O III], H α and rest-frame FIR emission to search for any spatial anticorrelation between ionised outflows (traced by the [O III] line) and star formation (SF; traced by H α and FIR), that has previously been claimed for some high-z AGN and used as evidence for negative and/or positive AGN feedback. First, we conclude that H α is unreliable to map SF inside our AGN host galaxies based on: (i) SF rates inferred from attenuation-corrected H α can lie below those inferred from FIR; (ii) the FIR continuum is more compact than the H α emission by a factor of ̃2 on average; (iii) in half of our sample, we observe significant spatial offsets between the FIR and H α emission, with an average offset of 1.4 ± 0.6 kpc. Secondly, for the five target	2018	We propose ALMA band-7 continuum follow-up observations of an uniformly selected sample of 533 submillimeter sources with S850 > 3.5mJy from our SCUBA-2 survey of the UKIDSS-UDS. We expect to precisely locate almost 1000 SMGs with S850 > 1mJy. With this unprecedented large number of SMGs with precise positions, our science goals are to 1) measure the angular correlation function and so derive the halo mass, building the evolutionary links between SMGs and other high-z galaxy populations and their local desendants, 2) test whether brighter SMGs are more likely to break up into multiple faint components, and derive intrinsic number counts, 3) precisely identify the counterparts in other wavelengths and so derive redshift distributions, in particular the form of the high-z tail. With a sample of ~1000 ALMA SMGs (~10 times larger than that of previously samples such as ALESS), we will measure the multi-wavelength properties of the population, redshift distribution and most critically their clustering, allowing us	UDS.0018_a_07_TE	Geach, James; Blain, Andrew; Chapman, Scott; Swinbank, Mark; Dunlop, James; Coppin, Kristen; van der Werf, Paul; Ma, Cheng-Jiun; Farrah, Duncan; Ivison, Rob; Simpson, James; Michałowski, Michał; Scott, Douglas; Thomson, Alasdair; Chen, Chian-Chou;	6.470490967968323	0.26551052153798016	0.7633934	uid://A001/X2f6/X417	uid://A001/X2f6/X418	uid://A002/Xb5f503/X2b0b	AS2UDS : Clustering of ~1000 ALMA-identified submillimeter galaxies	S	TARGET	T	2.3306891796191014	T	2018A&A...618A..85S 2018ApJ...860..161S 2018ApJ...861..100C 2018ApJ...869...71Z 2019ApJ...879...54L 2019ApJ...886...48A 2019MNRAS.487.4648S 2019MNRAS.489.1770L 2019MNRAS.490.4956G 2020A&A...635A.119C 2020ApJ...903..138A 2020MNRAS.492.3194S 2020MNRAS.492.4927K 2020MNRAS.494.3828D 2021MNRAS.502.3426S 2021MNRAS.504..172S 2022ApJ...939L...7C 2023ApJ...942L..19C 2024MNRAS.528.6222B 2024Natur.636...69T	Starburst galaxies;Sub-mm Galaxies (SMG)	Active galaxies	irs	Smail, Ian	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.01528.S	ALMA	JAO	ALMA	uid://A001/X2f6/X418.source.UDS.0388.spw.17	image	2	ari_l	UDS.0388	34.24816666669578	-5.40854722222337	0.004702340442186642	Polygon ICRS 34.248315 -5.406201 34.249172 -5.406420 34.249888 -5.406938 34.250236 -5.407415 34.250413 -5.407821 34.250524 -5.408695 34.250413 -5.409274 34.250236 -5.409680 34.249672 -5.410359 34.248896 -5.410783 34.248018 -5.410894 34.247161 -5.410675 34.246445 -5.410157 34.246097 -5.409680 34.245921 -5.409274 34.245810 -5.408400 34.246030 -5.407546 34.246256 -5.407165 34.246661 -5.406736 34.247437 -5.406311			128	1	2	0.17689425449646595	57596.449613	57596.510826	40.32	40.32	8.870455213902494E-4	8.922847389059161E-4	10815.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2f6/X418	application/x-votable+xml; content=datalink		2015.1.01528.S	Public	169.9121406876789	-60.22504047464271	7	8.250470036959713E-8	2.0E9	A001:DA59 A002:DA49 A006:DA61 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A048:DV15 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A078:DV12 A079:DA64 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A134:DA44 A135:DV19 T701:PM03 T703:PM04 T704:PM01	F	2017-09-30T06:57:11.000	0.17689425449646595	[335.98..337.97GHz,31250.00kHz,7.1mJy/beam@10km/s,532.5uJy/beam@native, XX YY] U [337.92..339.90GHz,31250.00kHz,6.5mJy/beam@10km/s,486.5uJy/beam@native, XX YY] U [347.98..349.97GHz,31250.00kHz,6.9mJy/beam@10km/s,528.1uJy/beam@native, XX YY] U [349.98..351.97GHz,31250.00kHz,7.7mJy/beam@10km/s,592.7uJy/beam@native, XX YY]	336.9751685974561	26767.00116081351	ALMA	A machine-learning approach for identifying the counterparts of submillimetre galaxies and applications to the GOODS-North field An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Identifying Candidate z ∼ 4.5 [C II] Emitters An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Number Counts of Submillimeter Galaxies An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: The Far-infrared/Radio Correlation for High-redshift Dusty Star-forming Galaxies An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: halo masses for submillimetre galaxies An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: high-resolution dust continuum morphologies and the link between sub-millimetre galaxies and spheroid formation An ALMA survey of the SCUBA-2 Cosmology	Algera, H. S. B. An, Fang Xia Borsato, E. Chen, Chian-Chou Cheng, Cheng Cooke, E. A. Dudzevičiūtė, U. Gullberg, B. Koprowski, M. P. Lang, Philipp Liu, Ruihan Henry Scholtz, J. Schreiber, C. Smail, Ian Stach, S. M. Stach, Stuart M. Tan, Qing-Hua Zavala, J. A.	Algera, H. S. B.; Smail, I.; Dudzevičiūtė, U.; Swinbank, A. M.; Stach, S.; Hodge, J. A.; Thomson, A. P.; Almaini, O.; Arumugam, V.; Blain, A. W.; Calistro-Rivera, G.; Chapman, S. C.; Chen, C.-C.; da Cunha, E.; Farrah, D.; Leslie, S.; Scott, D.; van der Vlugt, D.; Wardlow, J. L.; van der Werf, P. An, Fang Xia; Simpson, J. M.; Smail, Ian; Swinbank, A. M.; Ma, Cong; Liu, Daizhong; Lang, P.; Schinnerer, E.; Karim, A.; Magnelli, B.; Leslie, S.; Bertoldi, F.; Chen, Chian-Chou; Geach, J. E.; Matsuda, Y.; Stach, S. M.; Wardlow, J. L.; Gullberg, B.; Ivison, R. J.; Ao, Y.; Coogan, R. T.; Thomson, A. P.; Chapman, S. C.; Wang, R.; Wang, Wei-Hao; Yang, Y.; Asquith, R.; Bourne, N.; Coppin, K.; Hine, N. K.; Ho, L. C.; Hwang, H. S.; Kato, Y.; Lacaille, K.; Lewis, A. J. R.; Oteo, I.; Scholtz, J.; Sawicki, M.; Smith, D. Borsato, E.; Marchetti, L.; Negrello, M.; Corsini, E. M.; Wake, D.; Amvrosiadis, A.; Baker, A. J.; Bakx, T. J. L. C.; Beelen, A.; Berta, S.; Beyer, A.; Clements, D. L.; Cooray, A.; Cox, P.; Dannerbauer, H.; de	As part of our KMOS AGN Survey at High-redshift (KASHz), we present spatially resolved VLT/KMOS and VLT/SINFONI spectroscopic data and ALMA 870 μm continuum imaging of eight z = 1.4-2.6 moderate AGN (L_{2-10 kev} = 10<SUP>42</SUP>-10<SUP>45</SUP> ergs s<SUP>-1</SUP>). We map [O III], H α and rest-frame FIR emission to search for any spatial anticorrelation between ionised outflows (traced by the [O III] line) and star formation (SF; traced by H α and FIR), that has previously been claimed for some high-z AGN and used as evidence for negative and/or positive AGN feedback. First, we conclude that H α is unreliable to map SF inside our AGN host galaxies based on: (i) SF rates inferred from attenuation-corrected H α can lie below those inferred from FIR; (ii) the FIR continuum is more compact than the H α emission by a factor of ̃2 on average; (iii) in half of our sample, we observe significant spatial offsets between the FIR and H α emission, with an average offset of 1.4 ± 0.6 kpc. Secondly, for the five target	2018	We propose ALMA band-7 continuum follow-up observations of an uniformly selected sample of 533 submillimeter sources with S850 > 3.5mJy from our SCUBA-2 survey of the UKIDSS-UDS. We expect to precisely locate almost 1000 SMGs with S850 > 1mJy. With this unprecedented large number of SMGs with precise positions, our science goals are to 1) measure the angular correlation function and so derive the halo mass, building the evolutionary links between SMGs and other high-z galaxy populations and their local desendants, 2) test whether brighter SMGs are more likely to break up into multiple faint components, and derive intrinsic number counts, 3) precisely identify the counterparts in other wavelengths and so derive redshift distributions, in particular the form of the high-z tail. With a sample of ~1000 ALMA SMGs (~10 times larger than that of previously samples such as ALESS), we will measure the multi-wavelength properties of the population, redshift distribution and most critically their clustering, allowing us	UDS.0018_a_07_TE	Geach, James; Blain, Andrew; Chapman, Scott; Swinbank, Mark; Dunlop, James; Coppin, Kristen; van der Werf, Paul; Ma, Cheng-Jiun; Farrah, Duncan; Ivison, Rob; Simpson, James; Michałowski, Michał; Scott, Douglas; Thomson, Alasdair; Chen, Chian-Chou;	7.102707718106846	0.26551052153798016	0.7633934	uid://A001/X2f6/X417	uid://A001/X2f6/X418	uid://A002/Xb5f503/X2b0b	AS2UDS : Clustering of ~1000 ALMA-identified submillimeter galaxies	S	TARGET	T	2.3306891796191014	T	2018A&A...618A..85S 2018ApJ...860..161S 2018ApJ...861..100C 2018ApJ...869...71Z 2019ApJ...879...54L 2019ApJ...886...48A 2019MNRAS.487.4648S 2019MNRAS.489.1770L 2019MNRAS.490.4956G 2020A&A...635A.119C 2020ApJ...903..138A 2020MNRAS.492.3194S 2020MNRAS.492.4927K 2020MNRAS.494.3828D 2021MNRAS.502.3426S 2021MNRAS.504..172S 2022ApJ...939L...7C 2023ApJ...942L..19C 2024MNRAS.528.6222B 2024Natur.636...69T	Starburst galaxies;Sub-mm Galaxies (SMG)	Active galaxies	irs	Smail, Ian	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.01528.S	ALMA	JAO	ALMA	uid://A001/X2f6/X418.source.UDS.0388.spw.23	image	2	ari_l	UDS.0388	34.24816666669578	-5.40854722222337	0.004702340442186642	Polygon ICRS 34.248315 -5.406201 34.249172 -5.406420 34.249888 -5.406938 34.250236 -5.407415 34.250413 -5.407821 34.250524 -5.408695 34.250413 -5.409274 34.250236 -5.409680 34.249672 -5.410359 34.248896 -5.410783 34.248018 -5.410894 34.247161 -5.410675 34.246445 -5.410157 34.246097 -5.409680 34.245921 -5.409274 34.245810 -5.408400 34.246030 -5.407546 34.246256 -5.407165 34.246661 -5.406736 34.247437 -5.406311			128	1	2	0.17689425449646595	57596.449613	57596.510826	40.32	40.32	8.517639749728228E-4	8.565935928142831E-4	11200.0764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2f6/X418	application/x-votable+xml; content=datalink		2015.1.01528.S	Public	169.9121406876789	-60.22504047464271	7	7.605423603082118E-8	2.0E9	A001:DA59 A002:DA49 A006:DA61 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A048:DV15 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A078:DV12 A079:DA64 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A134:DA44 A135:DV19 T701:PM03 T703:PM04 T704:PM01	F	2017-09-30T06:57:11.000	0.17689425449646595	[335.98..337.97GHz,31250.00kHz,7.1mJy/beam@10km/s,532.5uJy/beam@native, XX YY] U [337.92..339.90GHz,31250.00kHz,6.5mJy/beam@10km/s,486.5uJy/beam@native, XX YY] U [347.98..349.97GHz,31250.00kHz,6.9mJy/beam@10km/s,528.1uJy/beam@native, XX YY] U [349.98..351.97GHz,31250.00kHz,7.7mJy/beam@10km/s,592.7uJy/beam@native, XX YY]	350.9743623728741	26767.00116081351	ALMA	A machine-learning approach for identifying the counterparts of submillimetre galaxies and applications to the GOODS-North field An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Identifying Candidate z ∼ 4.5 [C II] Emitters An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Number Counts of Submillimeter Galaxies An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: The Far-infrared/Radio Correlation for High-redshift Dusty Star-forming Galaxies An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: halo masses for submillimetre galaxies An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: high-resolution dust continuum morphologies and the link between sub-millimetre galaxies and spheroid formation An ALMA survey of the SCUBA-2 Cosmology	Algera, H. S. B. An, Fang Xia Borsato, E. Chen, Chian-Chou Cheng, Cheng Cooke, E. A. Dudzevičiūtė, U. Gullberg, B. Koprowski, M. P. Lang, Philipp Liu, Ruihan Henry Scholtz, J. Schreiber, C. Smail, Ian Stach, S. M. Stach, Stuart M. Tan, Qing-Hua Zavala, J. A.	Algera, H. S. B.; Smail, I.; Dudzevičiūtė, U.; Swinbank, A. M.; Stach, S.; Hodge, J. A.; Thomson, A. P.; Almaini, O.; Arumugam, V.; Blain, A. W.; Calistro-Rivera, G.; Chapman, S. C.; Chen, C.-C.; da Cunha, E.; Farrah, D.; Leslie, S.; Scott, D.; van der Vlugt, D.; Wardlow, J. L.; van der Werf, P. An, Fang Xia; Simpson, J. M.; Smail, Ian; Swinbank, A. M.; Ma, Cong; Liu, Daizhong; Lang, P.; Schinnerer, E.; Karim, A.; Magnelli, B.; Leslie, S.; Bertoldi, F.; Chen, Chian-Chou; Geach, J. E.; Matsuda, Y.; Stach, S. M.; Wardlow, J. L.; Gullberg, B.; Ivison, R. J.; Ao, Y.; Coogan, R. T.; Thomson, A. P.; Chapman, S. C.; Wang, R.; Wang, Wei-Hao; Yang, Y.; Asquith, R.; Bourne, N.; Coppin, K.; Hine, N. K.; Ho, L. C.; Hwang, H. S.; Kato, Y.; Lacaille, K.; Lewis, A. J. R.; Oteo, I.; Scholtz, J.; Sawicki, M.; Smith, D. Borsato, E.; Marchetti, L.; Negrello, M.; Corsini, E. M.; Wake, D.; Amvrosiadis, A.; Baker, A. J.; Bakx, T. J. L. C.; Beelen, A.; Berta, S.; Beyer, A.; Clements, D. L.; Cooray, A.; Cox, P.; Dannerbauer, H.; de	As part of our KMOS AGN Survey at High-redshift (KASHz), we present spatially resolved VLT/KMOS and VLT/SINFONI spectroscopic data and ALMA 870 μm continuum imaging of eight z = 1.4-2.6 moderate AGN (L_{2-10 kev} = 10<SUP>42</SUP>-10<SUP>45</SUP> ergs s<SUP>-1</SUP>). We map [O III], H α and rest-frame FIR emission to search for any spatial anticorrelation between ionised outflows (traced by the [O III] line) and star formation (SF; traced by H α and FIR), that has previously been claimed for some high-z AGN and used as evidence for negative and/or positive AGN feedback. First, we conclude that H α is unreliable to map SF inside our AGN host galaxies based on: (i) SF rates inferred from attenuation-corrected H α can lie below those inferred from FIR; (ii) the FIR continuum is more compact than the H α emission by a factor of ̃2 on average; (iii) in half of our sample, we observe significant spatial offsets between the FIR and H α emission, with an average offset of 1.4 ± 0.6 kpc. Secondly, for the five target	2018	We propose ALMA band-7 continuum follow-up observations of an uniformly selected sample of 533 submillimeter sources with S850 > 3.5mJy from our SCUBA-2 survey of the UKIDSS-UDS. We expect to precisely locate almost 1000 SMGs with S850 > 1mJy. With this unprecedented large number of SMGs with precise positions, our science goals are to 1) measure the angular correlation function and so derive the halo mass, building the evolutionary links between SMGs and other high-z galaxy populations and their local desendants, 2) test whether brighter SMGs are more likely to break up into multiple faint components, and derive intrinsic number counts, 3) precisely identify the counterparts in other wavelengths and so derive redshift distributions, in particular the form of the high-z tail. With a sample of ~1000 ALMA SMGs (~10 times larger than that of previously samples such as ALESS), we will measure the multi-wavelength properties of the population, redshift distribution and most critically their clustering, allowing us	UDS.0018_a_07_TE	Geach, James; Blain, Andrew; Chapman, Scott; Swinbank, Mark; Dunlop, James; Coppin, Kristen; van der Werf, Paul; Ma, Cheng-Jiun; Farrah, Duncan; Ivison, Rob; Simpson, James; Michałowski, Michał; Scott, Douglas; Thomson, Alasdair; Chen, Chian-Chou;	7.747219165573677	0.26551052153798016	0.7633934	uid://A001/X2f6/X417	uid://A001/X2f6/X418	uid://A002/Xb5f503/X2b0b	AS2UDS : Clustering of ~1000 ALMA-identified submillimeter galaxies	S	TARGET	T	2.3306891796191014	T	2018A&A...618A..85S 2018ApJ...860..161S 2018ApJ...861..100C 2018ApJ...869...71Z 2019ApJ...879...54L 2019ApJ...886...48A 2019MNRAS.487.4648S 2019MNRAS.489.1770L 2019MNRAS.490.4956G 2020A&A...635A.119C 2020ApJ...903..138A 2020MNRAS.492.3194S 2020MNRAS.492.4927K 2020MNRAS.494.3828D 2021MNRAS.502.3426S 2021MNRAS.504..172S 2022ApJ...939L...7C 2023ApJ...942L..19C 2024MNRAS.528.6222B 2024Natur.636...69T	Starburst galaxies;Sub-mm Galaxies (SMG)	Active galaxies	irs	Smail, Ian	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.01528.S	ALMA	JAO	ALMA	uid://A001/X2f6/X418.source.UDS.0388.spw.21	image	2	ari_l	UDS.0388	34.24816666669578	-5.40854722222337	0.004702340442186642	Polygon ICRS 34.248315 -5.406201 34.249172 -5.406420 34.249888 -5.406938 34.250236 -5.407415 34.250413 -5.407821 34.250524 -5.408695 34.250413 -5.409274 34.250236 -5.409680 34.249672 -5.410359 34.248896 -5.410783 34.248018 -5.410894 34.247161 -5.410675 34.246445 -5.410157 34.246097 -5.409680 34.245921 -5.409274 34.245810 -5.408400 34.246030 -5.407546 34.246256 -5.407165 34.246661 -5.406736 34.247437 -5.406311			128	1	2	0.17689425449646595	57596.449613	57596.510826	40.32	40.32	8.566313817792322E-4	8.615165107227948E-4	11136.0764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2f6/X418	application/x-votable+xml; content=datalink		2015.1.01528.S	Public	169.9121406876789	-60.22504047464271	7	7.692843616813177E-8	2.0E9	A001:DA59 A002:DA49 A006:DA61 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A048:DV15 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A078:DV12 A079:DA64 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A134:DA44 A135:DV19 T701:PM03 T703:PM04 T704:PM01	F	2017-09-30T06:57:11.000	0.17689425449646595	[335.98..337.97GHz,31250.00kHz,7.1mJy/beam@10km/s,532.5uJy/beam@native, XX YY] U [337.92..339.90GHz,31250.00kHz,6.5mJy/beam@10km/s,486.5uJy/beam@native, XX YY] U [347.98..349.97GHz,31250.00kHz,6.9mJy/beam@10km/s,528.1uJy/beam@native, XX YY] U [349.98..351.97GHz,31250.00kHz,7.7mJy/beam@10km/s,592.7uJy/beam@native, XX YY]	348.97447754781433	26767.00116081351	ALMA	A machine-learning approach for identifying the counterparts of submillimetre galaxies and applications to the GOODS-North field An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Identifying Candidate z ∼ 4.5 [C II] Emitters An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: Number Counts of Submillimeter Galaxies An ALMA Survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS Field: The Far-infrared/Radio Correlation for High-redshift Dusty Star-forming Galaxies An ALMA survey of the S2CLS UDS field: optically invisible submillimetre galaxies An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: halo masses for submillimetre galaxies An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: high-resolution dust continuum morphologies and the link between sub-millimetre galaxies and spheroid formation An ALMA survey of the SCUBA-2 Cosmology	Algera, H. S. B. An, Fang Xia Borsato, E. Chen, Chian-Chou Cheng, Cheng Cooke, E. A. Dudzevičiūtė, U. Gullberg, B. Koprowski, M. P. Lang, Philipp Liu, Ruihan Henry Scholtz, J. Schreiber, C. Smail, Ian Stach, S. M. Stach, Stuart M. Tan, Qing-Hua Zavala, J. A.	Algera, H. S. B.; Smail, I.; Dudzevičiūtė, U.; Swinbank, A. M.; Stach, S.; Hodge, J. A.; Thomson, A. P.; Almaini, O.; Arumugam, V.; Blain, A. W.; Calistro-Rivera, G.; Chapman, S. C.; Chen, C.-C.; da Cunha, E.; Farrah, D.; Leslie, S.; Scott, D.; van der Vlugt, D.; Wardlow, J. L.; van der Werf, P. An, Fang Xia; Simpson, J. M.; Smail, Ian; Swinbank, A. M.; Ma, Cong; Liu, Daizhong; Lang, P.; Schinnerer, E.; Karim, A.; Magnelli, B.; Leslie, S.; Bertoldi, F.; Chen, Chian-Chou; Geach, J. E.; Matsuda, Y.; Stach, S. M.; Wardlow, J. L.; Gullberg, B.; Ivison, R. J.; Ao, Y.; Coogan, R. T.; Thomson, A. P.; Chapman, S. C.; Wang, R.; Wang, Wei-Hao; Yang, Y.; Asquith, R.; Bourne, N.; Coppin, K.; Hine, N. K.; Ho, L. C.; Hwang, H. S.; Kato, Y.; Lacaille, K.; Lewis, A. J. R.; Oteo, I.; Scholtz, J.; Sawicki, M.; Smith, D. Borsato, E.; Marchetti, L.; Negrello, M.; Corsini, E. M.; Wake, D.; Amvrosiadis, A.; Baker, A. J.; Bakx, T. J. L. C.; Beelen, A.; Berta, S.; Beyer, A.; Clements, D. L.; Cooray, A.; Cox, P.; Dannerbauer, H.; de	As part of our KMOS AGN Survey at High-redshift (KASHz), we present spatially resolved VLT/KMOS and VLT/SINFONI spectroscopic data and ALMA 870 μm continuum imaging of eight z = 1.4-2.6 moderate AGN (L_{2-10 kev} = 10<SUP>42</SUP>-10<SUP>45</SUP> ergs s<SUP>-1</SUP>). We map [O III], H α and rest-frame FIR emission to search for any spatial anticorrelation between ionised outflows (traced by the [O III] line) and star formation (SF; traced by H α and FIR), that has previously been claimed for some high-z AGN and used as evidence for negative and/or positive AGN feedback. First, we conclude that H α is unreliable to map SF inside our AGN host galaxies based on: (i) SF rates inferred from attenuation-corrected H α can lie below those inferred from FIR; (ii) the FIR continuum is more compact than the H α emission by a factor of ̃2 on average; (iii) in half of our sample, we observe significant spatial offsets between the FIR and H α emission, with an average offset of 1.4 ± 0.6 kpc. Secondly, for the five target	2018	We propose ALMA band-7 continuum follow-up observations of an uniformly selected sample of 533 submillimeter sources with S850 > 3.5mJy from our SCUBA-2 survey of the UKIDSS-UDS. We expect to precisely locate almost 1000 SMGs with S850 > 1mJy. With this unprecedented large number of SMGs with precise positions, our science goals are to 1) measure the angular correlation function and so derive the halo mass, building the evolutionary links between SMGs and other high-z galaxy populations and their local desendants, 2) test whether brighter SMGs are more likely to break up into multiple faint components, and derive intrinsic number counts, 3) precisely identify the counterparts in other wavelengths and so derive redshift distributions, in particular the form of the high-z tail. With a sample of ~1000 ALMA SMGs (~10 times larger than that of previously samples such as ALESS), we will measure the multi-wavelength properties of the population, redshift distribution and most critically their clustering, allowing us	UDS.0018_a_07_TE	Geach, James; Blain, Andrew; Chapman, Scott; Swinbank, Mark; Dunlop, James; Coppin, Kristen; van der Werf, Paul; Ma, Cheng-Jiun; Farrah, Duncan; Ivison, Rob; Simpson, James; Michałowski, Michał; Scott, Douglas; Thomson, Alasdair; Chen, Chian-Chou;	6.92156196139877	0.26551052153798016	0.7633934	uid://A001/X2f6/X417	uid://A001/X2f6/X418	uid://A002/Xb5f503/X2b0b	AS2UDS : Clustering of ~1000 ALMA-identified submillimeter galaxies	S	TARGET	T	2.3306891796191014	T	2018A&A...618A..85S 2018ApJ...860..161S 2018ApJ...861..100C 2018ApJ...869...71Z 2019ApJ...879...54L 2019ApJ...886...48A 2019MNRAS.487.4648S 2019MNRAS.489.1770L 2019MNRAS.490.4956G 2020A&A...635A.119C 2020ApJ...903..138A 2020MNRAS.492.3194S 2020MNRAS.492.4927K 2020MNRAS.494.3828D 2021MNRAS.502.3426S 2021MNRAS.504..172S 2022ApJ...939L...7C 2023ApJ...942L..19C 2024MNRAS.528.6222B 2024Natur.636...69T	Starburst galaxies;Sub-mm Galaxies (SMG)	Active galaxies	irs	Smail, Ian	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.01778.S	ALMA	JAO	ALMA	uid://A001/X2d20/Xcd.source.J0725-0054.spw.8	image	2		J0725-0054	111.46099963300868	-0.9157063694439987	0.02843808513274785	Circle ICRS 111.461000 -0.915706 0.014219			128	1	2	13.078872320783873	59951.216444	59951.223449	604.8	604.8	0.0028960513342127154	0.0029526544977166312	3248.9219389616437	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/Xcd	application/x-votable+xml; content=datalink		2022.1.01778.S	Public	217.69712429289962	7.227169550893133	3	8.913498706976127E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J506:CM05 N601:CM07 N603:CM09 N605:CM04 N606:CM06	F	2024-01-12T15:35:07.000	13.078872320783873	[89.53..91.52GHz,31250.00kHz,13.4mJy/beam@10km/s,522.5uJy/beam@native, XX YY] U [91.43..93.41GHz,31250.00kHz,13.2mJy/beam@10km/s,519.2uJy/beam@native, XX YY] U [101.53..103.52GHz,31250.00kHz,13.1mJy/beam@10km/s,543.7uJy/beam@native, XX YY] U [103.49..105.48GHz,31250.00kHz,13.2mJy/beam@10km/s,549.1uJy/beam@native, XX YY]	102.5254298319166	90528.58290691503	ALMA						The horizon-scale observations of M87 are well modelled by synchrotron emission from a thermal particle distribution function [eDF]. However on larger scale the observed spectra is in good agreement with a non-thermal eDF. Thus the question arises where and how the thermal particles are accelerated into the non-thermal distribution. For studying and addressing these questions simultaneous multi-frequency observations are crucial. We thus request Bands 3, 6 and 9 ACA observations of 73 nearby AGNs. The millimetre spectra will allow us to test different accretion models and thus test the opacity of the flows. The high-frequency capabilities of the ACA will allow us to study the turnover-regime of the spectrum (transition between optically thick and thin emission). Thus capturing the spectral turnover position will not only provide a tight constraint on the particle distribution function (and possible acceleration mechanism) but will also allow us to estimate the contribution to the high-energy emission via the	J081022._a_03_7M	Marrone, Dan; Fromm, Christian; Olivares Sanchez, Hector; Nagar, Neil; Chan, Chi-kwan;	13.148817673308033	0.26657312417360157	5.186	uid://A001/X2d20/Xcc	uid://A001/X2d20/Xcd	uid://A002/X101c3b2/X25a1	Constraining the Accretion Properties of Nearby High-mass AGNs	S	BANDPASS FLUX WVR	F	70.153594966021	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Galactic centres/nuclei	Active galaxies	venkatessh	Ramakrishnan, Venkatessh	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.01778.S	ALMA	JAO	ALMA	uid://A001/X2d20/Xcd.source.J0725-0054.spw.10	image	2		J0725-0054	111.46099963300868	-0.9157063694439987	0.02843808513274785	Circle ICRS 111.461000 -0.915706 0.014219			128	1	2	13.078872320783873	59951.216444	59951.223449	604.8	604.8	0.0028422881335761524	0.0028967894316910556	3311.5779389616437	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/Xcd	application/x-votable+xml; content=datalink		2022.1.01778.S	Public	217.69712429289962	7.227169550893133	3	8.582510591339966E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J506:CM05 N601:CM07 N603:CM09 N605:CM04 N606:CM06	F	2024-01-12T15:35:07.000	13.078872320783873	[89.53..91.52GHz,31250.00kHz,13.4mJy/beam@10km/s,522.5uJy/beam@native, XX YY] U [91.43..93.41GHz,31250.00kHz,13.2mJy/beam@10km/s,519.2uJy/beam@native, XX YY] U [101.53..103.52GHz,31250.00kHz,13.1mJy/beam@10km/s,543.7uJy/beam@native, XX YY] U [103.49..105.48GHz,31250.00kHz,13.2mJy/beam@10km/s,549.1uJy/beam@native, XX YY]	104.48351447160834	90528.58290691503	ALMA						The horizon-scale observations of M87 are well modelled by synchrotron emission from a thermal particle distribution function [eDF]. However on larger scale the observed spectra is in good agreement with a non-thermal eDF. Thus the question arises where and how the thermal particles are accelerated into the non-thermal distribution. For studying and addressing these questions simultaneous multi-frequency observations are crucial. We thus request Bands 3, 6 and 9 ACA observations of 73 nearby AGNs. The millimetre spectra will allow us to test different accretion models and thus test the opacity of the flows. The high-frequency capabilities of the ACA will allow us to study the turnover-regime of the spectrum (transition between optically thick and thin emission). Thus capturing the spectral turnover position will not only provide a tight constraint on the particle distribution function (and possible acceleration mechanism) but will also allow us to estimate the contribution to the high-energy emission via the	J081022._a_03_7M	Marrone, Dan; Fromm, Christian; Olivares Sanchez, Hector; Nagar, Neil; Chan, Chi-kwan;	13.152958001937051	0.26657312417360157	5.186	uid://A001/X2d20/Xcc	uid://A001/X2d20/Xcd	uid://A002/X101c3b2/X25a1	Constraining the Accretion Properties of Nearby High-mass AGNs	S	BANDPASS FLUX WVR	F	70.153594966021	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Galactic centres/nuclei	Active galaxies	venkatessh	Ramakrishnan, Venkatessh	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.01778.S	ALMA	JAO	ALMA	uid://A001/X2d20/Xcd.source.J0725-0054.spw.4	image	2		J0725-0054	111.46099963300868	-0.9157063694439987	0.02843808513274785	Circle ICRS 111.461000 -0.915706 0.014219			128	1	2	13.078872320783873	59951.216444	59951.223449	604.8	604.8	0.003275806484132567	0.0033484135943125525	2928.422061031956	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/Xcd	application/x-votable+xml; content=datalink		2022.1.01778.S	Public	217.69712429289962	7.227169550893133	3	1.143369632797631E-6	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J506:CM05 N601:CM07 N603:CM09 N605:CM04 N606:CM06	F	2024-01-12T15:35:07.000	13.078872320783873	[89.53..91.52GHz,31250.00kHz,13.4mJy/beam@10km/s,522.5uJy/beam@native, XX YY] U [91.43..93.41GHz,31250.00kHz,13.2mJy/beam@10km/s,519.2uJy/beam@native, XX YY] U [101.53..103.52GHz,31250.00kHz,13.1mJy/beam@10km/s,543.7uJy/beam@native, XX YY] U [103.49..105.48GHz,31250.00kHz,13.2mJy/beam@10km/s,549.1uJy/beam@native, XX YY]	90.52491491526646	90528.58290691503	ALMA						The horizon-scale observations of M87 are well modelled by synchrotron emission from a thermal particle distribution function [eDF]. However on larger scale the observed spectra is in good agreement with a non-thermal eDF. Thus the question arises where and how the thermal particles are accelerated into the non-thermal distribution. For studying and addressing these questions simultaneous multi-frequency observations are crucial. We thus request Bands 3, 6 and 9 ACA observations of 73 nearby AGNs. The millimetre spectra will allow us to test different accretion models and thus test the opacity of the flows. The high-frequency capabilities of the ACA will allow us to study the turnover-regime of the spectrum (transition between optically thick and thin emission). Thus capturing the spectral turnover position will not only provide a tight constraint on the particle distribution function (and possible acceleration mechanism) but will also allow us to estimate the contribution to the high-energy emission via the	J081022._a_03_7M	Marrone, Dan; Fromm, Christian; Olivares Sanchez, Hector; Nagar, Neil; Chan, Chi-kwan;	13.447908628503301	0.26657312417360157	5.186	uid://A001/X2d20/Xcc	uid://A001/X2d20/Xcd	uid://A002/X101c3b2/X25a1	Constraining the Accretion Properties of Nearby High-mass AGNs	S	BANDPASS FLUX WVR	F	70.153594966021	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Galactic centres/nuclei	Active galaxies	venkatessh	Ramakrishnan, Venkatessh	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.01778.S	ALMA	JAO	ALMA	uid://A001/X2d20/Xcd.source.J0725-0054.spw.6	image	2		J0725-0054	111.46099963300868	-0.9157063694439987	0.02843808513274785	Circle ICRS 111.461000 -0.915706 0.014219			128	1	2	13.078872320783873	59951.216444	59951.223449	604.8	604.8	0.0032093320348058913	0.0032789909466375894	2989.078061031956	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/Xcd	application/x-votable+xml; content=datalink		2022.1.01778.S	Public	217.69712429289962	7.227169550893133	3	1.0969433192514751E-6	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J506:CM05 N601:CM07 N603:CM09 N605:CM04 N606:CM06	F	2024-01-12T15:35:07.000	13.078872320783873	[89.53..91.52GHz,31250.00kHz,13.4mJy/beam@10km/s,522.5uJy/beam@native, XX YY] U [91.43..93.41GHz,31250.00kHz,13.2mJy/beam@10km/s,519.2uJy/beam@native, XX YY] U [101.53..103.52GHz,31250.00kHz,13.1mJy/beam@10km/s,543.7uJy/beam@native, XX YY] U [103.49..105.48GHz,31250.00kHz,13.2mJy/beam@10km/s,549.1uJy/beam@native, XX YY]	92.4204968532316	90528.58290691503	ALMA						The horizon-scale observations of M87 are well modelled by synchrotron emission from a thermal particle distribution function [eDF]. However on larger scale the observed spectra is in good agreement with a non-thermal eDF. Thus the question arises where and how the thermal particles are accelerated into the non-thermal distribution. For studying and addressing these questions simultaneous multi-frequency observations are crucial. We thus request Bands 3, 6 and 9 ACA observations of 73 nearby AGNs. The millimetre spectra will allow us to test different accretion models and thus test the opacity of the flows. The high-frequency capabilities of the ACA will allow us to study the turnover-regime of the spectrum (transition between optically thick and thin emission). Thus capturing the spectral turnover position will not only provide a tight constraint on the particle distribution function (and possible acceleration mechanism) but will also allow us to estimate the contribution to the high-energy emission via the	J081022._a_03_7M	Marrone, Dan; Fromm, Christian; Olivares Sanchez, Hector; Nagar, Neil; Chan, Chi-kwan;	13.223262192508543	0.26657312417360157	5.186	uid://A001/X2d20/Xcc	uid://A001/X2d20/Xcd	uid://A002/X101c3b2/X25a1	Constraining the Accretion Properties of Nearby High-mass AGNs	S	BANDPASS FLUX WVR	F	70.153594966021	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Galactic centres/nuclei	Active galaxies	venkatessh	Ramakrishnan, Venkatessh	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.1.00460.S	ALMA	JAO	ALMA	uid://A001/X126d/X104.source.IRAS_04302+2247.spw.23	image	2	ari_l	IRAS_04302+2247	68.31874999995279	22.889000000008497	0.011156098900091987	Circle ICRS 68.318750 22.889000 0.005578			128	1	2	0.05439461068023409	58023.287185	58023.292914	362.88	362.88	0.0019597037558174817	0.0019854569058493005	4832.0764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X126d/X104	application/x-votable+xml; content=datalink		2016.1.00460.S	Public	175.3349361852637	-16.710053471499975	4	4.0558343484563976E-7	2.0E9	A007:DV09 A015:DA61 A027:DV06 A074:DA47 A087:DV25 A090:DV24 A091:DA45 A092:DV14 A093:DV20 A096:PM01 A104:DA58 A105:DV02 A108:DA50 A110:DA41 A111:PM02 A115:DA43 A116:DV07 A118:DV01 A120:DA44 A121:DA55 A122:DV11 A123:DA42 A124:DA51 A126:DV10 A127:DA49 A128:DV13 A129:DA46 A130:DV15 A131:PM03 A132:DV23 A133:PM04 A135:DA57 P401:DA65 P409:DV04 P410:DA64 S301:DA60 S303:DA63 S307:DV05 S309:DA56 W202:DA54 W207:DV17 W209:DA48 W210:DV22	F	2018-12-19T17:19:01.000	0.05439461068023409	[136.99..138.98GHz,31250.00kHz,1.3mJy/beam@10km/s,63uJy/beam@native, XX YY] U [138.93..140.92GHz,31250.00kHz,1.2mJy/beam@10km/s,59.6uJy/beam@native, XX YY] U [148.99..150.98GHz,31250.00kHz,1.3mJy/beam@10km/s,64.7uJy/beam@native, XX YY] U [150.99..152.98GHz,31250.00kHz,1.4mJy/beam@10km/s,69.3uJy/beam@native, XX YY]	151.9863240026164	62042.1601777654	ALMA	Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 - a testbed for binary-disc interaction Edge-On Disk Study (EODS): II. HCO<SUP>+</SUP> and CO vertical stratification in the disk surrounding SSTTau042021 Masses and Implications for Ages of Low-mass Pre-main-sequence Stars in Taurus and Ophiuchus Modest Dust Settling in the IRAS04302+2247 Class I Protoplanetary Disk Observations of edge-on protoplanetary disks with ALMA. I. Results from continuum data Observations of highly inclined disks with ALMA: Results from <SUP>12</SUP>CO gas and continuum observations Observations of pre- and proto-brown dwarfs in nearby clouds: Paving the way to further constraining theories of brown dwarf formation The edge-on protoplanetary disk HH 48 NE. I. Modeling the geometry and stellar parameters Turbulence in protoplanetary disks: A systematic analysis of dust settling in 33 disks	Foucher, C. Martinien, L. Palau, Aina Ragusa, Enrico Simon, M. Sturm, J. A. Villenave, M. Villenave, Marion	Foucher, C.; Dutrey, A.; Piétu, V.; Guilloteau, S.; Chapillon, E.; Denis-Alpizar, O.; Dartois, E.; Di Folco, E.; Gavino, S.; Gorti, U.; Henning, Th.; Kóspál, Á.; Le Petit, F.; Majumdar, L.; Meshaka, R.; Phuong, N. T.; Ruaud, M.; Semenov, D.; Tang, Y. W.; Wolf, S. Martinien, L.; Duchêne, G.; Ribas, Á.; Villenave, M.; Ménard, F.; Stapelfeldt, K. R.; Pinte, C. Palau, Aina; Huélamo, Nuria; Barrado, David; Dunham, Michael M.; Lee, Chang Won Ragusa, Enrico; Fasano, Daniele; Toci, Claudia; Duchêne, Gaspard; Cuello, Nicolás; Villenave, Marion; van der Plas, Gerrit; Lodato, Giuseppe; Ménard, François; Price, Daniel J.; Pinte, Christophe; Stapelfeldt, Karl; Wolff, Schuyler Simon, M.; Guilloteau, S.; Beck, Tracy L.; Chapillon, E.; Di Folco, E.; Dutrey, A.; Feiden, Gregory A.; Grosso, N.; Piétu, V.; Prato, L.; Schaefer, Gail H. Sturm, J. A.; McClure, M. K.; Law, C. J.; Harsono, D.; Bergner, J. B.; Dartois, E.; Drozdovskaya, M. N.; Ioppolo, S.; Öberg, K. I.; Palumbo, M. E.; Pendleton, Y. J.; Rocha, W. R. M.; Terada, H.; U	<BR /> Aims: We aim to study vertical settling and radial drift of dust in protoplanetary disks from a different perspective: an edge-on view. An estimation of the amplitude of settling and drift is highly relevant to understanding planet formation. <BR /> Methods: We analyze a sample of 12 HST-selected edge-on protoplanetary disks (i.e., seen with high inclinations) for which the vertical extent of the emission layers can be constrained directly. We present ALMA high angular resolution continuum images (~0.1'') of these disks at two wavelengths, 0.89 and 2.06 mm (respectively ALMA bands 7 and 4), supplemented with archival band 6 data (1.33 mm) where available. <BR /> Results: Several sources show constant brightness profiles along their major axis with a steep drop at the outer edges. Two disks have central holes with additional compact continuum emission at the location of the central star. For most sources, the millimeter continuum emission is more compact than the scattered light, both in the vertical an	2019	We propose to observe a well-defined sample of Edge-On Disks to study the radial and vertical distribution of the dust. Scattered light images of edge-on disks like HH 30 have established what we think is typical for the shape and flaring of protoplanetary disks. However, these conclusions are correct only for the small grains, i.e. the near-IR scattering opacity carriers, but are very likely incorrect for the larger dust particles emitting at longer wavelengths. The large particles are expected to be distributed differently in particular because of dust settling, but so far we are still missing direct images that would reveal the vertical stratification of dust of all sizes in T Tauri disks. ALMA cycle-4 offers the perfect opportunity (resolution, sensitivity), and the edge-on geometry allows for direct conclusions beyond doubt. By comparing the gas distribution to the distributions of small and large dust grains, we can draw definite conclusions about the disk shape, and the settling and radial migration of	HK_Tau_B_a_04_TM1	Stapelfeldt, Karl; Louvet, Fabien; Padgett, Deborah; Dent, Bill; Benisty, Myriam; Dougados, Catherine; Pinte, Christophe; Chripko, Svenya; Duchene, Gaspard; Perrin, Marshall; Hales, Antonio; Wolff, Schuyler;	1.3763225720878656	0.031933735311887014	1.3846008	uid://A001/X87d/Xa3d	uid://A001/X126d/X104	uid://A002/Xc4d618/X6812	Measuring vertical settling and radial drift of dust: A survey of young edge-on disks	S	TARGET	T	1.1287170476360884	F	2019ApJ...884...42S 2020A&A...642A.164V 2021MNRAS.507.1157R 2023A&A...677A..17S 2023ApJ...946...70V 2024NewAR..9901711P 2025A&A...697A..64V 2025A&A...704A..32F 2026A&A...710A.140M	Disks around low-mass stars;null	Disks and planet formation	fmenard	Menard, Francois	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.1.00460.S	ALMA	JAO	ALMA	uid://A001/X126d/X104.source.IRAS_04302+2247.spw.17	image	2	ari_l	IRAS_04302+2247	68.31874999995279	22.889000000008497	0.011156098900091987	Circle ICRS 68.318750 22.889000 0.005578			128	1	2	0.05439461068023409	58023.287185	58023.292914	362.88	362.88	0.002157102789278994	0.002188346776523198	4447.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X126d/X104	application/x-votable+xml; content=datalink		2016.1.00460.S	Public	175.3349361852637	-16.710053471499975	4	4.92058006462162E-7	2.0E9	A007:DV09 A015:DA61 A027:DV06 A074:DA47 A087:DV25 A090:DV24 A091:DA45 A092:DV14 A093:DV20 A096:PM01 A104:DA58 A105:DV02 A108:DA50 A110:DA41 A111:PM02 A115:DA43 A116:DV07 A118:DV01 A120:DA44 A121:DA55 A122:DV11 A123:DA42 A124:DA51 A126:DV10 A127:DA49 A128:DV13 A129:DA46 A130:DV15 A131:PM03 A132:DV23 A133:PM04 A135:DA57 P401:DA65 P409:DV04 P410:DA64 S301:DA60 S303:DA63 S307:DV05 S309:DA56 W202:DA54 W207:DV17 W209:DA48 W210:DV22	F	2018-12-19T17:19:01.000	0.05439461068023409	[136.99..138.98GHz,31250.00kHz,1.3mJy/beam@10km/s,63uJy/beam@native, XX YY] U [138.93..140.92GHz,31250.00kHz,1.2mJy/beam@10km/s,59.6uJy/beam@native, XX YY] U [148.99..150.98GHz,31250.00kHz,1.3mJy/beam@10km/s,64.7uJy/beam@native, XX YY] U [150.99..152.98GHz,31250.00kHz,1.4mJy/beam@10km/s,69.3uJy/beam@native, XX YY]	137.9870839900263	62042.1601777654	ALMA	Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 - a testbed for binary-disc interaction Edge-On Disk Study (EODS): II. HCO<SUP>+</SUP> and CO vertical stratification in the disk surrounding SSTTau042021 Masses and Implications for Ages of Low-mass Pre-main-sequence Stars in Taurus and Ophiuchus Modest Dust Settling in the IRAS04302+2247 Class I Protoplanetary Disk Observations of edge-on protoplanetary disks with ALMA. I. Results from continuum data Observations of highly inclined disks with ALMA: Results from <SUP>12</SUP>CO gas and continuum observations Observations of pre- and proto-brown dwarfs in nearby clouds: Paving the way to further constraining theories of brown dwarf formation The edge-on protoplanetary disk HH 48 NE. I. Modeling the geometry and stellar parameters Turbulence in protoplanetary disks: A systematic analysis of dust settling in 33 disks	Foucher, C. Martinien, L. Palau, Aina Ragusa, Enrico Simon, M. Sturm, J. A. Villenave, M. Villenave, Marion	Foucher, C.; Dutrey, A.; Piétu, V.; Guilloteau, S.; Chapillon, E.; Denis-Alpizar, O.; Dartois, E.; Di Folco, E.; Gavino, S.; Gorti, U.; Henning, Th.; Kóspál, Á.; Le Petit, F.; Majumdar, L.; Meshaka, R.; Phuong, N. T.; Ruaud, M.; Semenov, D.; Tang, Y. W.; Wolf, S. Martinien, L.; Duchêne, G.; Ribas, Á.; Villenave, M.; Ménard, F.; Stapelfeldt, K. R.; Pinte, C. Palau, Aina; Huélamo, Nuria; Barrado, David; Dunham, Michael M.; Lee, Chang Won Ragusa, Enrico; Fasano, Daniele; Toci, Claudia; Duchêne, Gaspard; Cuello, Nicolás; Villenave, Marion; van der Plas, Gerrit; Lodato, Giuseppe; Ménard, François; Price, Daniel J.; Pinte, Christophe; Stapelfeldt, Karl; Wolff, Schuyler Simon, M.; Guilloteau, S.; Beck, Tracy L.; Chapillon, E.; Di Folco, E.; Dutrey, A.; Feiden, Gregory A.; Grosso, N.; Piétu, V.; Prato, L.; Schaefer, Gail H. Sturm, J. A.; McClure, M. K.; Law, C. J.; Harsono, D.; Bergner, J. B.; Dartois, E.; Drozdovskaya, M. N.; Ioppolo, S.; Öberg, K. I.; Palumbo, M. E.; Pendleton, Y. J.; Rocha, W. R. M.; Terada, H.; U	<BR /> Aims: We aim to study vertical settling and radial drift of dust in protoplanetary disks from a different perspective: an edge-on view. An estimation of the amplitude of settling and drift is highly relevant to understanding planet formation. <BR /> Methods: We analyze a sample of 12 HST-selected edge-on protoplanetary disks (i.e., seen with high inclinations) for which the vertical extent of the emission layers can be constrained directly. We present ALMA high angular resolution continuum images (~0.1'') of these disks at two wavelengths, 0.89 and 2.06 mm (respectively ALMA bands 7 and 4), supplemented with archival band 6 data (1.33 mm) where available. <BR /> Results: Several sources show constant brightness profiles along their major axis with a steep drop at the outer edges. Two disks have central holes with additional compact continuum emission at the location of the central star. For most sources, the millimeter continuum emission is more compact than the scattered light, both in the vertical an	2019	We propose to observe a well-defined sample of Edge-On Disks to study the radial and vertical distribution of the dust. Scattered light images of edge-on disks like HH 30 have established what we think is typical for the shape and flaring of protoplanetary disks. However, these conclusions are correct only for the small grains, i.e. the near-IR scattering opacity carriers, but are very likely incorrect for the larger dust particles emitting at longer wavelengths. The large particles are expected to be distributed differently in particular because of dust settling, but so far we are still missing direct images that would reveal the vertical stratification of dust of all sizes in T Tauri disks. ALMA cycle-4 offers the perfect opportunity (resolution, sensitivity), and the edge-on geometry allows for direct conclusions beyond doubt. By comparing the gas distribution to the distributions of small and large dust grains, we can draw definite conclusions about the disk shape, and the settling and radial migration of	HK_Tau_B_a_04_TM1	Stapelfeldt, Karl; Louvet, Fabien; Padgett, Deborah; Dent, Bill; Benisty, Myriam; Dougados, Catherine; Pinte, Christophe; Chripko, Svenya; Duchene, Gaspard; Perrin, Marshall; Hales, Antonio; Wolff, Schuyler;	1.3125550648954356	0.031933735311887014	1.3846008	uid://A001/X87d/Xa3d	uid://A001/X126d/X104	uid://A002/Xc4d618/X6812	Measuring vertical settling and radial drift of dust: A survey of young edge-on disks	S	TARGET	T	1.1287170476360884	F	2019ApJ...884...42S 2020A&A...642A.164V 2021MNRAS.507.1157R 2023A&A...677A..17S 2023ApJ...946...70V 2024NewAR..9901711P 2025A&A...697A..64V 2025A&A...704A..32F 2026A&A...710A.140M	Disks around low-mass stars;null	Disks and planet formation	fmenard	Menard, Francois	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.1.00460.S	ALMA	JAO	ALMA	uid://A001/X126d/X104.source.IRAS_04302+2247.spw.19	image	2	ari_l	IRAS_04302+2247	68.31874999995279	22.889000000008497	0.011156098900091987	Circle ICRS 68.318750 22.889000 0.005578			128	1	2	0.05439461068023409	58023.287185	58023.292914	362.88	362.88	0.002127445819073256	0.002157830544246029	4509.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X126d/X104	application/x-votable+xml; content=datalink		2016.1.00460.S	Public	175.3349361852637	-16.710053471499975	4	4.785255856929346E-7	2.0E9	A007:DV09 A015:DA61 A027:DV06 A074:DA47 A087:DV25 A090:DV24 A091:DA45 A092:DV14 A093:DV20 A096:PM01 A104:DA58 A105:DV02 A108:DA50 A110:DA41 A111:PM02 A115:DA43 A116:DV07 A118:DV01 A120:DA44 A121:DA55 A122:DV11 A123:DA42 A124:DA51 A126:DV10 A127:DA49 A128:DV13 A129:DA46 A130:DV15 A131:PM03 A132:DV23 A133:PM04 A135:DA57 P401:DA65 P409:DV04 P410:DA64 S301:DA60 S303:DA63 S307:DV05 S309:DA56 W202:DA54 W207:DV17 W209:DA48 W210:DV22	F	2018-12-19T17:19:01.000	0.05439461068023409	[136.99..138.98GHz,31250.00kHz,1.3mJy/beam@10km/s,63uJy/beam@native, XX YY] U [138.93..140.92GHz,31250.00kHz,1.2mJy/beam@10km/s,59.6uJy/beam@native, XX YY] U [148.99..150.98GHz,31250.00kHz,1.3mJy/beam@10km/s,64.7uJy/beam@native, XX YY] U [150.99..152.98GHz,31250.00kHz,1.4mJy/beam@10km/s,69.3uJy/beam@native, XX YY]	139.92447881319725	62042.1601777654	ALMA	Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 - a testbed for binary-disc interaction Edge-On Disk Study (EODS): II. HCO<SUP>+</SUP> and CO vertical stratification in the disk surrounding SSTTau042021 Masses and Implications for Ages of Low-mass Pre-main-sequence Stars in Taurus and Ophiuchus Modest Dust Settling in the IRAS04302+2247 Class I Protoplanetary Disk Observations of edge-on protoplanetary disks with ALMA. I. Results from continuum data Observations of highly inclined disks with ALMA: Results from <SUP>12</SUP>CO gas and continuum observations Observations of pre- and proto-brown dwarfs in nearby clouds: Paving the way to further constraining theories of brown dwarf formation The edge-on protoplanetary disk HH 48 NE. I. Modeling the geometry and stellar parameters Turbulence in protoplanetary disks: A systematic analysis of dust settling in 33 disks	Foucher, C. Martinien, L. Palau, Aina Ragusa, Enrico Simon, M. Sturm, J. A. Villenave, M. Villenave, Marion	Foucher, C.; Dutrey, A.; Piétu, V.; Guilloteau, S.; Chapillon, E.; Denis-Alpizar, O.; Dartois, E.; Di Folco, E.; Gavino, S.; Gorti, U.; Henning, Th.; Kóspál, Á.; Le Petit, F.; Majumdar, L.; Meshaka, R.; Phuong, N. T.; Ruaud, M.; Semenov, D.; Tang, Y. W.; Wolf, S. Martinien, L.; Duchêne, G.; Ribas, Á.; Villenave, M.; Ménard, F.; Stapelfeldt, K. R.; Pinte, C. Palau, Aina; Huélamo, Nuria; Barrado, David; Dunham, Michael M.; Lee, Chang Won Ragusa, Enrico; Fasano, Daniele; Toci, Claudia; Duchêne, Gaspard; Cuello, Nicolás; Villenave, Marion; van der Plas, Gerrit; Lodato, Giuseppe; Ménard, François; Price, Daniel J.; Pinte, Christophe; Stapelfeldt, Karl; Wolff, Schuyler Simon, M.; Guilloteau, S.; Beck, Tracy L.; Chapillon, E.; Di Folco, E.; Dutrey, A.; Feiden, Gregory A.; Grosso, N.; Piétu, V.; Prato, L.; Schaefer, Gail H. Sturm, J. A.; McClure, M. K.; Law, C. J.; Harsono, D.; Bergner, J. B.; Dartois, E.; Drozdovskaya, M. N.; Ioppolo, S.; Öberg, K. I.; Palumbo, M. E.; Pendleton, Y. J.; Rocha, W. R. M.; Terada, H.; U	<BR /> Aims: We aim to study vertical settling and radial drift of dust in protoplanetary disks from a different perspective: an edge-on view. An estimation of the amplitude of settling and drift is highly relevant to understanding planet formation. <BR /> Methods: We analyze a sample of 12 HST-selected edge-on protoplanetary disks (i.e., seen with high inclinations) for which the vertical extent of the emission layers can be constrained directly. We present ALMA high angular resolution continuum images (~0.1'') of these disks at two wavelengths, 0.89 and 2.06 mm (respectively ALMA bands 7 and 4), supplemented with archival band 6 data (1.33 mm) where available. <BR /> Results: Several sources show constant brightness profiles along their major axis with a steep drop at the outer edges. Two disks have central holes with additional compact continuum emission at the location of the central star. For most sources, the millimeter continuum emission is more compact than the scattered light, both in the vertical an	2019	We propose to observe a well-defined sample of Edge-On Disks to study the radial and vertical distribution of the dust. Scattered light images of edge-on disks like HH 30 have established what we think is typical for the shape and flaring of protoplanetary disks. However, these conclusions are correct only for the small grains, i.e. the near-IR scattering opacity carriers, but are very likely incorrect for the larger dust particles emitting at longer wavelengths. The large particles are expected to be distributed differently in particular because of dust settling, but so far we are still missing direct images that would reveal the vertical stratification of dust of all sizes in T Tauri disks. ALMA cycle-4 offers the perfect opportunity (resolution, sensitivity), and the edge-on geometry allows for direct conclusions beyond doubt. By comparing the gas distribution to the distributions of small and large dust grains, we can draw definite conclusions about the disk shape, and the settling and radial migration of	HK_Tau_B_a_04_TM1	Stapelfeldt, Karl; Louvet, Fabien; Padgett, Deborah; Dent, Bill; Benisty, Myriam; Dougados, Catherine; Pinte, Christophe; Chripko, Svenya; Duchene, Gaspard; Perrin, Marshall; Hales, Antonio; Wolff, Schuyler;	1.2344995419843197	0.031933735311887014	1.3846008	uid://A001/X87d/Xa3d	uid://A001/X126d/X104	uid://A002/Xc4d618/X6812	Measuring vertical settling and radial drift of dust: A survey of young edge-on disks	S	TARGET	T	1.1287170476360884	F	2019ApJ...884...42S 2020A&A...642A.164V 2021MNRAS.507.1157R 2023A&A...677A..17S 2023ApJ...946...70V 2024NewAR..9901711P 2025A&A...697A..64V 2025A&A...704A..32F 2026A&A...710A.140M	Disks around low-mass stars;null	Disks and planet formation	fmenard	Menard, Francois	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.1.00460.S	ALMA	JAO	ALMA	uid://A001/X126d/X104.source.IRAS_04302+2247.spw.21	image	2	ari_l	IRAS_04302+2247	68.31874999995279	22.889000000008497	0.011156098900091987	Circle ICRS 68.318750 22.889000 0.005578			128	1	2	0.05439461068023409	58023.287185	58023.292914	362.88	362.88	0.0019856623726308923	0.0020121069070897072	4768.0764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X126d/X104	application/x-votable+xml; content=datalink		2016.1.00460.S	Public	175.3349361852637	-16.710053471499975	4	4.164719696599608E-7	2.0E9	A007:DV09 A015:DA61 A027:DV06 A074:DA47 A087:DV25 A090:DV24 A091:DA45 A092:DV14 A093:DV20 A096:PM01 A104:DA58 A105:DV02 A108:DA50 A110:DA41 A111:PM02 A115:DA43 A116:DV07 A118:DV01 A120:DA44 A121:DA55 A122:DV11 A123:DA42 A124:DA51 A126:DV10 A127:DA49 A128:DV13 A129:DA46 A130:DV15 A131:PM03 A132:DV23 A133:PM04 A135:DA57 P401:DA65 P409:DV04 P410:DA64 S301:DA60 S303:DA63 S307:DV05 S309:DA56 W202:DA54 W207:DV17 W209:DA48 W210:DV22	F	2018-12-19T17:19:01.000	0.05439461068023409	[136.99..138.98GHz,31250.00kHz,1.3mJy/beam@10km/s,63uJy/beam@native, XX YY] U [138.93..140.92GHz,31250.00kHz,1.2mJy/beam@10km/s,59.6uJy/beam@native, XX YY] U [148.99..150.98GHz,31250.00kHz,1.3mJy/beam@10km/s,64.7uJy/beam@native, XX YY] U [150.99..152.98GHz,31250.00kHz,1.4mJy/beam@10km/s,69.3uJy/beam@native, XX YY]	149.9864325722464	62042.1601777654	ALMA	Circumbinary and circumstellar discs around the eccentric binary IRAS 04158+2805 - a testbed for binary-disc interaction Edge-On Disk Study (EODS): II. HCO<SUP>+</SUP> and CO vertical stratification in the disk surrounding SSTTau042021 Masses and Implications for Ages of Low-mass Pre-main-sequence Stars in Taurus and Ophiuchus Modest Dust Settling in the IRAS04302+2247 Class I Protoplanetary Disk Observations of edge-on protoplanetary disks with ALMA. I. Results from continuum data Observations of highly inclined disks with ALMA: Results from <SUP>12</SUP>CO gas and continuum observations Observations of pre- and proto-brown dwarfs in nearby clouds: Paving the way to further constraining theories of brown dwarf formation The edge-on protoplanetary disk HH 48 NE. I. Modeling the geometry and stellar parameters Turbulence in protoplanetary disks: A systematic analysis of dust settling in 33 disks	Foucher, C. Martinien, L. Palau, Aina Ragusa, Enrico Simon, M. Sturm, J. A. Villenave, M. Villenave, Marion	Foucher, C.; Dutrey, A.; Piétu, V.; Guilloteau, S.; Chapillon, E.; Denis-Alpizar, O.; Dartois, E.; Di Folco, E.; Gavino, S.; Gorti, U.; Henning, Th.; Kóspál, Á.; Le Petit, F.; Majumdar, L.; Meshaka, R.; Phuong, N. T.; Ruaud, M.; Semenov, D.; Tang, Y. W.; Wolf, S. Martinien, L.; Duchêne, G.; Ribas, Á.; Villenave, M.; Ménard, F.; Stapelfeldt, K. R.; Pinte, C. Palau, Aina; Huélamo, Nuria; Barrado, David; Dunham, Michael M.; Lee, Chang Won Ragusa, Enrico; Fasano, Daniele; Toci, Claudia; Duchêne, Gaspard; Cuello, Nicolás; Villenave, Marion; van der Plas, Gerrit; Lodato, Giuseppe; Ménard, François; Price, Daniel J.; Pinte, Christophe; Stapelfeldt, Karl; Wolff, Schuyler Simon, M.; Guilloteau, S.; Beck, Tracy L.; Chapillon, E.; Di Folco, E.; Dutrey, A.; Feiden, Gregory A.; Grosso, N.; Piétu, V.; Prato, L.; Schaefer, Gail H. Sturm, J. A.; McClure, M. K.; Law, C. J.; Harsono, D.; Bergner, J. B.; Dartois, E.; Drozdovskaya, M. N.; Ioppolo, S.; Öberg, K. I.; Palumbo, M. E.; Pendleton, Y. J.; Rocha, W. R. M.; Terada, H.; U	<BR /> Aims: We aim to study vertical settling and radial drift of dust in protoplanetary disks from a different perspective: an edge-on view. An estimation of the amplitude of settling and drift is highly relevant to understanding planet formation. <BR /> Methods: We analyze a sample of 12 HST-selected edge-on protoplanetary disks (i.e., seen with high inclinations) for which the vertical extent of the emission layers can be constrained directly. We present ALMA high angular resolution continuum images (~0.1'') of these disks at two wavelengths, 0.89 and 2.06 mm (respectively ALMA bands 7 and 4), supplemented with archival band 6 data (1.33 mm) where available. <BR /> Results: Several sources show constant brightness profiles along their major axis with a steep drop at the outer edges. Two disks have central holes with additional compact continuum emission at the location of the central star. For most sources, the millimeter continuum emission is more compact than the scattered light, both in the vertical an	2019	We propose to observe a well-defined sample of Edge-On Disks to study the radial and vertical distribution of the dust. Scattered light images of edge-on disks like HH 30 have established what we think is typical for the shape and flaring of protoplanetary disks. However, these conclusions are correct only for the small grains, i.e. the near-IR scattering opacity carriers, but are very likely incorrect for the larger dust particles emitting at longer wavelengths. The large particles are expected to be distributed differently in particular because of dust settling, but so far we are still missing direct images that would reveal the vertical stratification of dust of all sizes in T Tauri disks. ALMA cycle-4 offers the perfect opportunity (resolution, sensitivity), and the edge-on geometry allows for direct conclusions beyond doubt. By comparing the gas distribution to the distributions of small and large dust grains, we can draw definite conclusions about the disk shape, and the settling and radial migration of	HK_Tau_B_a_04_TM1	Stapelfeldt, Karl; Louvet, Fabien; Padgett, Deborah; Dent, Bill; Benisty, Myriam; Dougados, Catherine; Pinte, Christophe; Chripko, Svenya; Duchene, Gaspard; Perrin, Marshall; Hales, Antonio; Wolff, Schuyler;	1.2933926526662614	0.031933735311887014	1.3846008	uid://A001/X87d/Xa3d	uid://A001/X126d/X104	uid://A002/Xc4d618/X6812	Measuring vertical settling and radial drift of dust: A survey of young edge-on disks	S	TARGET	T	1.1287170476360884	F	2019ApJ...884...42S 2020A&A...642A.164V 2021MNRAS.507.1157R 2023A&A...677A..17S 2023ApJ...946...70V 2024NewAR..9901711P 2025A&A...697A..64V 2025A&A...704A..32F 2026A&A...710A.140M	Disks around low-mass stars;null	Disks and planet formation	fmenard	Menard, Francois	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00027.S	ALMA	JAO	ALMA	uid://A001/X14c3/X4ca.source.J0006-0623.spw.22	cube	2		J0006-0623	1.5578874999859933	-6.393148611110186	0.020064157443853516	Circle ICRS 1.557887 -6.393149 0.010032			256	1	2	8.491258595966949	58861.864856	58861.871862	604.8	604.8	0.002232839911988313	0.00226647241581177	17185.357154134068	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/X4ca	application/x-votable+xml; content=datalink		2019.2.00027.S	Public	93.50553584426984	-66.64651638772955	4	1.318712757184586E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2022-10-28T04:31:47.000	8.491258595966949	[130.40..132.39GHz,7812.01kHz,13mJy/beam@10km/s,606.6uJy/beam@native, XX YY] U [132.27..134.27GHz,7812.01kHz,11.9mJy/beam@10km/s,562.7uJy/beam@native, XX YY] U [142.32..144.31GHz,7812.01kHz,12.1mJy/beam@10km/s,593.5uJy/beam@native, XX YY] U [144.01..146.00GHz,7812.01kHz,12.8mJy/beam@10km/s,629.8uJy/beam@native, XX YY]	133.26890348028485	16264.562456224106	ALMA	Characterization of Herschel-selected strong lens candidates through HST and sub-mm/mm observations	Borsato, E.	Borsato, E.; Marchetti, L.; Negrello, M.; Corsini, E. M.; Wake, D.; Amvrosiadis, A.; Baker, A. J.; Bakx, T. J. L. C.; Beelen, A.; Berta, S.; Beyer, A.; Clements, D. L.; Cooray, A.; Cox, P.; Dannerbauer, H.; de Zotti, G.; Dye, S.; Eales, S. A.; Enia, A.; Farrah, D.; Gonzalez-Nuevo, J.; Hughes, D. H.; Ismail, D.; Jin, S.; Lapi, A.; Lehnert, M. D.; Neri, R.; Pérez-Fournon, I.; Riechers, D. A.; Rodighiero, G.; Scott, D.; Serjeant, S.; Stanley, F.; Urquhart, S.; van der Werf, P.; Vaccari, M.; Wang, L.; Yang, C.; Young, A.	We have carried out Hubble Space Telescope (HST) snapshot observations at 1.1 μm of 281 candidate strongly lensed galaxies identified in the wide-area extragalactic surveys conducted with the Herschel Space Observatory. Our candidates comprise systems with flux densities at $500\, \mu$m, S<SUB>500</SUB> ≥ 80 mJy. We model and subtract the surface brightness distribution for 130 systems, where we identify a candidate for the foreground lens candidate. After combining visual inspection, archival high-resolution observations, and lens subtraction, we divide the systems into different classes according to their lensing likelihood. We confirm 65 systems to be lensed. Of these, 30 are new discoveries. We successfully perform lens modelling and source reconstruction on 23 systems, where the foreground lenses are isolated galaxies and the background sources are detected in the HST images. All the systems are successfully modelled as a singular isothermal ellipsoid. The Einstein radii of the lenses and the magnificati	2024	We request ACA observations of the CO(J=7-6) transition in a small sample of 5 high-redshift (z>~3), hyper-luminous (Lbol > 10^14 Lsun), dust-obscured quasars for which at least two other lower-J CO line transitions have already been detected with ALMA and VLA. This is a pilot program motivated by the surprisingly bright detection of the CO(J=12-11) transition in the most luminous obscured quasar known, W2246-0526, which suggests that it is possible to detect mid-J CO transitions in these extreme objects using the ACA. The goal of this project is two-fold: (1) to start investigating the excitation properties of the warm molecular gas in high-z obscured quasars and place them in context with other dusty galaxy populations, and (2) to determine whether the CO(J=7-6) line, which has recently been proposed as a good star formation rate indicator, can be truly used in galaxies with such extreme environments. This will be the first time that such a study is conducted in this new population of high-z quasars.	W2246-05_a_04_7M	Blain, Andrew; Penney, Jordan; Aravena, Manuel; Jun, Hyunsung; Tsai, Chao-Wei; Wu, Jingwen; Stern, Daniel; Assef, Roberto; González López, Jorge; Eisenhardt, Peter;	11.934583151161686	0.2983223799471183	5.186	uid://A001/X14c3/X4c9	uid://A001/X14c3/X4ca	uid://A002/Xe6a684/X751e	A Pilot Study of Warm Molecular Gas in High-redshift Obscured Quasars	S	BANDPASS FLUX WVR	F	49.18607660453939	F	2024MNRAS.528.6222B	High-z Active Galactic Nuclei (AGN);null	Active galaxies	tdiazsantos	Diaz-Santos, Tanio	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00027.S	ALMA	JAO	ALMA	uid://A001/X14c3/X4ca.source.J0006-0623.spw.18	cube	2		J0006-0623	1.5578874999859933	-6.393148611110186	0.020064157443853516	Circle ICRS 1.557887 -6.393149 0.010032			256	1	2	8.491258595966949	58861.864856	58861.871862	604.8	604.8	0.002053385146210099	0.0020817943735649664	18432.24856536339	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/X4ca	application/x-votable+xml; content=datalink		2019.2.00027.S	Public	93.50553584426984	-66.64651638772955	4	1.1139108384934392E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2022-10-28T04:31:47.000	8.491258595966949	[130.40..132.39GHz,7812.01kHz,13mJy/beam@10km/s,606.6uJy/beam@native, XX YY] U [132.27..134.27GHz,7812.01kHz,11.9mJy/beam@10km/s,562.7uJy/beam@native, XX YY] U [142.32..144.31GHz,7812.01kHz,12.1mJy/beam@10km/s,593.5uJy/beam@native, XX YY] U [144.01..146.00GHz,7812.01kHz,12.8mJy/beam@10km/s,629.8uJy/beam@native, XX YY]	145.00294705503072	16264.562456224106	ALMA	Characterization of Herschel-selected strong lens candidates through HST and sub-mm/mm observations	Borsato, E.	Borsato, E.; Marchetti, L.; Negrello, M.; Corsini, E. M.; Wake, D.; Amvrosiadis, A.; Baker, A. J.; Bakx, T. J. L. C.; Beelen, A.; Berta, S.; Beyer, A.; Clements, D. L.; Cooray, A.; Cox, P.; Dannerbauer, H.; de Zotti, G.; Dye, S.; Eales, S. A.; Enia, A.; Farrah, D.; Gonzalez-Nuevo, J.; Hughes, D. H.; Ismail, D.; Jin, S.; Lapi, A.; Lehnert, M. D.; Neri, R.; Pérez-Fournon, I.; Riechers, D. A.; Rodighiero, G.; Scott, D.; Serjeant, S.; Stanley, F.; Urquhart, S.; van der Werf, P.; Vaccari, M.; Wang, L.; Yang, C.; Young, A.	We have carried out Hubble Space Telescope (HST) snapshot observations at 1.1 μm of 281 candidate strongly lensed galaxies identified in the wide-area extragalactic surveys conducted with the Herschel Space Observatory. Our candidates comprise systems with flux densities at $500\, \mu$m, S<SUB>500</SUB> ≥ 80 mJy. We model and subtract the surface brightness distribution for 130 systems, where we identify a candidate for the foreground lens candidate. After combining visual inspection, archival high-resolution observations, and lens subtraction, we divide the systems into different classes according to their lensing likelihood. We confirm 65 systems to be lensed. Of these, 30 are new discoveries. We successfully perform lens modelling and source reconstruction on 23 systems, where the foreground lenses are isolated galaxies and the background sources are detected in the HST images. All the systems are successfully modelled as a singular isothermal ellipsoid. The Einstein radii of the lenses and the magnificati	2024	We request ACA observations of the CO(J=7-6) transition in a small sample of 5 high-redshift (z>~3), hyper-luminous (Lbol > 10^14 Lsun), dust-obscured quasars for which at least two other lower-J CO line transitions have already been detected with ALMA and VLA. This is a pilot program motivated by the surprisingly bright detection of the CO(J=12-11) transition in the most luminous obscured quasar known, W2246-0526, which suggests that it is possible to detect mid-J CO transitions in these extreme objects using the ACA. The goal of this project is two-fold: (1) to start investigating the excitation properties of the warm molecular gas in high-z obscured quasars and place them in context with other dusty galaxy populations, and (2) to determine whether the CO(J=7-6) line, which has recently been proposed as a good star formation rate indicator, can be truly used in galaxies with such extreme environments. This will be the first time that such a study is conducted in this new population of high-z quasars.	W2246-05_a_04_7M	Blain, Andrew; Penney, Jordan; Aravena, Manuel; Jun, Hyunsung; Tsai, Chao-Wei; Wu, Jingwen; Stern, Daniel; Assef, Roberto; González López, Jorge; Eisenhardt, Peter;	12.806699729476712	0.2983223799471183	5.186	uid://A001/X14c3/X4c9	uid://A001/X14c3/X4ca	uid://A002/Xe6a684/X751e	A Pilot Study of Warm Molecular Gas in High-redshift Obscured Quasars	S	BANDPASS FLUX WVR	F	49.18607660453939	F	2024MNRAS.528.6222B	High-z Active Galactic Nuclei (AGN);null	Active galaxies	tdiazsantos	Diaz-Santos, Tanio	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00027.S	ALMA	JAO	ALMA	uid://A001/X14c3/X4ca.source.J0006-0623.spw.16	cube	2		J0006-0623	1.5578874999859933	-6.393148611110186	0.020064157443853516	Circle ICRS 1.557887 -6.393149 0.010032			256	1	2	8.491258595966949	58861.864856	58861.871862	604.8	604.8	0.002077447881763904	0.002106531556733332	18215.797068347456	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/X4ca	application/x-votable+xml; content=datalink		2019.2.00027.S	Public	93.50553584426984	-66.64651638772955	4	1.1403555741587441E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2022-10-28T04:31:47.000	8.491258595966949	[130.40..132.39GHz,7812.01kHz,13mJy/beam@10km/s,606.6uJy/beam@native, XX YY] U [132.27..134.27GHz,7812.01kHz,11.9mJy/beam@10km/s,562.7uJy/beam@native, XX YY] U [142.32..144.31GHz,7812.01kHz,12.1mJy/beam@10km/s,593.5uJy/beam@native, XX YY] U [144.01..146.00GHz,7812.01kHz,12.8mJy/beam@10km/s,629.8uJy/beam@native, XX YY]	143.31186318206863	16264.562456224106	ALMA	Characterization of Herschel-selected strong lens candidates through HST and sub-mm/mm observations	Borsato, E.	Borsato, E.; Marchetti, L.; Negrello, M.; Corsini, E. M.; Wake, D.; Amvrosiadis, A.; Baker, A. J.; Bakx, T. J. L. C.; Beelen, A.; Berta, S.; Beyer, A.; Clements, D. L.; Cooray, A.; Cox, P.; Dannerbauer, H.; de Zotti, G.; Dye, S.; Eales, S. A.; Enia, A.; Farrah, D.; Gonzalez-Nuevo, J.; Hughes, D. H.; Ismail, D.; Jin, S.; Lapi, A.; Lehnert, M. D.; Neri, R.; Pérez-Fournon, I.; Riechers, D. A.; Rodighiero, G.; Scott, D.; Serjeant, S.; Stanley, F.; Urquhart, S.; van der Werf, P.; Vaccari, M.; Wang, L.; Yang, C.; Young, A.	We have carried out Hubble Space Telescope (HST) snapshot observations at 1.1 μm of 281 candidate strongly lensed galaxies identified in the wide-area extragalactic surveys conducted with the Herschel Space Observatory. Our candidates comprise systems with flux densities at $500\, \mu$m, S<SUB>500</SUB> ≥ 80 mJy. We model and subtract the surface brightness distribution for 130 systems, where we identify a candidate for the foreground lens candidate. After combining visual inspection, archival high-resolution observations, and lens subtraction, we divide the systems into different classes according to their lensing likelihood. We confirm 65 systems to be lensed. Of these, 30 are new discoveries. We successfully perform lens modelling and source reconstruction on 23 systems, where the foreground lenses are isolated galaxies and the background sources are detected in the HST images. All the systems are successfully modelled as a singular isothermal ellipsoid. The Einstein radii of the lenses and the magnificati	2024	We request ACA observations of the CO(J=7-6) transition in a small sample of 5 high-redshift (z>~3), hyper-luminous (Lbol > 10^14 Lsun), dust-obscured quasars for which at least two other lower-J CO line transitions have already been detected with ALMA and VLA. This is a pilot program motivated by the surprisingly bright detection of the CO(J=12-11) transition in the most luminous obscured quasar known, W2246-0526, which suggests that it is possible to detect mid-J CO transitions in these extreme objects using the ACA. The goal of this project is two-fold: (1) to start investigating the excitation properties of the warm molecular gas in high-z obscured quasars and place them in context with other dusty galaxy populations, and (2) to determine whether the CO(J=7-6) line, which has recently been proposed as a good star formation rate indicator, can be truly used in galaxies with such extreme environments. This will be the first time that such a study is conducted in this new population of high-z quasars.	W2246-05_a_04_7M	Blain, Andrew; Penney, Jordan; Aravena, Manuel; Jun, Hyunsung; Tsai, Chao-Wei; Wu, Jingwen; Stern, Daniel; Assef, Roberto; González López, Jorge; Eisenhardt, Peter;	12.140618009111432	0.2983223799471183	5.186	uid://A001/X14c3/X4c9	uid://A001/X14c3/X4ca	uid://A002/Xe6a684/X751e	A Pilot Study of Warm Molecular Gas in High-redshift Obscured Quasars	S	BANDPASS FLUX WVR	F	49.18607660453939	F	2024MNRAS.528.6222B	High-z Active Galactic Nuclei (AGN);null	Active galaxies	tdiazsantos	Diaz-Santos, Tanio	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00027.S	ALMA	JAO	ALMA	uid://A001/X14c3/X4ca.source.J0006-0623.spw.20	cube	2		J0006-0623	1.5578874999859933	-6.393148611110186	0.020064157443853516	Circle ICRS 1.557887 -6.393149 0.010032			256	1	2	8.491258595966949	58861.864856	58861.871862	604.8	604.8	0.002264466011285942	0.002299065390449191	16945.342153196507	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/X4ca	application/x-votable+xml; content=datalink		2019.2.00027.S	Public	93.50553584426984	-66.64651638772955	4	1.3566234299041584E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2022-10-28T04:31:47.000	8.491258595966949	[130.40..132.39GHz,7812.01kHz,13mJy/beam@10km/s,606.6uJy/beam@native, XX YY] U [132.27..134.27GHz,7812.01kHz,11.9mJy/beam@10km/s,562.7uJy/beam@native, XX YY] U [142.32..144.31GHz,7812.01kHz,12.1mJy/beam@10km/s,593.5uJy/beam@native, XX YY] U [144.01..146.00GHz,7812.01kHz,12.8mJy/beam@10km/s,629.8uJy/beam@native, XX YY]	131.39372357647204	16264.562456224106	ALMA	Characterization of Herschel-selected strong lens candidates through HST and sub-mm/mm observations	Borsato, E.	Borsato, E.; Marchetti, L.; Negrello, M.; Corsini, E. M.; Wake, D.; Amvrosiadis, A.; Baker, A. J.; Bakx, T. J. L. C.; Beelen, A.; Berta, S.; Beyer, A.; Clements, D. L.; Cooray, A.; Cox, P.; Dannerbauer, H.; de Zotti, G.; Dye, S.; Eales, S. A.; Enia, A.; Farrah, D.; Gonzalez-Nuevo, J.; Hughes, D. H.; Ismail, D.; Jin, S.; Lapi, A.; Lehnert, M. D.; Neri, R.; Pérez-Fournon, I.; Riechers, D. A.; Rodighiero, G.; Scott, D.; Serjeant, S.; Stanley, F.; Urquhart, S.; van der Werf, P.; Vaccari, M.; Wang, L.; Yang, C.; Young, A.	We have carried out Hubble Space Telescope (HST) snapshot observations at 1.1 μm of 281 candidate strongly lensed galaxies identified in the wide-area extragalactic surveys conducted with the Herschel Space Observatory. Our candidates comprise systems with flux densities at $500\, \mu$m, S<SUB>500</SUB> ≥ 80 mJy. We model and subtract the surface brightness distribution for 130 systems, where we identify a candidate for the foreground lens candidate. After combining visual inspection, archival high-resolution observations, and lens subtraction, we divide the systems into different classes according to their lensing likelihood. We confirm 65 systems to be lensed. Of these, 30 are new discoveries. We successfully perform lens modelling and source reconstruction on 23 systems, where the foreground lenses are isolated galaxies and the background sources are detected in the HST images. All the systems are successfully modelled as a singular isothermal ellipsoid. The Einstein radii of the lenses and the magnificati	2024	We request ACA observations of the CO(J=7-6) transition in a small sample of 5 high-redshift (z>~3), hyper-luminous (Lbol > 10^14 Lsun), dust-obscured quasars for which at least two other lower-J CO line transitions have already been detected with ALMA and VLA. This is a pilot program motivated by the surprisingly bright detection of the CO(J=12-11) transition in the most luminous obscured quasar known, W2246-0526, which suggests that it is possible to detect mid-J CO transitions in these extreme objects using the ACA. The goal of this project is two-fold: (1) to start investigating the excitation properties of the warm molecular gas in high-z obscured quasars and place them in context with other dusty galaxy populations, and (2) to determine whether the CO(J=7-6) line, which has recently been proposed as a good star formation rate indicator, can be truly used in galaxies with such extreme environments. This will be the first time that such a study is conducted in this new population of high-z quasars.	W2246-05_a_04_7M	Blain, Andrew; Penney, Jordan; Aravena, Manuel; Jun, Hyunsung; Tsai, Chao-Wei; Wu, Jingwen; Stern, Daniel; Assef, Roberto; González López, Jorge; Eisenhardt, Peter;	12.957037162286747	0.2983223799471183	5.186	uid://A001/X14c3/X4c9	uid://A001/X14c3/X4ca	uid://A002/Xe6a684/X751e	A Pilot Study of Warm Molecular Gas in High-redshift Obscured Quasars	S	BANDPASS FLUX WVR	F	49.18607660453939	F	2024MNRAS.528.6222B	High-z Active Galactic Nuclei (AGN);null	Active galaxies	tdiazsantos	Diaz-Santos, Tanio	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00968.S	ALMA	JAO	ALMA	uid://A001/X2d20/X1d04.source.HD_113457.spw.27	cube	2		HD_113457	196.25796653987481	-64.4416894357759	0.007189168021281242	Polygon ICRS 196.266037 -64.442583 196.264708 -64.443802 196.262431 -64.444724 196.259528 -64.445220 196.257967 -64.445284 196.255894 -64.445171 196.253069 -64.444597 196.251892 -64.444150 196.250665 -64.443421 196.249700 -64.442140 196.249897 -64.440795 196.251227 -64.439576 196.253503 -64.438654 196.256406 -64.438159 196.257967 -64.438095 196.260038 -64.438208 196.262863 -64.438781 196.264040 -64.439229 196.265267 -64.439958 196.266232 -64.441239			3840	1	2	0.86803063999998	59931.423263	59931.591616	1814.398	1814.398	0.001297825803813311	0.0013031130613531613	471167.45564775355	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X1d04	application/x-votable+xml; content=datalink		2022.1.00968.S	Public	304.39802531712195	-1.6086930966607902	6	2.7545321602065926E-9	9.375E8	A001:DA46 A002:DV06 A003:DA50 A006:DA43 A010:DV15 A015:DV21 A016:DA64 A017:DV17 A019:DV13 A022:DV02 A023:DA63 A024:DV10 A025:DV16 A026:DV05 A027:DV03 A028:DV08 A033:DV01 A034:DV24 A036:DA55 A039:DV07 A040:DA45 A041:DV14 A044:DA44 A046:DA59 A047:DA42 A048:DV19 A049:DA47 A050:DA49 A058:DV12 A060:DV20 A062:DA65 A066:DA62 A068:DV09 A069:DV18 A070:DV11 A073:DA61 A074:DA57 A076:DV04 A083:DA41 A085:DA53 A088:DV22 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2024-01-09T18:51:07.000	0.86803063999998	[216.00..217.98GHz,31250.00kHz,920.8uJy/beam@10km/s,55.4uJy/beam@native, XX YY] U [218.85..220.73GHz,1128.91kHz,1mJy/beam@10km/s,62.8uJy/beam@native, XX YY] U [230.06..231.00GHz,488.28kHz,1mJy/beam@10km/s,95uJy/beam@native, XX YY] U [232.00..233.98GHz,31250.00kHz,897.3uJy/beam@10km/s,55.9uJy/beam@native, XX YY]	230.52729218485797	636.2758174540091	ALMA	Dust populations from 30 to 1000 au in the debris disk of HD 120326: Panchromatic view with VLT/SPHERE, ALMA, and HST/STIS Resolving the large exoKuiper belt of the HD 126062 debris disc and extended gas emission in its vicinity	Desgrange, C. Miley, James M.	Desgrange, C.; Milli, J.; Chauvin, G.; Bonnefoy, M.; Henning, Th.; Miley, J.; Kennedy, G.; Juillard, S.; Olofsson, J.; Augereau, J.-C.; Faramaz, V.; Christiaens, V.; Sefilian, A. A.; Mazoyer, J.; Pearce, T. D.; Beust, H.; Ménard, F.; Booth, M. Miley, James M.; Kennedy, Grant M.; Ribas, Álvaro; Macias, Enrique; Carpenter, John; Vioque, Miguel; Luhman, Kevin; Haworth, Thomas; Weber, Philipp; Perez, Sebastian; Zurlo, Alice	Context. Intermediate mass stars (1─3 M<SUB>⊙</SUB>) host some of the brightest and most well-studied debris discs. This stellar class is also the most frequent host of molecular gas in systems with ages beyond typical protoplanetary disc lifetimes and the most likely to host detected giant planets in radial velocity surveys. The debris discs of intermediate mass stars have therefore become a fertile ground for studying disc-planet interactions. Aims. In this work, we present the first ALMA observations towards the A-type star HD 126062, located in Upper Centaurus Lupus/Lower Centaurus Crux, with the aim of characterising the properties of its debris disc. Methods. We probed the thermal continuum emission using observations at 1.3 mm, which were analysed through image reconstruction while employing different visibility weighting regimes in addition to parametric model fitting to the observed visibilities. The observational setup also covers the frequency of the <SUP>12</SUP>CO molecular line, allowing for ima	2025	ALMA detections of gas-rich debris disks around A type stars of 10-50 Myr have led to a re-writing of our understanding of late disk evolution. Collisions between planetesimals in debris disks release a second generation of molecular gas that can have a transformative influence on the atmospheres of planets in the system. Although only found in around 20 objects so far, the detection rate of secondary gas in debris disks suggests that this is not an exceptional group, but rather the normal state for debris disks, particularly around A-type stars. We require a large survey to validate the proposed ubiquity of large amounts of molecular gas in systems that have evolved beyond the protoplanetary phase. We request a deep survey of gas and dust in the debris disks of A type stars in Lower Centarus Crux and Upper Centaurus Lupus (15-20 Myr). Our 46 targets + 10 archival objects comprise a nearby, complete sample that is ideal for detecting molecular gas in systems that have evolved from the protoplanetary- to debri	HD_10679_a_06_TM1	Luhman, Kevin; Ribas, Álvaro; Carpenter, John; Macias, Enrique; Vioque, Miguel;	1.0492416981048454	0.03146861862332155	0.34809595	uid://A001/X2d20/X1d03	uid://A001/X2d20/X1d04	uid://A002/X1009c59/X22ed5	Exception or the Rule? A Survey for Gas in Debris Disks	S	TARGET	T	9.905355908309456	T	2025A&A...698A.183D 2025A&A...703A.235M	Debris disks;null	Disks and planet formation	jmiley	Miley, James	488.28125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00968.S	ALMA	JAO	ALMA	uid://A001/X2d20/X1d04.source.HD_113457.spw.25	cube	2		HD_113457	196.25796653987481	-64.4416894357759	0.007189168021281242	Polygon ICRS 196.266037 -64.442583 196.264708 -64.443802 196.262431 -64.444724 196.259528 -64.445220 196.257967 -64.445284 196.255894 -64.445171 196.253069 -64.444597 196.251892 -64.444150 196.250665 -64.443421 196.249700 -64.442140 196.249897 -64.440795 196.251227 -64.439576 196.253503 -64.438654 196.256406 -64.438159 196.257967 -64.438095 196.260038 -64.438208 196.262863 -64.438781 196.264040 -64.439229 196.265267 -64.439958 196.266232 -64.441239			1920	1	2	0.86803063999998	59931.423263	59931.591616	1814.398	1814.398	0.0013582060713091446	0.0013698361470712301	195525.71396593194	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X1d04	application/x-votable+xml; content=datalink		2022.1.00968.S	Public	304.39802531712195	-1.6086930966607902	6	7.0060214739132665E-9	1.875E9	A001:DA46 A002:DV06 A003:DA50 A006:DA43 A010:DV15 A015:DV21 A016:DA64 A017:DV17 A019:DV13 A022:DV02 A023:DA63 A024:DV10 A025:DV16 A026:DV05 A027:DV03 A028:DV08 A033:DV01 A034:DV24 A036:DA55 A039:DV07 A040:DA45 A041:DV14 A044:DA44 A046:DA59 A047:DA42 A048:DV19 A049:DA47 A050:DA49 A058:DV12 A060:DV20 A062:DA65 A066:DA62 A068:DV09 A069:DV18 A070:DV11 A073:DA61 A074:DA57 A076:DV04 A083:DA41 A085:DA53 A088:DV22 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2024-01-09T18:51:07.000	0.86803063999998	[216.00..217.98GHz,31250.00kHz,920.8uJy/beam@10km/s,55.4uJy/beam@native, XX YY] U [218.85..220.73GHz,1128.91kHz,1mJy/beam@10km/s,62.8uJy/beam@native, XX YY] U [230.06..231.00GHz,488.28kHz,1mJy/beam@10km/s,95uJy/beam@native, XX YY] U [232.00..233.98GHz,31250.00kHz,897.3uJy/beam@10km/s,55.9uJy/beam@native, XX YY]	219.78978526262478	636.2758174540091	ALMA	Dust populations from 30 to 1000 au in the debris disk of HD 120326: Panchromatic view with VLT/SPHERE, ALMA, and HST/STIS Resolving the large exoKuiper belt of the HD 126062 debris disc and extended gas emission in its vicinity	Desgrange, C. Miley, James M.	Desgrange, C.; Milli, J.; Chauvin, G.; Bonnefoy, M.; Henning, Th.; Miley, J.; Kennedy, G.; Juillard, S.; Olofsson, J.; Augereau, J.-C.; Faramaz, V.; Christiaens, V.; Sefilian, A. A.; Mazoyer, J.; Pearce, T. D.; Beust, H.; Ménard, F.; Booth, M. Miley, James M.; Kennedy, Grant M.; Ribas, Álvaro; Macias, Enrique; Carpenter, John; Vioque, Miguel; Luhman, Kevin; Haworth, Thomas; Weber, Philipp; Perez, Sebastian; Zurlo, Alice	Context. Intermediate mass stars (1─3 M<SUB>⊙</SUB>) host some of the brightest and most well-studied debris discs. This stellar class is also the most frequent host of molecular gas in systems with ages beyond typical protoplanetary disc lifetimes and the most likely to host detected giant planets in radial velocity surveys. The debris discs of intermediate mass stars have therefore become a fertile ground for studying disc-planet interactions. Aims. In this work, we present the first ALMA observations towards the A-type star HD 126062, located in Upper Centaurus Lupus/Lower Centaurus Crux, with the aim of characterising the properties of its debris disc. Methods. We probed the thermal continuum emission using observations at 1.3 mm, which were analysed through image reconstruction while employing different visibility weighting regimes in addition to parametric model fitting to the observed visibilities. The observational setup also covers the frequency of the <SUP>12</SUP>CO molecular line, allowing for ima	2025	ALMA detections of gas-rich debris disks around A type stars of 10-50 Myr have led to a re-writing of our understanding of late disk evolution. Collisions between planetesimals in debris disks release a second generation of molecular gas that can have a transformative influence on the atmospheres of planets in the system. Although only found in around 20 objects so far, the detection rate of secondary gas in debris disks suggests that this is not an exceptional group, but rather the normal state for debris disks, particularly around A-type stars. We require a large survey to validate the proposed ubiquity of large amounts of molecular gas in systems that have evolved beyond the protoplanetary phase. We request a deep survey of gas and dust in the debris disks of A type stars in Lower Centarus Crux and Upper Centaurus Lupus (15-20 Myr). Our 46 targets + 10 archival objects comprise a nearby, complete sample that is ideal for detecting molecular gas in systems that have evolved from the protoplanetary- to debri	HD_10679_a_06_TM1	Luhman, Kevin; Ribas, Álvaro; Carpenter, John; Macias, Enrique; Vioque, Miguel;	1.0043244707003216	0.03146861862332155	0.34809595	uid://A001/X2d20/X1d03	uid://A001/X2d20/X1d04	uid://A002/X1009c59/X22ed5	Exception or the Rule? A Survey for Gas in Debris Disks	S	TARGET	T	9.905355908309456	T	2025A&A...698A.183D 2025A&A...703A.235M	Debris disks;null	Disks and planet formation	jmiley	Miley, James	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00968.S	ALMA	JAO	ALMA	uid://A001/X2d20/X1d04.source.HD_113457.spw.17	image	2		HD_113457	196.25796653987481	-64.4416894357759	0.007189168021281242	Polygon ICRS 196.266037 -64.442583 196.264708 -64.443802 196.262431 -64.444724 196.259528 -64.445220 196.257967 -64.445284 196.255894 -64.445171 196.253069 -64.444597 196.251892 -64.444150 196.250665 -64.443421 196.249700 -64.442140 196.249897 -64.440795 196.251227 -64.439576 196.253503 -64.438654 196.256406 -64.438159 196.257967 -64.438095 196.260038 -64.438208 196.262863 -64.438781 196.264040 -64.439229 196.265267 -64.439958 196.266232 -64.441239			128	1	2	0.86803063999998	59931.423263	59931.591616	1814.398	1814.398	0.0013753077577410013	0.0013879425565930378	6975.534818550265	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X1d04	application/x-votable+xml; content=datalink		2022.1.00968.S	Public	304.39802531712195	-1.6086930966607902	6	1.9897600348626891E-7	2.0E9	A001:DA46 A002:DV06 A003:DA50 A006:DA43 A010:DV15 A015:DV21 A016:DA64 A017:DV17 A019:DV13 A022:DV02 A023:DA63 A024:DV10 A025:DV16 A026:DV05 A027:DV03 A028:DV08 A033:DV01 A034:DV24 A036:DA55 A039:DV07 A040:DA45 A041:DV14 A044:DA44 A046:DA59 A047:DA42 A048:DV19 A049:DA47 A050:DA49 A058:DV12 A060:DV20 A062:DA65 A066:DA62 A068:DV09 A069:DV18 A070:DV11 A073:DA61 A074:DA57 A076:DV04 A083:DA41 A085:DA53 A088:DV22 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2024-01-09T18:51:07.000	0.86803063999998	[216.00..217.98GHz,31250.00kHz,920.8uJy/beam@10km/s,55.4uJy/beam@native, XX YY] U [218.85..220.73GHz,1128.91kHz,1mJy/beam@10km/s,62.8uJy/beam@native, XX YY] U [230.06..231.00GHz,488.28kHz,1mJy/beam@10km/s,95uJy/beam@native, XX YY] U [232.00..233.98GHz,31250.00kHz,897.3uJy/beam@10km/s,55.9uJy/beam@native, XX YY]	216.9899153917265	636.2758174540091	ALMA	Dust populations from 30 to 1000 au in the debris disk of HD 120326: Panchromatic view with VLT/SPHERE, ALMA, and HST/STIS Resolving the large exoKuiper belt of the HD 126062 debris disc and extended gas emission in its vicinity	Desgrange, C. Miley, James M.	Desgrange, C.; Milli, J.; Chauvin, G.; Bonnefoy, M.; Henning, Th.; Miley, J.; Kennedy, G.; Juillard, S.; Olofsson, J.; Augereau, J.-C.; Faramaz, V.; Christiaens, V.; Sefilian, A. A.; Mazoyer, J.; Pearce, T. D.; Beust, H.; Ménard, F.; Booth, M. Miley, James M.; Kennedy, Grant M.; Ribas, Álvaro; Macias, Enrique; Carpenter, John; Vioque, Miguel; Luhman, Kevin; Haworth, Thomas; Weber, Philipp; Perez, Sebastian; Zurlo, Alice	Context. Intermediate mass stars (1─3 M<SUB>⊙</SUB>) host some of the brightest and most well-studied debris discs. This stellar class is also the most frequent host of molecular gas in systems with ages beyond typical protoplanetary disc lifetimes and the most likely to host detected giant planets in radial velocity surveys. The debris discs of intermediate mass stars have therefore become a fertile ground for studying disc-planet interactions. Aims. In this work, we present the first ALMA observations towards the A-type star HD 126062, located in Upper Centaurus Lupus/Lower Centaurus Crux, with the aim of characterising the properties of its debris disc. Methods. We probed the thermal continuum emission using observations at 1.3 mm, which were analysed through image reconstruction while employing different visibility weighting regimes in addition to parametric model fitting to the observed visibilities. The observational setup also covers the frequency of the <SUP>12</SUP>CO molecular line, allowing for ima	2025	ALMA detections of gas-rich debris disks around A type stars of 10-50 Myr have led to a re-writing of our understanding of late disk evolution. Collisions between planetesimals in debris disks release a second generation of molecular gas that can have a transformative influence on the atmospheres of planets in the system. Although only found in around 20 objects so far, the detection rate of secondary gas in debris disks suggests that this is not an exceptional group, but rather the normal state for debris disks, particularly around A-type stars. We require a large survey to validate the proposed ubiquity of large amounts of molecular gas in systems that have evolved beyond the protoplanetary phase. We request a deep survey of gas and dust in the debris disks of A type stars in Lower Centarus Crux and Upper Centaurus Lupus (15-20 Myr). Our 46 targets + 10 archival objects comprise a nearby, complete sample that is ideal for detecting molecular gas in systems that have evolved from the protoplanetary- to debri	HD_10679_a_06_TM1	Luhman, Kevin; Ribas, Álvaro; Carpenter, John; Macias, Enrique; Vioque, Miguel;	0.9208111645889425	0.03146861862332155	0.34809595	uid://A001/X2d20/X1d03	uid://A001/X2d20/X1d04	uid://A002/X1009c59/X22ed5	Exception or the Rule? A Survey for Gas in Debris Disks	S	TARGET	T	9.905355908309456	T	2025A&A...698A.183D 2025A&A...703A.235M	Debris disks;null	Disks and planet formation	jmiley	Miley, James	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00968.S	ALMA	JAO	ALMA	uid://A001/X2d20/X1d04.source.HD_113457.spw.23	image	2		HD_113457	196.25796653987481	-64.4416894357759	0.007189168021281242	Polygon ICRS 196.266037 -64.442583 196.264708 -64.443802 196.262431 -64.444724 196.259528 -64.445220 196.257967 -64.445284 196.255894 -64.445171 196.253069 -64.444597 196.251892 -64.444150 196.250665 -64.443421 196.249700 -64.442140 196.249897 -64.440795 196.251227 -64.439576 196.253503 -64.438654 196.256406 -64.438159 196.257967 -64.438095 196.260038 -64.438208 196.262863 -64.438781 196.264040 -64.439229 196.265267 -64.439958 196.266232 -64.441239			128	1	2	0.86803063999998	59931.423263	59931.591616	1814.398	1814.398	0.001281266493236242	0.0012922255907186048	7424.018952643896	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X1d04	application/x-votable+xml; content=datalink		2022.1.00968.S	Public	304.39802531712195	-1.6086930966607902	6	1.7258662064663226E-7	2.0E9	A001:DA46 A002:DV06 A003:DA50 A006:DA43 A010:DV15 A015:DV21 A016:DA64 A017:DV17 A019:DV13 A022:DV02 A023:DA63 A024:DV10 A025:DV16 A026:DV05 A027:DV03 A028:DV08 A033:DV01 A034:DV24 A036:DA55 A039:DV07 A040:DA45 A041:DV14 A044:DA44 A046:DA59 A047:DA42 A048:DV19 A049:DA47 A050:DA49 A058:DV12 A060:DV20 A062:DA65 A066:DA62 A068:DV09 A069:DV18 A070:DV11 A073:DA61 A074:DA57 A076:DV04 A083:DA41 A085:DA53 A088:DV22 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2024-01-09T18:51:07.000	0.86803063999998	[216.00..217.98GHz,31250.00kHz,920.8uJy/beam@10km/s,55.4uJy/beam@native, XX YY] U [218.85..220.73GHz,1128.91kHz,1mJy/beam@10km/s,62.8uJy/beam@native, XX YY] U [230.06..231.00GHz,488.28kHz,1mJy/beam@10km/s,95uJy/beam@native, XX YY] U [232.00..233.98GHz,31250.00kHz,897.3uJy/beam@10km/s,55.9uJy/beam@native, XX YY]	232.98917182071335	636.2758174540091	ALMA	Dust populations from 30 to 1000 au in the debris disk of HD 120326: Panchromatic view with VLT/SPHERE, ALMA, and HST/STIS Resolving the large exoKuiper belt of the HD 126062 debris disc and extended gas emission in its vicinity	Desgrange, C. Miley, James M.	Desgrange, C.; Milli, J.; Chauvin, G.; Bonnefoy, M.; Henning, Th.; Miley, J.; Kennedy, G.; Juillard, S.; Olofsson, J.; Augereau, J.-C.; Faramaz, V.; Christiaens, V.; Sefilian, A. A.; Mazoyer, J.; Pearce, T. D.; Beust, H.; Ménard, F.; Booth, M. Miley, James M.; Kennedy, Grant M.; Ribas, Álvaro; Macias, Enrique; Carpenter, John; Vioque, Miguel; Luhman, Kevin; Haworth, Thomas; Weber, Philipp; Perez, Sebastian; Zurlo, Alice	Context. Intermediate mass stars (1─3 M<SUB>⊙</SUB>) host some of the brightest and most well-studied debris discs. This stellar class is also the most frequent host of molecular gas in systems with ages beyond typical protoplanetary disc lifetimes and the most likely to host detected giant planets in radial velocity surveys. The debris discs of intermediate mass stars have therefore become a fertile ground for studying disc-planet interactions. Aims. In this work, we present the first ALMA observations towards the A-type star HD 126062, located in Upper Centaurus Lupus/Lower Centaurus Crux, with the aim of characterising the properties of its debris disc. Methods. We probed the thermal continuum emission using observations at 1.3 mm, which were analysed through image reconstruction while employing different visibility weighting regimes in addition to parametric model fitting to the observed visibilities. The observational setup also covers the frequency of the <SUP>12</SUP>CO molecular line, allowing for ima	2025	ALMA detections of gas-rich debris disks around A type stars of 10-50 Myr have led to a re-writing of our understanding of late disk evolution. Collisions between planetesimals in debris disks release a second generation of molecular gas that can have a transformative influence on the atmospheres of planets in the system. Although only found in around 20 objects so far, the detection rate of secondary gas in debris disks suggests that this is not an exceptional group, but rather the normal state for debris disks, particularly around A-type stars. We require a large survey to validate the proposed ubiquity of large amounts of molecular gas in systems that have evolved beyond the protoplanetary phase. We request a deep survey of gas and dust in the debris disks of A type stars in Lower Centarus Crux and Upper Centaurus Lupus (15-20 Myr). Our 46 targets + 10 archival objects comprise a nearby, complete sample that is ideal for detecting molecular gas in systems that have evolved from the protoplanetary- to debri	HD_10679_a_06_TM1	Luhman, Kevin; Ribas, Álvaro; Carpenter, John; Macias, Enrique; Vioque, Miguel;	0.8972817871593292	0.03146861862332155	0.34809595	uid://A001/X2d20/X1d03	uid://A001/X2d20/X1d04	uid://A002/X1009c59/X22ed5	Exception or the Rule? A Survey for Gas in Debris Disks	S	TARGET	T	9.905355908309456	T	2025A&A...698A.183D 2025A&A...703A.235M	Debris disks;null	Disks and planet formation	jmiley	Miley, James	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00235.S	ALMA	JAO	ALMA	uid://A001/X14c3/Xa6a.source.WR_77aa.spw.20	image	2		WR_77aa	251.69283089684998	-45.79953937291711	0.01053627317772616	Circle ICRS 251.692831 -45.799539 0.005268			128	1	2	4.816322643560846	59465.956957	59465.971575	151.2	151.2	0.0011061920398449136	0.0011143520241138904	8608.251218964842	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/Xa6a	application/x-votable+xml; content=datalink		2019.2.00235.S	Public	339.55551431879366	-0.3314330226818277	6	1.284938239944662E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N604:CM11	F	2022-10-12T14:56:43.000	4.816322643560846	[253.33..255.31GHz,31250.00kHz,28.2mJy/beam@10km/s,1.8mJy/beam@native, XX YY] U [255.32..257.32GHz,976.56kHz,25.9mJy/beam@10km/s,1.7mJy/beam@native, XX YY] U [269.03..271.01GHz,31250.00kHz,28.2mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [271.03..273.01GHz,31250.00kHz,32.6mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	270.02076769736846	1137.8314503373933	ALMA						The powerful and highly ionized winds of Wolf-Rayet (WR) stars emit free-free radiation and recombination lines from the radio to near-IR. Despite being bright at sub-mm wavelengths, few suitable observations have been made in the gap between radio and near-IR wavelengths to characterise the wind properties and compare with models. We propose to use ACA in Bands 3 and 6 (92 and 263GHz) to build a catalogue of mm/sub-mm spectral indices and flux densities of the winds of 57 of the brightest Galactic WR stars. This will be used to identify potential new high-frequency calibration sources for ALMA (to increase the number of phase calibrators available for high frequency bands), investigate statistical trends and compare with wind emission models, and use to select sources and plan future high spatial resolution imaging of the wind morphologies. The catalogue and images will have a strong legacy value to the evolved massive star community.	HD_15193_a_06_7M	Agliozzo, Claudia;	28.249458338719243	0.9397814171930079	1.8	uid://A001/X14c3/Xa69	uid://A001/X14c3/Xa6a	uid://A002/Xf06573/X2c	A legacy survey of Wolf-Rayet star winds	S	TARGET	T	27.424128345117644	T		Hypergiants;Evolved stars - Shaping/physical structure	Stars and stellar evolution	nphillip	Phillips, Neil	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00235.S	ALMA	JAO	ALMA	uid://A001/X14c3/Xa6a.source.WR_77aa.spw.16	cube	2		WR_77aa	251.69283089684998	-45.79953937291711	0.01053627317772616	Circle ICRS 251.692831 -45.799539 0.005268			4096	1	2	4.816322643560846	59465.956957	59465.971575	151.2	151.2	0.0011650499569170636	0.0011741745563150733	263477.03599782253	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/Xa6a	application/x-votable+xml; content=datalink		2019.2.00235.S	Public	339.55551431879366	-0.3314330226818277	6	4.456116678282734E-9	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N604:CM11	F	2022-10-12T14:56:43.000	4.816322643560846	[253.33..255.31GHz,31250.00kHz,28.2mJy/beam@10km/s,1.8mJy/beam@native, XX YY] U [255.32..257.32GHz,976.56kHz,25.9mJy/beam@10km/s,1.7mJy/beam@native, XX YY] U [269.03..271.01GHz,31250.00kHz,28.2mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [271.03..273.01GHz,31250.00kHz,32.6mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	256.3217150300925	1137.8314503373933	ALMA						The powerful and highly ionized winds of Wolf-Rayet (WR) stars emit free-free radiation and recombination lines from the radio to near-IR. Despite being bright at sub-mm wavelengths, few suitable observations have been made in the gap between radio and near-IR wavelengths to characterise the wind properties and compare with models. We propose to use ACA in Bands 3 and 6 (92 and 263GHz) to build a catalogue of mm/sub-mm spectral indices and flux densities of the winds of 57 of the brightest Galactic WR stars. This will be used to identify potential new high-frequency calibration sources for ALMA (to increase the number of phase calibrators available for high frequency bands), investigate statistical trends and compare with wind emission models, and use to select sources and plan future high spatial resolution imaging of the wind morphologies. The catalogue and images will have a strong legacy value to the evolved massive star community.	HD_15193_a_06_7M	Agliozzo, Claudia;	25.88507541000786	0.9397814171930079	1.8	uid://A001/X14c3/Xa69	uid://A001/X14c3/Xa6a	uid://A002/Xf06573/X2c	A legacy survey of Wolf-Rayet star winds	S	TARGET	T	27.424128345117644	T		Hypergiants;Evolved stars - Shaping/physical structure	Stars and stellar evolution	nphillip	Phillips, Neil	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00235.S	ALMA	JAO	ALMA	uid://A001/X14c3/Xa6a.source.WR_77aa.spw.22	image	2		WR_77aa	251.69283089684998	-45.79953937291711	0.01053627317772616	Circle ICRS 251.692831 -45.799539 0.005268			128	1	2	4.816322643560846	59465.956957	59465.971575	151.2	151.2	0.001098087838068153	0.0011061282621698952	8672.251218964842	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/Xa6a	application/x-votable+xml; content=datalink		2019.2.00235.S	Public	339.55551431879366	-0.3314330226818277	6	1.2661113126137075E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N604:CM11	F	2022-10-12T14:56:43.000	4.816322643560846	[253.33..255.31GHz,31250.00kHz,28.2mJy/beam@10km/s,1.8mJy/beam@native, XX YY] U [255.32..257.32GHz,976.56kHz,25.9mJy/beam@10km/s,1.7mJy/beam@native, XX YY] U [269.03..271.01GHz,31250.00kHz,28.2mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [271.03..273.01GHz,31250.00kHz,32.6mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	272.0209212499743	1137.8314503373933	ALMA						The powerful and highly ionized winds of Wolf-Rayet (WR) stars emit free-free radiation and recombination lines from the radio to near-IR. Despite being bright at sub-mm wavelengths, few suitable observations have been made in the gap between radio and near-IR wavelengths to characterise the wind properties and compare with models. We propose to use ACA in Bands 3 and 6 (92 and 263GHz) to build a catalogue of mm/sub-mm spectral indices and flux densities of the winds of 57 of the brightest Galactic WR stars. This will be used to identify potential new high-frequency calibration sources for ALMA (to increase the number of phase calibrators available for high frequency bands), investigate statistical trends and compare with wind emission models, and use to select sources and plan future high spatial resolution imaging of the wind morphologies. The catalogue and images will have a strong legacy value to the evolved massive star community.	HD_15193_a_06_7M	Agliozzo, Claudia;	32.58552273956551	0.9397814171930079	1.8	uid://A001/X14c3/Xa69	uid://A001/X14c3/Xa6a	uid://A002/Xf06573/X2c	A legacy survey of Wolf-Rayet star winds	S	TARGET	T	27.424128345117644	T		Hypergiants;Evolved stars - Shaping/physical structure	Stars and stellar evolution	nphillip	Phillips, Neil	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2019.2.00235.S	ALMA	JAO	ALMA	uid://A001/X14c3/Xa6a.source.WR_77aa.spw.18	image	2		WR_77aa	251.69283089684998	-45.79953937291711	0.01053627317772616	Circle ICRS 251.692831 -45.799539 0.005268			128	1	2	4.816322643560846	59465.956957	59465.971575	151.2	151.2	0.00117422115606121	0.0011834198279614726	8169.348781035155	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X14c3/Xa6a	application/x-votable+xml; content=datalink		2019.2.00235.S	Public	339.55551431879366	-0.3314330226818277	6	1.448498537710335E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N604:CM11	F	2022-10-12T14:56:43.000	4.816322643560846	[253.33..255.31GHz,31250.00kHz,28.2mJy/beam@10km/s,1.8mJy/beam@native, XX YY] U [255.32..257.32GHz,976.56kHz,25.9mJy/beam@10km/s,1.7mJy/beam@native, XX YY] U [269.03..271.01GHz,31250.00kHz,28.2mJy/beam@10km/s,1.9mJy/beam@native, XX YY] U [271.03..273.01GHz,31250.00kHz,32.6mJy/beam@10km/s,2.2mJy/beam@native, XX YY]	254.31948611826044	1137.8314503373933	ALMA						The powerful and highly ionized winds of Wolf-Rayet (WR) stars emit free-free radiation and recombination lines from the radio to near-IR. Despite being bright at sub-mm wavelengths, few suitable observations have been made in the gap between radio and near-IR wavelengths to characterise the wind properties and compare with models. We propose to use ACA in Bands 3 and 6 (92 and 263GHz) to build a catalogue of mm/sub-mm spectral indices and flux densities of the winds of 57 of the brightest Galactic WR stars. This will be used to identify potential new high-frequency calibration sources for ALMA (to increase the number of phase calibrators available for high frequency bands), investigate statistical trends and compare with wind emission models, and use to select sources and plan future high spatial resolution imaging of the wind morphologies. The catalogue and images will have a strong legacy value to the evolved massive star community.	HD_15193_a_06_7M	Agliozzo, Claudia;	28.15979453580765	0.9397814171930079	1.8	uid://A001/X14c3/Xa69	uid://A001/X14c3/Xa6a	uid://A002/Xf06573/X2c	A legacy survey of Wolf-Rayet star winds	S	TARGET	T	27.424128345117644	T		Hypergiants;Evolved stars - Shaping/physical structure	Stars and stellar evolution	nphillip	Phillips, Neil	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.00180.L	ALMA	JAO	ALMA	uid://A001/X3645/Xd4.source.S20_29.spw.27	cube	2		S20_29	150.14546875000332	2.451224444445148	0.006472532857231973	Polygon ICRS 150.145469 2.447988 150.144276 2.448215 150.143251 2.448865 150.142848 2.449322 150.142457 2.450033 150.142230 2.451224 150.142287 2.451831 150.142538 2.452602 150.143251 2.453584 150.144276 2.454233 150.145469 2.454461 150.146076 2.454403 150.146848 2.454153 150.147830 2.453440 150.148481 2.452416 150.148708 2.451224 150.148481 2.450033 150.148204 2.449490 150.147686 2.448865 150.146661 2.448215			480	1	2	0.6309309744519427	60599.518612	60600.449254	72.576	72.576	0.0012299908689014122	0.0012395057761373043	62430.74930780874	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3645/Xd4	application/x-votable+xml; content=datalink		2023.1.00180.L	Public	236.57279856962563	42.285161551624746	6	1.9855122575516044E-8	1.875E9	A001:DA63 A002:DA45 A003:DA57 A005:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A017:DA48 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV09 A027:DV03 A034:DV15 A035:DA51 A036:DV16 A039:DA50 A040:DV24 A041:DA59 A042:DV04 A043:DV13 A044:DA46 A045:DA65 A047:DA42 A049:DV11 A050:DV10 A058:DV12 A060:DV23 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DA61 A073:DA41 A074:DV14 A075:DV22 A076:DA53 A082:DA58 A083:DV08 A085:DV05 A088:DA54	F	2025-10-31T03:25:14.000	0.6309309744519427	[240.06..241.94GHz,3904.30kHz,6.7mJy/beam@10km/s,438.8uJy/beam@native, XX YY] U [241.86..243.74GHz,3904.30kHz,6.7mJy/beam@10km/s,439.3uJy/beam@native, XX YY] U [256.06..257.94GHz,3904.30kHz,6.3mJy/beam@10km/s,427.8uJy/beam@native, XX YY] U [257.86..259.74GHz,3904.30kHz,6.3mJy/beam@10km/s,428.2uJy/beam@native, XX YY]	242.80001287771086	4538.887103577384	ALMA	ALMA and JWST Identification of Faint Dusty Star-forming Galaxies up to z ∼ 8 and Their Connection with Other Galaxy Populations Active galactic nuclei-heated dust revealed in ''little red dots'' COSMOS-3D: Dense Circumnuclear Gas Across Black Hole Growth Phases at z ∼ 3 PANORAMIC: Discovery of an ultra-massive grand-design spiral galaxy at z ∼ 5.2 Probing infrared eXcess to investigate early-Universe dust (PIXIEDust) The ALPINE-CRISTAL-JWST Survey: JWST/IFU Optical Observations for 18 Main-sequence Galaxies at z = 4─6	Bakx, Tom J. L. C. Delvecchio, I. Faisst, A. L. Li, Zi-Jian Xiao, Mengyuan Zavala, Jorge A.	Bakx, Tom J. L. C.; Algera, Hiddo S. B.; Jolly, Jean-Baptiste; Esmerian, Clarke; Knudsen, Kirsten; Sommovigo, Laura; Witstok, Joris; Carniani, Stefano; Chen, Jianhang; Eales, Stephen; Ferrara, Andrea; Fudamoto, Yoshinobu; Hagimoto, Masato; Hashimoto, Takuya; Inami, Hanae; Inoue, Akio K.; Khouri, Theo; Mitsuhashi, Ikki; Nyman, Gunnar; Olander, Gustav; Serjeant, Stephen; Smit, Renske; Yoon, Ilsang; Zavala, Jorge; Aalto, Susanne; Casey, Caitlin M.; Tamura, Yoichi; Vlemmings, Wouter Delvecchio, I.; Daddi, E.; Magnelli, B.; Elbaz, D.; Giavalisco, M.; Traina, A.; Lanzuisi, G.; Akins, H. B.; Belli, S.; Casey, C. M.; Gentile, F.; Gruppioni, C.; Pozzi, F.; Zamorani, G. Faisst, A. L.; Fujimoto, S.; Tsujita, A.; Wang, W.; Nezhad, N.; Loiacono, F.; Übler, H.; Béthermin, M.; Cassata, P.; Dessauges-Zavadsky, M.; Herrera-Camus, R.; Schaerer, D.; Silverman, J. D.; Yan, L.; Aravena, M.; De Looze, I.; Förster Schreiber, N. M.; González-López, J.; Spilker, J.; Tadaki, K.; Casey, C. M.; Franco, M.; Harish, S.; McCracken, H. J.;	Despite the implied presence of dust through reddened UV emission in high-redshift galaxies, no dust emission has been detected in the (sub)millimetre regime beyond <inline-formula><tex-math>$z &gt; 8.3$</tex-math></inline-formula>. This study combines around 200 h of Atacama Large Millimetre/submillimetre Array (ALMA) and Northern Extended Millimetre Array (NOEMA) observations on 10 <inline-formula><tex-math>$z &gt; 8$</tex-math></inline-formula> galaxies, revealing no significant dust emission down to a <inline-formula><tex-math>$1 \sigma$</tex-math></inline-formula> depth of 2.0, 2.0, and <inline-formula><tex-math>$1.5 \, \mu$</tex-math></inline-formula>Jy at rest-frame 158, 88 <inline-formula><tex-math>$\mu$</tex-math></inline-formula>m, and across all the data, respectively. This constrains average dust masses to be below <inline-formula><tex-math>$&lt; 10^{5}$</tex-math></inline-formula> M<inline-formula><tex-math>$_{\odot }$</tex-math></inline-formula> at <inline-formula><tex-math>$3 \sigma$</tex-math>	2025	To trace the evolution of galaxies through cosmic time, a multi-band survey including sub-mm data is crucial, especially since recent small-area blank-field surveys show a considerable number of dust-obscured sources even into the Epoch of Reionization at z=6. We propose to carry out a 0.18deg2 blank-field survey at 1.1mm in the COSMOS field, CHAMPS, 3x the area of existing ALMA surveys, to push our understanding of the dusty Universe. CHAMPS complements deep, high-resolution MIRI and NIRCam observations from two JWST Cycle 1 programs with essential sub-mm observations. This will enable us to construct UV-FIR multiwavelength SEDs of ~30,000 MIRI-detected sources, including ~1200 bright, dusty sources directly detected with ALMA out to z~6, and an additional ~120,000 sources with NIRCam-only detections from stacking. With this large area we will find dusty high-z galaxies and provide limits to sub-mm properties of fainter sources via stacking. This program provides a unique opportunity to combine cutting-edge	S20_2_a_06_TM1	Rhodes, Jason; Franco, Maximilien; Maraston, Claudia; Valentino, Francesco; Sanders, David; Shuntov, Marko; Wilkins, Stephen; Martin, Crystal; Bagley, Micaela; Drakos, Nicole; Robertson, Brant; Mercier, Wilfried; Hemmati, Shoubaneh; Mainieri, Vincenzo; Suzuki, Tomoko; Rodighiero, Giulia; Renzini, Alvio; Fujimoto, Seiji; Darvish, Behnam; Akins, Hollis; McCracken, Henry; Kalita, Boris Sindhu; Paquereau, Louise; Gozaliasl, Ghassem; Magdis, Georgios; Enia, Andrea Francesco Maria; González López, Jorge; Gentile, Fabrizio; Scoville, Nick; Champagne, Jaclyn; Algera, Hiddo; Massey, Richard; Ilbert, Olivier; Manning, Sinclaire; Talia, Margherita; Cooke, Kevin; Hayward, Christopher; Vardoulaki, Eleni; Lambrides, Erini; Bongiorno, Angela; Long, Arianna; McKinney, Jed; Nayyeri, Hooshang; Gomez-Guijarro, Carlos; Trakhtenbrot, Benny; Davidzon , Iary; Mobasher, Bahram; Jin, Shuowen; Battisti, Andrew; Koekemoer, Anton; Sparre, Martin; Sommovigo, Laura; Moutard, Thibaud; Onoue, Masafusa; Jahnke, Knud; Kokorev, Vasily; Kashino	6.683564523884541	0.2167077351801419	1.9318154	uid://A001/X3645/Xd3	uid://A001/X3645/Xd4	uid://A002/X11edb41/X10373	The COSMOS High-z ALMA-MIRI Population Survey (CHAMPS): A Wide-Area Comprehensive Survey of the Dusty Universe	L	TARGET	T	8.587340975876911	T	2025A&A...696A.156X 2025A&A...704A.313D 2026ApJ...998L..36Z 2026ApJ..1002....9L 2026ApJS..282...19F 2026MNRAS.546f2284B	Lyman Break Galaxies (LBG);null	Galaxy evolution	afaisst	Faisst, Andreas	3904.296875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.00180.L	ALMA	JAO	ALMA	uid://A001/X3645/Xd4.source.S20_29.spw.25	cube	2		S20_29	150.14546875000332	2.451224444445148	0.006472532857231973	Polygon ICRS 150.145469 2.447988 150.144276 2.448215 150.143251 2.448865 150.142848 2.449322 150.142457 2.450033 150.142230 2.451224 150.142287 2.451831 150.142538 2.452602 150.143251 2.453584 150.144276 2.454233 150.145469 2.454461 150.146076 2.454403 150.146848 2.454153 150.147830 2.453440 150.148481 2.452416 150.148708 2.451224 150.148481 2.450033 150.148204 2.449490 150.147686 2.448865 150.146661 2.448215			480	1	2	0.6309309744519427	60599.518612	60600.449254	72.576	72.576	0.001239142000356119	0.0012487995717649697	61969.69480578451	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3645/Xd4	application/x-votable+xml; content=datalink		2023.1.00180.L	Public	236.57279856962563	42.285161551624746	6	2.0152825705542568E-8	1.875E9	A001:DA63 A002:DA45 A003:DA57 A005:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A017:DA48 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV09 A027:DV03 A034:DV15 A035:DA51 A036:DV16 A039:DA50 A040:DV24 A041:DA59 A042:DV04 A043:DV13 A044:DA46 A045:DA65 A047:DA42 A049:DV11 A050:DV10 A058:DV12 A060:DV23 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DA61 A073:DA41 A074:DV14 A075:DV22 A076:DA53 A082:DA58 A083:DV08 A085:DV05 A088:DA54	F	2025-10-31T03:25:14.000	0.6309309744519427	[240.06..241.94GHz,3904.30kHz,6.7mJy/beam@10km/s,438.8uJy/beam@native, XX YY] U [241.86..243.74GHz,3904.30kHz,6.7mJy/beam@10km/s,439.3uJy/beam@native, XX YY] U [256.06..257.94GHz,3904.30kHz,6.3mJy/beam@10km/s,427.8uJy/beam@native, XX YY] U [257.86..259.74GHz,3904.30kHz,6.3mJy/beam@10km/s,428.2uJy/beam@native, XX YY]	241.00001278092319	4538.887103577384	ALMA	ALMA and JWST Identification of Faint Dusty Star-forming Galaxies up to z ∼ 8 and Their Connection with Other Galaxy Populations Active galactic nuclei-heated dust revealed in ''little red dots'' COSMOS-3D: Dense Circumnuclear Gas Across Black Hole Growth Phases at z ∼ 3 PANORAMIC: Discovery of an ultra-massive grand-design spiral galaxy at z ∼ 5.2 Probing infrared eXcess to investigate early-Universe dust (PIXIEDust) The ALPINE-CRISTAL-JWST Survey: JWST/IFU Optical Observations for 18 Main-sequence Galaxies at z = 4─6	Bakx, Tom J. L. C. Delvecchio, I. Faisst, A. L. Li, Zi-Jian Xiao, Mengyuan Zavala, Jorge A.	Bakx, Tom J. L. C.; Algera, Hiddo S. B.; Jolly, Jean-Baptiste; Esmerian, Clarke; Knudsen, Kirsten; Sommovigo, Laura; Witstok, Joris; Carniani, Stefano; Chen, Jianhang; Eales, Stephen; Ferrara, Andrea; Fudamoto, Yoshinobu; Hagimoto, Masato; Hashimoto, Takuya; Inami, Hanae; Inoue, Akio K.; Khouri, Theo; Mitsuhashi, Ikki; Nyman, Gunnar; Olander, Gustav; Serjeant, Stephen; Smit, Renske; Yoon, Ilsang; Zavala, Jorge; Aalto, Susanne; Casey, Caitlin M.; Tamura, Yoichi; Vlemmings, Wouter Delvecchio, I.; Daddi, E.; Magnelli, B.; Elbaz, D.; Giavalisco, M.; Traina, A.; Lanzuisi, G.; Akins, H. B.; Belli, S.; Casey, C. M.; Gentile, F.; Gruppioni, C.; Pozzi, F.; Zamorani, G. Faisst, A. L.; Fujimoto, S.; Tsujita, A.; Wang, W.; Nezhad, N.; Loiacono, F.; Übler, H.; Béthermin, M.; Cassata, P.; Dessauges-Zavadsky, M.; Herrera-Camus, R.; Schaerer, D.; Silverman, J. D.; Yan, L.; Aravena, M.; De Looze, I.; Förster Schreiber, N. M.; González-López, J.; Spilker, J.; Tadaki, K.; Casey, C. M.; Franco, M.; Harish, S.; McCracken, H. J.;	Despite the implied presence of dust through reddened UV emission in high-redshift galaxies, no dust emission has been detected in the (sub)millimetre regime beyond <inline-formula><tex-math>$z &gt; 8.3$</tex-math></inline-formula>. This study combines around 200 h of Atacama Large Millimetre/submillimetre Array (ALMA) and Northern Extended Millimetre Array (NOEMA) observations on 10 <inline-formula><tex-math>$z &gt; 8$</tex-math></inline-formula> galaxies, revealing no significant dust emission down to a <inline-formula><tex-math>$1 \sigma$</tex-math></inline-formula> depth of 2.0, 2.0, and <inline-formula><tex-math>$1.5 \, \mu$</tex-math></inline-formula>Jy at rest-frame 158, 88 <inline-formula><tex-math>$\mu$</tex-math></inline-formula>m, and across all the data, respectively. This constrains average dust masses to be below <inline-formula><tex-math>$&lt; 10^{5}$</tex-math></inline-formula> M<inline-formula><tex-math>$_{\odot }$</tex-math></inline-formula> at <inline-formula><tex-math>$3 \sigma$</tex-math>	2025	To trace the evolution of galaxies through cosmic time, a multi-band survey including sub-mm data is crucial, especially since recent small-area blank-field surveys show a considerable number of dust-obscured sources even into the Epoch of Reionization at z=6. We propose to carry out a 0.18deg2 blank-field survey at 1.1mm in the COSMOS field, CHAMPS, 3x the area of existing ALMA surveys, to push our understanding of the dusty Universe. CHAMPS complements deep, high-resolution MIRI and NIRCam observations from two JWST Cycle 1 programs with essential sub-mm observations. This will enable us to construct UV-FIR multiwavelength SEDs of ~30,000 MIRI-detected sources, including ~1200 bright, dusty sources directly detected with ALMA out to z~6, and an additional ~120,000 sources with NIRCam-only detections from stacking. With this large area we will find dusty high-z galaxies and provide limits to sub-mm properties of fainter sources via stacking. This program provides a unique opportunity to combine cutting-edge	S20_2_a_06_TM1	Rhodes, Jason; Franco, Maximilien; Maraston, Claudia; Valentino, Francesco; Sanders, David; Shuntov, Marko; Wilkins, Stephen; Martin, Crystal; Bagley, Micaela; Drakos, Nicole; Robertson, Brant; Mercier, Wilfried; Hemmati, Shoubaneh; Mainieri, Vincenzo; Suzuki, Tomoko; Rodighiero, Giulia; Renzini, Alvio; Fujimoto, Seiji; Darvish, Behnam; Akins, Hollis; McCracken, Henry; Kalita, Boris Sindhu; Paquereau, Louise; Gozaliasl, Ghassem; Magdis, Georgios; Enia, Andrea Francesco Maria; González López, Jorge; Gentile, Fabrizio; Scoville, Nick; Champagne, Jaclyn; Algera, Hiddo; Massey, Richard; Ilbert, Olivier; Manning, Sinclaire; Talia, Margherita; Cooke, Kevin; Hayward, Christopher; Vardoulaki, Eleni; Lambrides, Erini; Bongiorno, Angela; Long, Arianna; McKinney, Jed; Nayyeri, Hooshang; Gomez-Guijarro, Carlos; Trakhtenbrot, Benny; Davidzon , Iary; Mobasher, Bahram; Jin, Shuowen; Battisti, Andrew; Koekemoer, Anton; Sparre, Martin; Sommovigo, Laura; Moutard, Thibaud; Onoue, Masafusa; Jahnke, Knud; Kokorev, Vasily; Kashino	6.7020651732460115	0.2167077351801419	1.9318154	uid://A001/X3645/Xd3	uid://A001/X3645/Xd4	uid://A002/X11edb41/X10373	The COSMOS High-z ALMA-MIRI Population Survey (CHAMPS): A Wide-Area Comprehensive Survey of the Dusty Universe	L	TARGET	T	8.587340975876911	T	2025A&A...696A.156X 2025A&A...704A.313D 2026ApJ...998L..36Z 2026ApJ..1002....9L 2026ApJS..282...19F 2026MNRAS.546f2284B	Lyman Break Galaxies (LBG);null	Galaxy evolution	afaisst	Faisst, Andreas	3904.296875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.00180.L	ALMA	JAO	ALMA	uid://A001/X3645/Xd4.source.S20_29.spw.29	cube	2		S20_29	150.14546875000332	2.451224444445148	0.006472532857231973	Polygon ICRS 150.145469 2.447988 150.144276 2.448215 150.143251 2.448865 150.142848 2.449322 150.142457 2.450033 150.142230 2.451224 150.142287 2.451831 150.142538 2.452602 150.143251 2.453584 150.144276 2.454233 150.145469 2.454461 150.146076 2.454403 150.146848 2.454153 150.147830 2.453440 150.148481 2.452416 150.148708 2.451224 150.148481 2.450033 150.148204 2.449490 150.147686 2.448865 150.146661 2.448215			480	1	2	0.6309309744519427	60599.518612	60600.449254	72.576	72.576	0.0011622767685178716	0.0011707692583959534	65588.71742636643	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3645/Xd4	application/x-votable+xml; content=datalink		2023.1.00180.L	Public	236.57279856962563	42.285161551624746	6	1.7721602779370612E-8	1.875E9	A001:DA63 A002:DA45 A003:DA57 A005:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A017:DA48 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV09 A027:DV03 A034:DV15 A035:DA51 A036:DV16 A039:DA50 A040:DV24 A041:DA59 A042:DV04 A043:DV13 A044:DA46 A045:DA65 A047:DA42 A049:DV11 A050:DV10 A058:DV12 A060:DV23 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DA61 A073:DA41 A074:DV14 A075:DV22 A076:DA53 A082:DA58 A083:DV08 A085:DV05 A088:DA54	F	2025-10-31T03:25:14.000	0.6309309744519427	[240.06..241.94GHz,3904.30kHz,6.7mJy/beam@10km/s,438.8uJy/beam@native, XX YY] U [241.86..243.74GHz,3904.30kHz,6.7mJy/beam@10km/s,439.3uJy/beam@native, XX YY] U [256.06..257.94GHz,3904.30kHz,6.3mJy/beam@10km/s,427.8uJy/beam@native, XX YY] U [257.86..259.74GHz,3904.30kHz,6.3mJy/beam@10km/s,428.2uJy/beam@native, XX YY]	257.0000136419467	4538.887103577384	ALMA	ALMA and JWST Identification of Faint Dusty Star-forming Galaxies up to z ∼ 8 and Their Connection with Other Galaxy Populations Active galactic nuclei-heated dust revealed in ''little red dots'' COSMOS-3D: Dense Circumnuclear Gas Across Black Hole Growth Phases at z ∼ 3 PANORAMIC: Discovery of an ultra-massive grand-design spiral galaxy at z ∼ 5.2 Probing infrared eXcess to investigate early-Universe dust (PIXIEDust) The ALPINE-CRISTAL-JWST Survey: JWST/IFU Optical Observations for 18 Main-sequence Galaxies at z = 4─6	Bakx, Tom J. L. C. Delvecchio, I. Faisst, A. L. Li, Zi-Jian Xiao, Mengyuan Zavala, Jorge A.	Bakx, Tom J. L. C.; Algera, Hiddo S. B.; Jolly, Jean-Baptiste; Esmerian, Clarke; Knudsen, Kirsten; Sommovigo, Laura; Witstok, Joris; Carniani, Stefano; Chen, Jianhang; Eales, Stephen; Ferrara, Andrea; Fudamoto, Yoshinobu; Hagimoto, Masato; Hashimoto, Takuya; Inami, Hanae; Inoue, Akio K.; Khouri, Theo; Mitsuhashi, Ikki; Nyman, Gunnar; Olander, Gustav; Serjeant, Stephen; Smit, Renske; Yoon, Ilsang; Zavala, Jorge; Aalto, Susanne; Casey, Caitlin M.; Tamura, Yoichi; Vlemmings, Wouter Delvecchio, I.; Daddi, E.; Magnelli, B.; Elbaz, D.; Giavalisco, M.; Traina, A.; Lanzuisi, G.; Akins, H. B.; Belli, S.; Casey, C. M.; Gentile, F.; Gruppioni, C.; Pozzi, F.; Zamorani, G. Faisst, A. L.; Fujimoto, S.; Tsujita, A.; Wang, W.; Nezhad, N.; Loiacono, F.; Übler, H.; Béthermin, M.; Cassata, P.; Dessauges-Zavadsky, M.; Herrera-Camus, R.; Schaerer, D.; Silverman, J. D.; Yan, L.; Aravena, M.; De Looze, I.; Förster Schreiber, N. M.; González-López, J.; Spilker, J.; Tadaki, K.; Casey, C. M.; Franco, M.; Harish, S.; McCracken, H. J.;	Despite the implied presence of dust through reddened UV emission in high-redshift galaxies, no dust emission has been detected in the (sub)millimetre regime beyond <inline-formula><tex-math>$z &gt; 8.3$</tex-math></inline-formula>. This study combines around 200 h of Atacama Large Millimetre/submillimetre Array (ALMA) and Northern Extended Millimetre Array (NOEMA) observations on 10 <inline-formula><tex-math>$z &gt; 8$</tex-math></inline-formula> galaxies, revealing no significant dust emission down to a <inline-formula><tex-math>$1 \sigma$</tex-math></inline-formula> depth of 2.0, 2.0, and <inline-formula><tex-math>$1.5 \, \mu$</tex-math></inline-formula>Jy at rest-frame 158, 88 <inline-formula><tex-math>$\mu$</tex-math></inline-formula>m, and across all the data, respectively. This constrains average dust masses to be below <inline-formula><tex-math>$&lt; 10^{5}$</tex-math></inline-formula> M<inline-formula><tex-math>$_{\odot }$</tex-math></inline-formula> at <inline-formula><tex-math>$3 \sigma$</tex-math>	2025	To trace the evolution of galaxies through cosmic time, a multi-band survey including sub-mm data is crucial, especially since recent small-area blank-field surveys show a considerable number of dust-obscured sources even into the Epoch of Reionization at z=6. We propose to carry out a 0.18deg2 blank-field survey at 1.1mm in the COSMOS field, CHAMPS, 3x the area of existing ALMA surveys, to push our understanding of the dusty Universe. CHAMPS complements deep, high-resolution MIRI and NIRCam observations from two JWST Cycle 1 programs with essential sub-mm observations. This will enable us to construct UV-FIR multiwavelength SEDs of ~30,000 MIRI-detected sources, including ~1200 bright, dusty sources directly detected with ALMA out to z~6, and an additional ~120,000 sources with NIRCam-only detections from stacking. With this large area we will find dusty high-z galaxies and provide limits to sub-mm properties of fainter sources via stacking. This program provides a unique opportunity to combine cutting-edge	S20_2_a_06_TM1	Rhodes, Jason; Franco, Maximilien; Maraston, Claudia; Valentino, Francesco; Sanders, David; Shuntov, Marko; Wilkins, Stephen; Martin, Crystal; Bagley, Micaela; Drakos, Nicole; Robertson, Brant; Mercier, Wilfried; Hemmati, Shoubaneh; Mainieri, Vincenzo; Suzuki, Tomoko; Rodighiero, Giulia; Renzini, Alvio; Fujimoto, Seiji; Darvish, Behnam; Akins, Hollis; McCracken, Henry; Kalita, Boris Sindhu; Paquereau, Louise; Gozaliasl, Ghassem; Magdis, Georgios; Enia, Andrea Francesco Maria; González López, Jorge; Gentile, Fabrizio; Scoville, Nick; Champagne, Jaclyn; Algera, Hiddo; Massey, Richard; Ilbert, Olivier; Manning, Sinclaire; Talia, Margherita; Cooke, Kevin; Hayward, Christopher; Vardoulaki, Eleni; Lambrides, Erini; Bongiorno, Angela; Long, Arianna; McKinney, Jed; Nayyeri, Hooshang; Gomez-Guijarro, Carlos; Trakhtenbrot, Benny; Davidzon , Iary; Mobasher, Bahram; Jin, Shuowen; Battisti, Andrew; Koekemoer, Anton; Sparre, Martin; Sommovigo, Laura; Moutard, Thibaud; Onoue, Masafusa; Jahnke, Knud; Kokorev, Vasily; Kashino	6.3264409384951055	0.2167077351801419	1.9318154	uid://A001/X3645/Xd3	uid://A001/X3645/Xd4	uid://A002/X11edb41/X10373	The COSMOS High-z ALMA-MIRI Population Survey (CHAMPS): A Wide-Area Comprehensive Survey of the Dusty Universe	L	TARGET	T	8.587340975876911	T	2025A&A...696A.156X 2025A&A...704A.313D 2026ApJ...998L..36Z 2026ApJ..1002....9L 2026ApJS..282...19F 2026MNRAS.546f2284B	Lyman Break Galaxies (LBG);null	Galaxy evolution	afaisst	Faisst, Andreas	3904.296875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2023.1.00180.L	ALMA	JAO	ALMA	uid://A001/X3645/Xd4.source.S20_29.spw.31	cube	2		S20_29	150.14546875000332	2.451224444445148	0.006472532857231973	Polygon ICRS 150.145469 2.447988 150.144276 2.448215 150.143251 2.448865 150.142848 2.449322 150.142457 2.450033 150.142230 2.451224 150.142287 2.451831 150.142538 2.452602 150.143251 2.453584 150.144276 2.454233 150.145469 2.454461 150.146076 2.454403 150.146848 2.454153 150.147830 2.453440 150.148481 2.452416 150.148708 2.451224 150.148481 2.450033 150.148204 2.449490 150.147686 2.448865 150.146661 2.448215			480	1	2	0.6309309744519427	60599.518612	60600.449254	72.576	72.576	0.0011542220429090902	0.0011625968086477097	66049.77192839069	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3645/Xd4	application/x-votable+xml; content=datalink		2023.1.00180.L	Public	236.57279856962563	42.285161551624746	6	1.7475943048453685E-8	1.875E9	A001:DA63 A002:DA45 A003:DA57 A005:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A017:DA48 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV09 A027:DV03 A034:DV15 A035:DA51 A036:DV16 A039:DA50 A040:DV24 A041:DA59 A042:DV04 A043:DV13 A044:DA46 A045:DA65 A047:DA42 A049:DV11 A050:DV10 A058:DV12 A060:DV23 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DA61 A073:DA41 A074:DV14 A075:DV22 A076:DA53 A082:DA58 A083:DV08 A085:DV05 A088:DA54	F	2025-10-31T03:25:14.000	0.6309309744519427	[240.06..241.94GHz,3904.30kHz,6.7mJy/beam@10km/s,438.8uJy/beam@native, XX YY] U [241.86..243.74GHz,3904.30kHz,6.7mJy/beam@10km/s,439.3uJy/beam@native, XX YY] U [256.06..257.94GHz,3904.30kHz,6.3mJy/beam@10km/s,427.8uJy/beam@native, XX YY] U [257.86..259.74GHz,3904.30kHz,6.3mJy/beam@10km/s,428.2uJy/beam@native, XX YY]	258.80001373873426	4538.887103577384	ALMA	ALMA and JWST Identification of Faint Dusty Star-forming Galaxies up to z ∼ 8 and Their Connection with Other Galaxy Populations Active galactic nuclei-heated dust revealed in ''little red dots'' COSMOS-3D: Dense Circumnuclear Gas Across Black Hole Growth Phases at z ∼ 3 PANORAMIC: Discovery of an ultra-massive grand-design spiral galaxy at z ∼ 5.2 Probing infrared eXcess to investigate early-Universe dust (PIXIEDust) The ALPINE-CRISTAL-JWST Survey: JWST/IFU Optical Observations for 18 Main-sequence Galaxies at z = 4─6	Bakx, Tom J. L. C. Delvecchio, I. Faisst, A. L. Li, Zi-Jian Xiao, Mengyuan Zavala, Jorge A.	Bakx, Tom J. L. C.; Algera, Hiddo S. B.; Jolly, Jean-Baptiste; Esmerian, Clarke; Knudsen, Kirsten; Sommovigo, Laura; Witstok, Joris; Carniani, Stefano; Chen, Jianhang; Eales, Stephen; Ferrara, Andrea; Fudamoto, Yoshinobu; Hagimoto, Masato; Hashimoto, Takuya; Inami, Hanae; Inoue, Akio K.; Khouri, Theo; Mitsuhashi, Ikki; Nyman, Gunnar; Olander, Gustav; Serjeant, Stephen; Smit, Renske; Yoon, Ilsang; Zavala, Jorge; Aalto, Susanne; Casey, Caitlin M.; Tamura, Yoichi; Vlemmings, Wouter Delvecchio, I.; Daddi, E.; Magnelli, B.; Elbaz, D.; Giavalisco, M.; Traina, A.; Lanzuisi, G.; Akins, H. B.; Belli, S.; Casey, C. M.; Gentile, F.; Gruppioni, C.; Pozzi, F.; Zamorani, G. Faisst, A. L.; Fujimoto, S.; Tsujita, A.; Wang, W.; Nezhad, N.; Loiacono, F.; Übler, H.; Béthermin, M.; Cassata, P.; Dessauges-Zavadsky, M.; Herrera-Camus, R.; Schaerer, D.; Silverman, J. D.; Yan, L.; Aravena, M.; De Looze, I.; Förster Schreiber, N. M.; González-López, J.; Spilker, J.; Tadaki, K.; Casey, C. M.; Franco, M.; Harish, S.; McCracken, H. J.;	Despite the implied presence of dust through reddened UV emission in high-redshift galaxies, no dust emission has been detected in the (sub)millimetre regime beyond <inline-formula><tex-math>$z &gt; 8.3$</tex-math></inline-formula>. This study combines around 200 h of Atacama Large Millimetre/submillimetre Array (ALMA) and Northern Extended Millimetre Array (NOEMA) observations on 10 <inline-formula><tex-math>$z &gt; 8$</tex-math></inline-formula> galaxies, revealing no significant dust emission down to a <inline-formula><tex-math>$1 \sigma$</tex-math></inline-formula> depth of 2.0, 2.0, and <inline-formula><tex-math>$1.5 \, \mu$</tex-math></inline-formula>Jy at rest-frame 158, 88 <inline-formula><tex-math>$\mu$</tex-math></inline-formula>m, and across all the data, respectively. This constrains average dust masses to be below <inline-formula><tex-math>$&lt; 10^{5}$</tex-math></inline-formula> M<inline-formula><tex-math>$_{\odot }$</tex-math></inline-formula> at <inline-formula><tex-math>$3 \sigma$</tex-math>	2025	To trace the evolution of galaxies through cosmic time, a multi-band survey including sub-mm data is crucial, especially since recent small-area blank-field surveys show a considerable number of dust-obscured sources even into the Epoch of Reionization at z=6. We propose to carry out a 0.18deg2 blank-field survey at 1.1mm in the COSMOS field, CHAMPS, 3x the area of existing ALMA surveys, to push our understanding of the dusty Universe. CHAMPS complements deep, high-resolution MIRI and NIRCam observations from two JWST Cycle 1 programs with essential sub-mm observations. This will enable us to construct UV-FIR multiwavelength SEDs of ~30,000 MIRI-detected sources, including ~1200 bright, dusty sources directly detected with ALMA out to z~6, and an additional ~120,000 sources with NIRCam-only detections from stacking. With this large area we will find dusty high-z galaxies and provide limits to sub-mm properties of fainter sources via stacking. This program provides a unique opportunity to combine cutting-edge	S20_2_a_06_TM1	Rhodes, Jason; Franco, Maximilien; Maraston, Claudia; Valentino, Francesco; Sanders, David; Shuntov, Marko; Wilkins, Stephen; Martin, Crystal; Bagley, Micaela; Drakos, Nicole; Robertson, Brant; Mercier, Wilfried; Hemmati, Shoubaneh; Mainieri, Vincenzo; Suzuki, Tomoko; Rodighiero, Giulia; Renzini, Alvio; Fujimoto, Seiji; Darvish, Behnam; Akins, Hollis; McCracken, Henry; Kalita, Boris Sindhu; Paquereau, Louise; Gozaliasl, Ghassem; Magdis, Georgios; Enia, Andrea Francesco Maria; González López, Jorge; Gentile, Fabrizio; Scoville, Nick; Champagne, Jaclyn; Algera, Hiddo; Massey, Richard; Ilbert, Olivier; Manning, Sinclaire; Talia, Margherita; Cooke, Kevin; Hayward, Christopher; Vardoulaki, Eleni; Lambrides, Erini; Bongiorno, Angela; Long, Arianna; McKinney, Jed; Nayyeri, Hooshang; Gomez-Guijarro, Carlos; Trakhtenbrot, Benny; Davidzon , Iary; Mobasher, Bahram; Jin, Shuowen; Battisti, Andrew; Koekemoer, Anton; Sparre, Martin; Sommovigo, Laura; Moutard, Thibaud; Onoue, Masafusa; Jahnke, Knud; Kokorev, Vasily; Kashino	6.310832774888936	0.2167077351801419	1.9318154	uid://A001/X3645/Xd3	uid://A001/X3645/Xd4	uid://A002/X11edb41/X10373	The COSMOS High-z ALMA-MIRI Population Survey (CHAMPS): A Wide-Area Comprehensive Survey of the Dusty Universe	L	TARGET	T	8.587340975876911	T	2025A&A...696A.156X 2025A&A...704A.313D 2026ApJ...998L..36Z 2026ApJ..1002....9L 2026ApJS..282...19F 2026MNRAS.546f2284B	Lyman Break Galaxies (LBG);null	Galaxy evolution	afaisst	Faisst, Andreas	3904.296875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00564.S	ALMA	JAO	ALMA	uid://A001/X134b/Xd.source.2MASS_J16142091-1906051.spw.31	cube	2		2MASS_J16142091-1906051	243.58713750005026	-19.101425000010735	0.004741221551943115	Polygon ICRS 243.589167 -19.100032 243.589567 -19.100835 243.589626 -19.101722 243.589523 -19.102158 243.589256 -19.102695 243.588612 -19.103343 243.588206 -19.103570 243.587608 -19.103754 243.586667 -19.103754 243.585793 -19.103427 243.585108 -19.102818 243.584708 -19.102015 243.584649 -19.101128 243.584939 -19.100283 243.585205 -19.099914 243.585663 -19.099507 243.586514 -19.099129 243.586980 -19.099059 243.587608 -19.099096 243.588482 -19.099423			1920	1	2	0.3181644136036313	58593.390178	58594.395147	145.152	145.152	8.945064114955135E-4	8.9953584632621E-4	296907.1797298963	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X134b/Xd	application/x-votable+xml; content=datalink		2018.1.00564.S	Public	355.3003791912594	22.52788328878749	7	3.029975430270911E-9	1.875E9	A001:DA44 A002:DA51 A007:DV05 A008:DV07 A010:DV13 A011:DV21 A015:DA64 A016:DV11 A022:DV23 A023:DA42 A024:DA49 A025:DA46 A027:DV06 A034:DA50 A035:DA43 A036:DA45 A040:DA55 A042:DV08 A043:DA60 A044:DV03 A045:DV01 A047:DV15 A048:DV02 A049:DA47 A058:DA41 A060:DV17 A062:DV10 A066:DV04 A068:DA65 A069:DV16 A070:DA62 A072:DV20 A073:DA59 A074:DV09 A082:DA54 A085:DA48 A086:DA58 A087:DV19 A088:DV24 A089:DA56 A090:DV25 A091:DA61 A092:DV12 A094:DV14 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2020-08-28T04:50:08.000	0.3181644136036313	[333.27..335.15GHz,1128.91kHz,4.5mJy/beam@10km/s,345.8uJy/beam@native, XX YY] U [335.16..337.03GHz,1128.91kHz,4.6mJy/beam@10km/s,359.4uJy/beam@native, XX YY] U [345.28..347.16GHz,976.56kHz,4.5mJy/beam@10km/s,356.7uJy/beam@native, XX YY] U [347.16..349.03GHz,1128.91kHz,4.5mJy/beam@10km/s,357.2uJy/beam@native, XX YY]	334.211541351999	847.820872585631	ALMA	Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars Benchmarking pre-main sequence stellar evolutionary tracks using disk-based dynamical stellar masses Bridging the Gap between Protoplanetary and Debris Disks: Separate Evolution of Millimeter and Micrometer-sized Dust Extending the ALMA Census of Circumstellar Disks in the Upper Scorpius OB Association Observational constraints on evolution of dust disc properties in Upper Scorpius Radiative Transfer Modeling of a Shadowed Protoplanetary Disk Assisted by a Neural Network The <SUP>12</SUP>CO gas structures of protoplanetary disks in the Upper Scorpius region	Ansdell, M. Carpenter, John M. Michel, Arnaud Pinilla, Paola Williams, Jonathan P. Zallio, Luigi	Ansdell, M.; Gaidos, E.; Hedges, C.; Tazzari, M.; Kraus, A. L.; Wyatt, M. C.; Kennedy, G. M.; Williams, J. P.; Mann, A. W.; Angelo, I.; Dûchene, G.; Mamajek, E. E.; Carpenter, J.; Esplin, T. L.; Rizzuto, A. C. Carpenter, John M.; Esplin, Taran L.; Luhman, Kevin L.; Mamajek, Eric E.; Andrews, Sean M. Michel, Arnaud; van der Marel, Nienke; Matthews, Brenda C. Pinilla, Paola; Sierra, Anibal; Kurtovic, Nicolas T.; Anania, Rossella; Andrews, Sean; Carpenter, John; Guerra-Alvarado, Osmar; Long, Feng; Marino, Sebastian; Vioque, Miguel; Zhang, Ke Williams, Jonathan P.; Benisty, Myriam; Ginski, Christian; Lodato, Giuseppe; Vincent, Maria Zallio, Luigi; Rosotti, Giovanni P.; Vioque, Miguel; Miotello, Anna; Andrews, Sean M.; Manara, Carlo F.; Carpenter, John M.; Empey, Aaron; Kurtovic, Nicolás T.; Law, Charles J.; Longarini, Cristiano; Paneque-Carreño, Teresa; Teague, Richard; Villenave, Marion; Yen, Hsi-Wei; Zagaria, Francesco Zallio, Luigi; Vioque, Miguel; Andrews, Sean M.; Empey, Aaron; Rosotti, Giovanni P.; Miotello	Dippers are a common class of young variable star exhibiting day-long dimmings with depths of up to several tens of per cent. A standard explanation is that dippers host nearly edge-on (i<SUB>d</SUB> ≈ 70°) protoplanetary discs that allow close-in (&lt;1 au) dust lifted slightly out of the mid-plane to partially occult the star. The identification of a face-on dipper disc and growing evidence of inner disc misalignments brings this scenario into question. Thus, we uniformly (re)derive the inclinations of 24 dipper discs resolved with (sub-)mm interferometry from ALMA. We find that dipper disc inclinations are consistent with an isotropic distribution over i<SUB>d</SUB> ≈ 0-75°, above which the occurrence rate declines (likely an observational selection effect due to optically thick disc mid-planes blocking their host stars). These findings indicate that the dipper phenomenon is unrelated to the outer (&gt;10 au) disc resolved by ALMA and that inner disc misalignments may be common during the protoplanetary ph	2020	The Upper Scorpius OB Association plays a central role in establishing the evolutionary history of circumstellar disks. As the closest OB association and at an advanced age of 11 Myr, it is the benchmark region in which to establish the disk properties at the end stage of disk evolution. In the past few years, members of our team led an optical and near-infrared spectroscopic campaign to identify new members of Upper Sco that expanded the disk population to 260 stars with spectral types between G0 and M5, which nearly triples the number of previously known disks in Upper Sco. We propose to complete the ALMA census of Upper Sco by surveying the newly identified disks in the dust continuum and CO J=3-2. The full survey is anticipated to yield 140 continuum detections and 65 CO detections, which will provide an unprecedented census of the final stages of disk evolution. Our specific goal is to determine if dust depletes faster around low-mass stars as suggested by recent studies. More broadly, by tripling the nu	2MASS_J1_a_07_TM1	Luhman, Kevin; Mamajek, Eric; Esplin, Taran;	4.484828301022586	0.17732271304882513	0.7372181	uid://A001/X134b/Xc	uid://A001/X134b/Xd	uid://A002/Xdb1b89/X4df2	Completing the Census of Disks in the Upper Sco OB Association	S	TARGET	T	4.305070096091297	T	2020MNRAS.492..572A 2021ApJ...921...72M 2025ApJ...978..117C 2025ApJ...991..176W 2025MNRAS.543.2723P 2026A&A...705A..49Z 2026A&A...708L...1Z	Debris disks;Disks around low-mass stars	Disks and planet formation	carp	Carpenter, John	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00564.S	ALMA	JAO	ALMA	uid://A001/X134b/Xd.source.2MASS_J16142091-1906051.spw.27	cube	2		2MASS_J16142091-1906051	243.58713750005026	-19.101425000010735	0.004741221551943115	Polygon ICRS 243.589167 -19.100032 243.589567 -19.100835 243.589626 -19.101722 243.589523 -19.102158 243.589256 -19.102695 243.588612 -19.103343 243.588206 -19.103570 243.587608 -19.103754 243.586667 -19.103754 243.585793 -19.103427 243.585108 -19.102818 243.584708 -19.102015 243.584649 -19.101128 243.584939 -19.100283 243.585205 -19.099914 243.585663 -19.099507 243.586514 -19.099129 243.586980 -19.099059 243.587608 -19.099096 243.588482 -19.099423			1920	1	2	0.3181644136036313	58593.390178	58594.395147	145.152	145.152	8.589226610955972E-4	8.635588746809823E-4	307547.52033098397	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X134b/Xd	application/x-votable+xml; content=datalink		2018.1.00564.S	Public	355.3003791912594	22.52788328878749	7	2.793078791920988E-9	1.875E9	A001:DA44 A002:DA51 A007:DV05 A008:DV07 A010:DV13 A011:DV21 A015:DA64 A016:DV11 A022:DV23 A023:DA42 A024:DA49 A025:DA46 A027:DV06 A034:DA50 A035:DA43 A036:DA45 A040:DA55 A042:DV08 A043:DA60 A044:DV03 A045:DV01 A047:DV15 A048:DV02 A049:DA47 A058:DA41 A060:DV17 A062:DV10 A066:DV04 A068:DA65 A069:DV16 A070:DA62 A072:DV20 A073:DA59 A074:DV09 A082:DA54 A085:DA48 A086:DA58 A087:DV19 A088:DV24 A089:DA56 A090:DV25 A091:DA61 A092:DV12 A094:DV14 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2020-08-28T04:50:08.000	0.3181644136036313	[333.27..335.15GHz,1128.91kHz,4.5mJy/beam@10km/s,345.8uJy/beam@native, XX YY] U [335.16..337.03GHz,1128.91kHz,4.6mJy/beam@10km/s,359.4uJy/beam@native, XX YY] U [345.28..347.16GHz,976.56kHz,4.5mJy/beam@10km/s,356.7uJy/beam@native, XX YY] U [347.16..349.03GHz,1128.91kHz,4.5mJy/beam@10km/s,357.2uJy/beam@native, XX YY]	348.09618992352205	847.820872585631	ALMA	Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars Benchmarking pre-main sequence stellar evolutionary tracks using disk-based dynamical stellar masses Bridging the Gap between Protoplanetary and Debris Disks: Separate Evolution of Millimeter and Micrometer-sized Dust Extending the ALMA Census of Circumstellar Disks in the Upper Scorpius OB Association Observational constraints on evolution of dust disc properties in Upper Scorpius Radiative Transfer Modeling of a Shadowed Protoplanetary Disk Assisted by a Neural Network The <SUP>12</SUP>CO gas structures of protoplanetary disks in the Upper Scorpius region	Ansdell, M. Carpenter, John M. Michel, Arnaud Pinilla, Paola Williams, Jonathan P. Zallio, Luigi	Ansdell, M.; Gaidos, E.; Hedges, C.; Tazzari, M.; Kraus, A. L.; Wyatt, M. C.; Kennedy, G. M.; Williams, J. P.; Mann, A. W.; Angelo, I.; Dûchene, G.; Mamajek, E. E.; Carpenter, J.; Esplin, T. L.; Rizzuto, A. C. Carpenter, John M.; Esplin, Taran L.; Luhman, Kevin L.; Mamajek, Eric E.; Andrews, Sean M. Michel, Arnaud; van der Marel, Nienke; Matthews, Brenda C. Pinilla, Paola; Sierra, Anibal; Kurtovic, Nicolas T.; Anania, Rossella; Andrews, Sean; Carpenter, John; Guerra-Alvarado, Osmar; Long, Feng; Marino, Sebastian; Vioque, Miguel; Zhang, Ke Williams, Jonathan P.; Benisty, Myriam; Ginski, Christian; Lodato, Giuseppe; Vincent, Maria Zallio, Luigi; Rosotti, Giovanni P.; Vioque, Miguel; Miotello, Anna; Andrews, Sean M.; Manara, Carlo F.; Carpenter, John M.; Empey, Aaron; Kurtovic, Nicolás T.; Law, Charles J.; Longarini, Cristiano; Paneque-Carreño, Teresa; Teague, Richard; Villenave, Marion; Yen, Hsi-Wei; Zagaria, Francesco Zallio, Luigi; Vioque, Miguel; Andrews, Sean M.; Empey, Aaron; Rosotti, Giovanni P.; Miotello	Dippers are a common class of young variable star exhibiting day-long dimmings with depths of up to several tens of per cent. A standard explanation is that dippers host nearly edge-on (i<SUB>d</SUB> ≈ 70°) protoplanetary discs that allow close-in (&lt;1 au) dust lifted slightly out of the mid-plane to partially occult the star. The identification of a face-on dipper disc and growing evidence of inner disc misalignments brings this scenario into question. Thus, we uniformly (re)derive the inclinations of 24 dipper discs resolved with (sub-)mm interferometry from ALMA. We find that dipper disc inclinations are consistent with an isotropic distribution over i<SUB>d</SUB> ≈ 0-75°, above which the occurrence rate declines (likely an observational selection effect due to optically thick disc mid-planes blocking their host stars). These findings indicate that the dipper phenomenon is unrelated to the outer (&gt;10 au) disc resolved by ALMA and that inner disc misalignments may be common during the protoplanetary ph	2020	The Upper Scorpius OB Association plays a central role in establishing the evolutionary history of circumstellar disks. As the closest OB association and at an advanced age of 11 Myr, it is the benchmark region in which to establish the disk properties at the end stage of disk evolution. In the past few years, members of our team led an optical and near-infrared spectroscopic campaign to identify new members of Upper Sco that expanded the disk population to 260 stars with spectral types between G0 and M5, which nearly triples the number of previously known disks in Upper Sco. We propose to complete the ALMA census of Upper Sco by surveying the newly identified disks in the dust continuum and CO J=3-2. The full survey is anticipated to yield 140 continuum detections and 65 CO detections, which will provide an unprecedented census of the final stages of disk evolution. Our specific goal is to determine if dust depletes faster around low-mass stars as suggested by recent studies. More broadly, by tripling the nu	2MASS_J1_a_07_TM1	Luhman, Kevin; Mamajek, Eric; Esplin, Taran;	4.539050995329133	0.17732271304882513	0.7372181	uid://A001/X134b/Xc	uid://A001/X134b/Xd	uid://A002/Xdb1b89/X4df2	Completing the Census of Disks in the Upper Sco OB Association	S	TARGET	T	4.305070096091297	T	2020MNRAS.492..572A 2021ApJ...921...72M 2025ApJ...978..117C 2025ApJ...991..176W 2025MNRAS.543.2723P 2026A&A...705A..49Z 2026A&A...708L...1Z	Debris disks;Disks around low-mass stars	Disks and planet formation	carp	Carpenter, John	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00564.S	ALMA	JAO	ALMA	uid://A001/X134b/Xd.source.2MASS_J16142091-1906051.spw.25	cube	2		2MASS_J16142091-1906051	243.58713750005026	-19.101425000010735	0.004741221551943115	Polygon ICRS 243.589167 -19.100032 243.589567 -19.100835 243.589626 -19.101722 243.589523 -19.102158 243.589256 -19.102695 243.588612 -19.103343 243.588206 -19.103570 243.587608 -19.103754 243.586667 -19.103754 243.585793 -19.103427 243.585108 -19.102818 243.584708 -19.102015 243.584649 -19.101128 243.584939 -19.100283 243.585205 -19.099914 243.585663 -19.099507 243.586514 -19.099129 243.586980 -19.099059 243.587608 -19.099096 243.588482 -19.099423			3840	1	2	0.3181644136036313	58593.390178	58594.395147	145.152	145.152	8.635634372829337E-4	8.682512494673138E-4	353603.53547997907	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X134b/Xd	application/x-votable+xml; content=datalink		2018.1.00564.S	Public	355.3003791912594	22.52788328878749	7	2.44241244223371E-9	1.875E9	A001:DA44 A002:DA51 A007:DV05 A008:DV07 A010:DV13 A011:DV21 A015:DA64 A016:DV11 A022:DV23 A023:DA42 A024:DA49 A025:DA46 A027:DV06 A034:DA50 A035:DA43 A036:DA45 A040:DA55 A042:DV08 A043:DA60 A044:DV03 A045:DV01 A047:DV15 A048:DV02 A049:DA47 A058:DA41 A060:DV17 A062:DV10 A066:DV04 A068:DA65 A069:DV16 A070:DA62 A072:DV20 A073:DA59 A074:DV09 A082:DA54 A085:DA48 A086:DA58 A087:DV19 A088:DV24 A089:DA56 A090:DV25 A091:DA61 A092:DV12 A094:DV14 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2020-08-28T04:50:08.000	0.3181644136036313	[333.27..335.15GHz,1128.91kHz,4.5mJy/beam@10km/s,345.8uJy/beam@native, XX YY] U [335.16..337.03GHz,1128.91kHz,4.6mJy/beam@10km/s,359.4uJy/beam@native, XX YY] U [345.28..347.16GHz,976.56kHz,4.5mJy/beam@10km/s,356.7uJy/beam@native, XX YY] U [347.16..349.03GHz,1128.91kHz,4.5mJy/beam@10km/s,357.2uJy/beam@native, XX YY]	346.2202474048215	847.820872585631	ALMA	Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars Benchmarking pre-main sequence stellar evolutionary tracks using disk-based dynamical stellar masses Bridging the Gap between Protoplanetary and Debris Disks: Separate Evolution of Millimeter and Micrometer-sized Dust Extending the ALMA Census of Circumstellar Disks in the Upper Scorpius OB Association Observational constraints on evolution of dust disc properties in Upper Scorpius Radiative Transfer Modeling of a Shadowed Protoplanetary Disk Assisted by a Neural Network The <SUP>12</SUP>CO gas structures of protoplanetary disks in the Upper Scorpius region	Ansdell, M. Carpenter, John M. Michel, Arnaud Pinilla, Paola Williams, Jonathan P. Zallio, Luigi	Ansdell, M.; Gaidos, E.; Hedges, C.; Tazzari, M.; Kraus, A. L.; Wyatt, M. C.; Kennedy, G. M.; Williams, J. P.; Mann, A. W.; Angelo, I.; Dûchene, G.; Mamajek, E. E.; Carpenter, J.; Esplin, T. L.; Rizzuto, A. C. Carpenter, John M.; Esplin, Taran L.; Luhman, Kevin L.; Mamajek, Eric E.; Andrews, Sean M. Michel, Arnaud; van der Marel, Nienke; Matthews, Brenda C. Pinilla, Paola; Sierra, Anibal; Kurtovic, Nicolas T.; Anania, Rossella; Andrews, Sean; Carpenter, John; Guerra-Alvarado, Osmar; Long, Feng; Marino, Sebastian; Vioque, Miguel; Zhang, Ke Williams, Jonathan P.; Benisty, Myriam; Ginski, Christian; Lodato, Giuseppe; Vincent, Maria Zallio, Luigi; Rosotti, Giovanni P.; Vioque, Miguel; Miotello, Anna; Andrews, Sean M.; Manara, Carlo F.; Carpenter, John M.; Empey, Aaron; Kurtovic, Nicolás T.; Law, Charles J.; Longarini, Cristiano; Paneque-Carreño, Teresa; Teague, Richard; Villenave, Marion; Yen, Hsi-Wei; Zagaria, Francesco Zallio, Luigi; Vioque, Miguel; Andrews, Sean M.; Empey, Aaron; Rosotti, Giovanni P.; Miotello	Dippers are a common class of young variable star exhibiting day-long dimmings with depths of up to several tens of per cent. A standard explanation is that dippers host nearly edge-on (i<SUB>d</SUB> ≈ 70°) protoplanetary discs that allow close-in (&lt;1 au) dust lifted slightly out of the mid-plane to partially occult the star. The identification of a face-on dipper disc and growing evidence of inner disc misalignments brings this scenario into question. Thus, we uniformly (re)derive the inclinations of 24 dipper discs resolved with (sub-)mm interferometry from ALMA. We find that dipper disc inclinations are consistent with an isotropic distribution over i<SUB>d</SUB> ≈ 0-75°, above which the occurrence rate declines (likely an observational selection effect due to optically thick disc mid-planes blocking their host stars). These findings indicate that the dipper phenomenon is unrelated to the outer (&gt;10 au) disc resolved by ALMA and that inner disc misalignments may be common during the protoplanetary ph	2020	The Upper Scorpius OB Association plays a central role in establishing the evolutionary history of circumstellar disks. As the closest OB association and at an advanced age of 11 Myr, it is the benchmark region in which to establish the disk properties at the end stage of disk evolution. In the past few years, members of our team led an optical and near-infrared spectroscopic campaign to identify new members of Upper Sco that expanded the disk population to 260 stars with spectral types between G0 and M5, which nearly triples the number of previously known disks in Upper Sco. We propose to complete the ALMA census of Upper Sco by surveying the newly identified disks in the dust continuum and CO J=3-2. The full survey is anticipated to yield 140 continuum detections and 65 CO detections, which will provide an unprecedented census of the final stages of disk evolution. Our specific goal is to determine if dust depletes faster around low-mass stars as suggested by recent studies. More broadly, by tripling the nu	2MASS_J1_a_07_TM1	Luhman, Kevin; Mamajek, Eric; Esplin, Taran;	4.544826228065722	0.17732271304882513	0.7372181	uid://A001/X134b/Xc	uid://A001/X134b/Xd	uid://A002/Xdb1b89/X4df2	Completing the Census of Disks in the Upper Sco OB Association	S	TARGET	T	4.305070096091297	T	2020MNRAS.492..572A 2021ApJ...921...72M 2025ApJ...978..117C 2025ApJ...991..176W 2025MNRAS.543.2723P 2026A&A...705A..49Z 2026A&A...708L...1Z	Debris disks;Disks around low-mass stars	Disks and planet formation	carp	Carpenter, John	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.00564.S	ALMA	JAO	ALMA	uid://A001/X134b/Xd.source.2MASS_J16142091-1906051.spw.29	cube	2		2MASS_J16142091-1906051	243.58713750005026	-19.101425000010735	0.004741221551943115	Polygon ICRS 243.589167 -19.100032 243.589567 -19.100835 243.589626 -19.101722 243.589523 -19.102158 243.589256 -19.102695 243.588612 -19.103343 243.588206 -19.103570 243.587608 -19.103754 243.586667 -19.103754 243.585793 -19.103427 243.585108 -19.102818 243.584708 -19.102015 243.584649 -19.101128 243.584939 -19.100283 243.585205 -19.099914 243.585663 -19.099507 243.586514 -19.099129 243.586980 -19.099059 243.587608 -19.099096 243.588482 -19.099423			1920	1	2	0.3181644136036313	58593.390178	58594.395147	145.152	145.152	8.89506250568499E-4	8.944794588910997E-4	298576.1772010369	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X134b/Xd	application/x-votable+xml; content=datalink		2018.1.00564.S	Public	355.3003791912594	22.52788328878749	7	2.9961016963052784E-9	1.875E9	A001:DA44 A002:DA51 A007:DV05 A008:DV07 A010:DV13 A011:DV21 A015:DA64 A016:DV11 A022:DV23 A023:DA42 A024:DA49 A025:DA46 A027:DV06 A034:DA50 A035:DA43 A036:DA45 A040:DA55 A042:DV08 A043:DA60 A044:DV03 A045:DV01 A047:DV15 A048:DV02 A049:DA47 A058:DA41 A060:DV17 A062:DV10 A066:DV04 A068:DA65 A069:DV16 A070:DA62 A072:DV20 A073:DA59 A074:DV09 A082:DA54 A085:DA48 A086:DA58 A087:DV19 A088:DV24 A089:DA56 A090:DV25 A091:DA61 A092:DV12 A094:DV14 T701:PM02 T702:PM03 T703:PM01 T704:PM04	F	2020-08-28T04:50:08.000	0.3181644136036313	[333.27..335.15GHz,1128.91kHz,4.5mJy/beam@10km/s,345.8uJy/beam@native, XX YY] U [335.16..337.03GHz,1128.91kHz,4.6mJy/beam@10km/s,359.4uJy/beam@native, XX YY] U [345.28..347.16GHz,976.56kHz,4.5mJy/beam@10km/s,356.7uJy/beam@native, XX YY] U [347.16..349.03GHz,1128.91kHz,4.5mJy/beam@10km/s,357.2uJy/beam@native, XX YY]	336.09550366784674	847.820872585631	ALMA	Are inner disc misalignments common? ALMA reveals an isotropic outer disc inclination distribution for young dipper stars Benchmarking pre-main sequence stellar evolutionary tracks using disk-based dynamical stellar masses Bridging the Gap between Protoplanetary and Debris Disks: Separate Evolution of Millimeter and Micrometer-sized Dust Extending the ALMA Census of Circumstellar Disks in the Upper Scorpius OB Association Observational constraints on evolution of dust disc properties in Upper Scorpius Radiative Transfer Modeling of a Shadowed Protoplanetary Disk Assisted by a Neural Network The <SUP>12</SUP>CO gas structures of protoplanetary disks in the Upper Scorpius region	Ansdell, M. Carpenter, John M. Michel, Arnaud Pinilla, Paola Williams, Jonathan P. Zallio, Luigi	Ansdell, M.; Gaidos, E.; Hedges, C.; Tazzari, M.; Kraus, A. L.; Wyatt, M. C.; Kennedy, G. M.; Williams, J. P.; Mann, A. W.; Angelo, I.; Dûchene, G.; Mamajek, E. E.; Carpenter, J.; Esplin, T. L.; Rizzuto, A. C. Carpenter, John M.; Esplin, Taran L.; Luhman, Kevin L.; Mamajek, Eric E.; Andrews, Sean M. Michel, Arnaud; van der Marel, Nienke; Matthews, Brenda C. Pinilla, Paola; Sierra, Anibal; Kurtovic, Nicolas T.; Anania, Rossella; Andrews, Sean; Carpenter, John; Guerra-Alvarado, Osmar; Long, Feng; Marino, Sebastian; Vioque, Miguel; Zhang, Ke Williams, Jonathan P.; Benisty, Myriam; Ginski, Christian; Lodato, Giuseppe; Vincent, Maria Zallio, Luigi; Rosotti, Giovanni P.; Vioque, Miguel; Miotello, Anna; Andrews, Sean M.; Manara, Carlo F.; Carpenter, John M.; Empey, Aaron; Kurtovic, Nicolás T.; Law, Charles J.; Longarini, Cristiano; Paneque-Carreño, Teresa; Teague, Richard; Villenave, Marion; Yen, Hsi-Wei; Zagaria, Francesco Zallio, Luigi; Vioque, Miguel; Andrews, Sean M.; Empey, Aaron; Rosotti, Giovanni P.; Miotello	Dippers are a common class of young variable star exhibiting day-long dimmings with depths of up to several tens of per cent. A standard explanation is that dippers host nearly edge-on (i<SUB>d</SUB> ≈ 70°) protoplanetary discs that allow close-in (&lt;1 au) dust lifted slightly out of the mid-plane to partially occult the star. The identification of a face-on dipper disc and growing evidence of inner disc misalignments brings this scenario into question. Thus, we uniformly (re)derive the inclinations of 24 dipper discs resolved with (sub-)mm interferometry from ALMA. We find that dipper disc inclinations are consistent with an isotropic distribution over i<SUB>d</SUB> ≈ 0-75°, above which the occurrence rate declines (likely an observational selection effect due to optically thick disc mid-planes blocking their host stars). These findings indicate that the dipper phenomenon is unrelated to the outer (&gt;10 au) disc resolved by ALMA and that inner disc misalignments may be common during the protoplanetary ph	2020	The Upper Scorpius OB Association plays a central role in establishing the evolutionary history of circumstellar disks. As the closest OB association and at an advanced age of 11 Myr, it is the benchmark region in which to establish the disk properties at the end stage of disk evolution. In the past few years, members of our team led an optical and near-infrared spectroscopic campaign to identify new members of Upper Sco that expanded the disk population to 260 stars with spectral types between G0 and M5, which nearly triples the number of previously known disks in Upper Sco. We propose to complete the ALMA census of Upper Sco by surveying the newly identified disks in the dust continuum and CO J=3-2. The full survey is anticipated to yield 140 continuum detections and 65 CO detections, which will provide an unprecedented census of the final stages of disk evolution. Our specific goal is to determine if dust depletes faster around low-mass stars as suggested by recent studies. More broadly, by tripling the nu	2MASS_J1_a_07_TM1	Luhman, Kevin; Mamajek, Eric; Esplin, Taran;	4.647481552889137	0.17732271304882513	0.7372181	uid://A001/X134b/Xc	uid://A001/X134b/Xd	uid://A002/Xdb1b89/X4df2	Completing the Census of Disks in the Upper Sco OB Association	S	TARGET	T	4.305070096091297	T	2020MNRAS.492..572A 2021ApJ...921...72M 2025ApJ...978..117C 2025ApJ...991..176W 2025MNRAS.543.2723P 2026A&A...705A..49Z 2026A&A...708L...1Z	Debris disks;Disks around low-mass stars	Disks and planet formation	carp	Carpenter, John	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00927.S	ALMA	JAO	ALMA	uid://A001/X159b/X21.source.Betelgeuse.spw.22	cube	2		Betelgeuse	88.79310812363141	7.407132905681428	0.012544144592574946	Circle ICRS 88.793108 7.407133 0.006272			1024	1	2	6.030335428482976	59608.037179	59608.046372	635.04	635.04	0.0012977076507207893	0.0013090306460292202	118130.12294552897	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X159b/X21	application/x-votable+xml; content=datalink		2021.1.00927.S	Public	199.78726414834546	-8.958414216879447	6	1.0984151912432457E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N606:CM06	F	2023-02-01T11:12:30.000	6.030335428482976	[211.08..213.07GHz,1938.48kHz,12.7mJy/beam@10km/s,752.5uJy/beam@native, XX YY] U [212.93..214.93GHz,1938.48kHz,11.6mJy/beam@10km/s,690uJy/beam@native, XX YY] U [227.13..229.13GHz,1938.48kHz,11.4mJy/beam@10km/s,701.8uJy/beam@native, XX YY] U [229.02..231.02GHz,1938.48kHz,12.4mJy/beam@10km/s,771uJy/beam@native, XX YY]	230.01780807044787	2537.81550822763	ALMA						One year ago the visual dimming of Betelgeuse caused a cascade of public news, following the suggestion of an imminent core-collapse. Other hypotheses formulated to explain this extraordinary event were the formation of large cold spots on the stellar photosphere, or an increased extinction along the line of sight. Betelgeuse may have undergone an increased mass-loss episode that favours dust grain formation, consistently with the erratic stellar activity of evolved massive stars. We propose a monitoring programme with ACA in Bands 3, 6 and 7, to test the role of dust in the recent visual dimming and to perform an unprecedented study of the dust properties and formation cycle. We request calibration-limited observations (with photometric uncertainty of 5%) to derive light curves at five different frequencies and, additionally, spectral indices to disentangle different emission mechanisms contributing to the sub-mm wavelengths. With these observations we will gain a rare insight into dust processes and mass-lo	Betelgeu_f_06_7M	Etoka, Sandra; Scicluna, Peter; Richards, Anita; Phillips, Neil; Mairs, Steve; Wong, Ka Tat; de Wit, Willem-Jan; Menten, Karl; Lundgren, Andreas; Jones, Olivia; Mehner, Andrea; De Breuck, Carlos; Kemper, Ciska; Baade, Dietrich; Dharmawardena, Thavisha; Trejo, Alfonso; Montarges, Miguel; Randall, Suzanna; Humphreys, Elizabeth;	12.447447693958958	0.3632221299301987	1.8	uid://A001/X159b/X20	uid://A001/X159b/X21	uid://A002/Xf53eeb/X1c0f3	The fall and rise of Betelgeuse: diving in its ejecta with ACA	S	TARGET	T	33.524562462203136	F		Hypergiants;null	Stars and stellar evolution	cagliozzo	Agliozzo, Claudia	1938.4765625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00927.S	ALMA	JAO	ALMA	uid://A001/X159b/X21.source.Betelgeuse.spw.16	cube	2		Betelgeuse	88.79310812363141	7.407132905681428	0.012544144592574946	Circle ICRS 88.793108 7.407133 0.006272			1024	1	2	6.030335428482976	59608.037179	59608.046372	635.04	635.04	0.0014069917608312635	0.0014203119360991945	109905.37077739295	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X159b/X21	application/x-votable+xml; content=datalink		2021.1.00927.S	Public	199.78726414834546	-8.958414216879447	6	1.2921565774582323E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N606:CM06	F	2023-02-01T11:12:30.000	6.030335428482976	[211.08..213.07GHz,1938.48kHz,12.7mJy/beam@10km/s,752.5uJy/beam@native, XX YY] U [212.93..214.93GHz,1938.48kHz,11.6mJy/beam@10km/s,690uJy/beam@native, XX YY] U [227.13..229.13GHz,1938.48kHz,11.4mJy/beam@10km/s,701.8uJy/beam@native, XX YY] U [229.02..231.02GHz,1938.48kHz,12.4mJy/beam@10km/s,771uJy/beam@native, XX YY]	212.07421945528318	2537.81550822763	ALMA						One year ago the visual dimming of Betelgeuse caused a cascade of public news, following the suggestion of an imminent core-collapse. Other hypotheses formulated to explain this extraordinary event were the formation of large cold spots on the stellar photosphere, or an increased extinction along the line of sight. Betelgeuse may have undergone an increased mass-loss episode that favours dust grain formation, consistently with the erratic stellar activity of evolved massive stars. We propose a monitoring programme with ACA in Bands 3, 6 and 7, to test the role of dust in the recent visual dimming and to perform an unprecedented study of the dust properties and formation cycle. We request calibration-limited observations (with photometric uncertainty of 5%) to derive light curves at five different frequencies and, additionally, spectral indices to disentangle different emission mechanisms contributing to the sub-mm wavelengths. With these observations we will gain a rare insight into dust processes and mass-lo	Betelgeu_f_06_7M	Etoka, Sandra; Scicluna, Peter; Richards, Anita; Phillips, Neil; Mairs, Steve; Wong, Ka Tat; de Wit, Willem-Jan; Menten, Karl; Lundgren, Andreas; Jones, Olivia; Mehner, Andrea; De Breuck, Carlos; Kemper, Ciska; Baade, Dietrich; Dharmawardena, Thavisha; Trejo, Alfonso; Montarges, Miguel; Randall, Suzanna; Humphreys, Elizabeth;	12.65204998331095	0.3632221299301987	1.8	uid://A001/X159b/X20	uid://A001/X159b/X21	uid://A002/Xf53eeb/X1c0f3	The fall and rise of Betelgeuse: diving in its ejecta with ACA	S	TARGET	T	33.524562462203136	F		Hypergiants;null	Stars and stellar evolution	cagliozzo	Agliozzo, Claudia	1938.4765625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00927.S	ALMA	JAO	ALMA	uid://A001/X159b/X21.source.Betelgeuse.spw.18	cube	2		Betelgeuse	88.79310812363141	7.407132905681428	0.012544144592574946	Circle ICRS 88.793108 7.407133 0.006272			1024	1	2	6.030335428482976	59608.037179	59608.046372	635.04	635.04	0.0013948239669721173	0.0014079136785641658	110864.13398142318	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X159b/X21	application/x-votable+xml; content=datalink		2021.1.00927.S	Public	199.78726414834546	-8.958414216879447	6	1.269799878040497E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N606:CM06	F	2023-02-01T11:12:30.000	6.030335428482976	[211.08..213.07GHz,1938.48kHz,12.7mJy/beam@10km/s,752.5uJy/beam@native, XX YY] U [212.93..214.93GHz,1938.48kHz,11.6mJy/beam@10km/s,690uJy/beam@native, XX YY] U [227.13..229.13GHz,1938.48kHz,11.4mJy/beam@10km/s,701.8uJy/beam@native, XX YY] U [229.02..231.02GHz,1938.48kHz,12.4mJy/beam@10km/s,771uJy/beam@native, XX YY]	213.9329720637776	2537.81550822763	ALMA						One year ago the visual dimming of Betelgeuse caused a cascade of public news, following the suggestion of an imminent core-collapse. Other hypotheses formulated to explain this extraordinary event were the formation of large cold spots on the stellar photosphere, or an increased extinction along the line of sight. Betelgeuse may have undergone an increased mass-loss episode that favours dust grain formation, consistently with the erratic stellar activity of evolved massive stars. We propose a monitoring programme with ACA in Bands 3, 6 and 7, to test the role of dust in the recent visual dimming and to perform an unprecedented study of the dust properties and formation cycle. We request calibration-limited observations (with photometric uncertainty of 5%) to derive light curves at five different frequencies and, additionally, spectral indices to disentangle different emission mechanisms contributing to the sub-mm wavelengths. With these observations we will gain a rare insight into dust processes and mass-lo	Betelgeu_f_06_7M	Etoka, Sandra; Scicluna, Peter; Richards, Anita; Phillips, Neil; Mairs, Steve; Wong, Ka Tat; de Wit, Willem-Jan; Menten, Karl; Lundgren, Andreas; Jones, Olivia; Mehner, Andrea; De Breuck, Carlos; Kemper, Ciska; Baade, Dietrich; Dharmawardena, Thavisha; Trejo, Alfonso; Montarges, Miguel; Randall, Suzanna; Humphreys, Elizabeth;	11.550976199362305	0.3632221299301987	1.8	uid://A001/X159b/X20	uid://A001/X159b/X21	uid://A002/Xf53eeb/X1c0f3	The fall and rise of Betelgeuse: diving in its ejecta with ACA	S	TARGET	T	33.524562462203136	F		Hypergiants;null	Stars and stellar evolution	cagliozzo	Agliozzo, Claudia	1938.4765625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00927.S	ALMA	JAO	ALMA	uid://A001/X159b/X21.source.Betelgeuse.spw.20	cube	2		Betelgeuse	88.79310812363141	7.407132905681428	0.012544144592574946	Circle ICRS 88.793108 7.407133 0.006272			1024	1	2	6.030335428482976	59608.037179	59608.046372	635.04	635.04	0.0013084216278826265	0.001319933191354692	117154.37733343829	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X159b/X21	application/x-votable+xml; content=datalink		2021.1.00927.S	Public	199.78726414834546	-8.958414216879447	6	1.1167077127783425E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N606:CM06	F	2023-02-01T11:12:30.000	6.030335428482976	[211.08..213.07GHz,1938.48kHz,12.7mJy/beam@10km/s,752.5uJy/beam@native, XX YY] U [212.93..214.93GHz,1938.48kHz,11.6mJy/beam@10km/s,690uJy/beam@native, XX YY] U [227.13..229.13GHz,1938.48kHz,11.4mJy/beam@10km/s,701.8uJy/beam@native, XX YY] U [229.02..231.02GHz,1938.48kHz,12.4mJy/beam@10km/s,771uJy/beam@native, XX YY]	228.12613169605567	2537.81550822763	ALMA						One year ago the visual dimming of Betelgeuse caused a cascade of public news, following the suggestion of an imminent core-collapse. Other hypotheses formulated to explain this extraordinary event were the formation of large cold spots on the stellar photosphere, or an increased extinction along the line of sight. Betelgeuse may have undergone an increased mass-loss episode that favours dust grain formation, consistently with the erratic stellar activity of evolved massive stars. We propose a monitoring programme with ACA in Bands 3, 6 and 7, to test the role of dust in the recent visual dimming and to perform an unprecedented study of the dust properties and formation cycle. We request calibration-limited observations (with photometric uncertainty of 5%) to derive light curves at five different frequencies and, additionally, spectral indices to disentangle different emission mechanisms contributing to the sub-mm wavelengths. With these observations we will gain a rare insight into dust processes and mass-lo	Betelgeu_f_06_7M	Etoka, Sandra; Scicluna, Peter; Richards, Anita; Phillips, Neil; Mairs, Steve; Wong, Ka Tat; de Wit, Willem-Jan; Menten, Karl; Lundgren, Andreas; Jones, Olivia; Mehner, Andrea; De Breuck, Carlos; Kemper, Ciska; Baade, Dietrich; Dharmawardena, Thavisha; Trejo, Alfonso; Montarges, Miguel; Randall, Suzanna; Humphreys, Elizabeth;	11.37696016817975	0.3632221299301987	1.8	uid://A001/X159b/X20	uid://A001/X159b/X21	uid://A002/Xf53eeb/X1c0f3	The fall and rise of Betelgeuse: diving in its ejecta with ACA	S	TARGET	T	33.524562462203136	F		Hypergiants;null	Stars and stellar evolution	cagliozzo	Agliozzo, Claudia	1938.4765625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00403.S	ALMA	JAO	ALMA	uid://A001/X2d20/X2a70.source.J0112+3208.spw.24	image	2		J0112+3208	18.20972108328526	32.138175694400836	0.01233008774189321	Circle ICRS 18.209721 32.138176 0.006165			128	1	2	6.164406714785668	60119.464296	60119.505816	423.36	423.36	0.0012831922590153559	0.0012941836929658498	7413.291915729959	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X2a70	application/x-votable+xml; content=datalink		2022.1.00403.S	Public	128.190446158207	-30.51491802941016	6	1.7310793394751664E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2024-07-04T19:28:22.000	6.164406714785668	[216.14..218.12GHz,31250.00kHz,15.1mJy/beam@10km/s,908uJy/beam@native, XX YY] U [219.57..219.82GHz,282.23kHz,16.4mJy/beam@10km/s,2.8mJy/beam@native, XX YY] U [220.40..220.65GHz,282.23kHz,18.8mJy/beam@10km/s,3.2mJy/beam@native, XX YY] U [230.42..230.92GHz,282.23kHz,17.5mJy/beam@10km/s,2.2mJy/beam@native, XX YY] U [231.65..233.63GHz,31250.00kHz,14.6mJy/beam@10km/s,912.3uJy/beam@native, XX YY]	232.63809076432034	367.15784371426656	ALMA						Milky Way studies show that the molecular ISM is filamentary on few pc scales, including recent discoveries of large-scale galactic filaments, but coarse resolution in extragalactic observations has stifled direct comparisons beyond the Milky Way. We propose observations to enable this comparison with complete mapping of M33's inner star-forming disc (25 kpc2) to resolve filamentary molecular clouds on 4 pc scales, down to masses of 900 Msol (5-sigma). We will efficiently detect widespread 12CO & 13CO(2-1) to (1) identify how galactic structure shapes the molecular ISM morphology in different environments (centre vs. spiral arms vs. inter-arms); (2) trace molecular clouds from formation to dispersal, building a resolved view of the molecular cloud lifecycle; (3) resolve whether filamentary morphology influences where massive star form, testing predictions from competing star formation theories. This survey enters a new regime in molecular cloud studies by resolving similar scales to Galactic plane surveys acr	m33_bric_ac_06_7M	Zhang, Qizhou; Konietzka, Ralf; Williams, Benjamin; Kepley, Amanda; Jeffreson, Sarah; Smercina, Adam; Thilker, David; Zucker, Catherine; Henshaw, Jonathan; Sarbadhicary, Sumit; Battersby, Cara; Beane, Angus; Corbelli, Edvige; Schruba, Andreas; Bialy, Shmuel; Goodman, Alyssa; Semenov, Vadim; Leroy, Adam; Sandstrom, Karin; Braine, Jonathan; Williams, Thomas; Foley, Michael; Rosolowsky, Erik;	14.645576153238059	0.5923049440177783	1.8	uid://A001/X2d20/X2a6d	uid://A001/X2d20/X2a70	uid://A002/X10924ab/X836b	Linking the Resolved Filamentary Molecular ISM to Massive Star Formation across M33	S	PHASE WVR	F	32.06565122045067	T		Giant Molecular Clouds (GMC) properties;null	ISM and star formation	ekoch	Koch, Eric	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00403.S	ALMA	JAO	ALMA	uid://A001/X2d20/X2a70.source.J0112+3208.spw.18	cube	2		J0112+3208	18.20972108328526	32.138175694400836	0.01233008774189321	Circle ICRS 18.209721 32.138176 0.006165			1024	1	2	6.164406714785668	60119.464296	60119.505816	423.36	423.36	0.0013586533988977738	0.0013601928567682155	781898.6820661933	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X2a70	application/x-votable+xml; content=datalink		2022.1.00403.S	Public	128.190446158207	-30.51491802941016	6	1.7397480265530503E-9	2.5E8	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2024-07-04T19:28:22.000	6.164406714785668	[216.14..218.12GHz,31250.00kHz,15.1mJy/beam@10km/s,908uJy/beam@native, XX YY] U [219.57..219.82GHz,282.23kHz,16.4mJy/beam@10km/s,2.8mJy/beam@native, XX YY] U [220.40..220.65GHz,282.23kHz,18.8mJy/beam@10km/s,3.2mJy/beam@native, XX YY] U [230.42..230.92GHz,282.23kHz,17.5mJy/beam@10km/s,2.2mJy/beam@native, XX YY] U [231.65..233.63GHz,31250.00kHz,14.6mJy/beam@10km/s,912.3uJy/beam@native, XX YY]	220.52924360055596	367.15784371426656	ALMA						Milky Way studies show that the molecular ISM is filamentary on few pc scales, including recent discoveries of large-scale galactic filaments, but coarse resolution in extragalactic observations has stifled direct comparisons beyond the Milky Way. We propose observations to enable this comparison with complete mapping of M33's inner star-forming disc (25 kpc2) to resolve filamentary molecular clouds on 4 pc scales, down to masses of 900 Msol (5-sigma). We will efficiently detect widespread 12CO & 13CO(2-1) to (1) identify how galactic structure shapes the molecular ISM morphology in different environments (centre vs. spiral arms vs. inter-arms); (2) trace molecular clouds from formation to dispersal, building a resolved view of the molecular cloud lifecycle; (3) resolve whether filamentary morphology influences where massive star form, testing predictions from competing star formation theories. This survey enters a new regime in molecular cloud studies by resolving similar scales to Galactic plane surveys acr	m33_bric_ac_06_7M	Zhang, Qizhou; Konietzka, Ralf; Williams, Benjamin; Kepley, Amanda; Jeffreson, Sarah; Smercina, Adam; Thilker, David; Zucker, Catherine; Henshaw, Jonathan; Sarbadhicary, Sumit; Battersby, Cara; Beane, Angus; Corbelli, Edvige; Schruba, Andreas; Bialy, Shmuel; Goodman, Alyssa; Semenov, Vadim; Leroy, Adam; Sandstrom, Karin; Braine, Jonathan; Williams, Thomas; Foley, Michael; Rosolowsky, Erik;	18.84842208846961	0.5923049440177783	1.8	uid://A001/X2d20/X2a6d	uid://A001/X2d20/X2a70	uid://A002/X10924ab/X836b	Linking the Resolved Filamentary Molecular ISM to Massive Star Formation across M33	S	PHASE WVR	F	32.06565122045067	T		Giant Molecular Clouds (GMC) properties;null	ISM and star formation	ekoch	Koch, Eric	282.2265625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00403.S	ALMA	JAO	ALMA	uid://A001/X2d20/X2a70.source.J0112+3208.spw.16	image	2		J0112+3208	18.20972108328526	32.138175694400836	0.01233008774189321	Circle ICRS 18.209721 32.138176 0.006165			128	1	2	6.164406714785668	60119.464296	60119.505816	423.36	423.36	0.0013744319336324439	0.0013870496847026548	6980.455906009957	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X2a70	application/x-votable+xml; content=datalink		2022.1.00403.S	Public	128.190446158207	-30.51491802941016	6	1.9872137053875424E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2024-07-04T19:28:22.000	6.164406714785668	[216.14..218.12GHz,31250.00kHz,15.1mJy/beam@10km/s,908uJy/beam@native, XX YY] U [219.57..219.82GHz,282.23kHz,16.4mJy/beam@10km/s,2.8mJy/beam@native, XX YY] U [220.40..220.65GHz,282.23kHz,18.8mJy/beam@10km/s,3.2mJy/beam@native, XX YY] U [230.42..230.92GHz,282.23kHz,17.5mJy/beam@10km/s,2.2mJy/beam@native, XX YY] U [231.65..233.63GHz,31250.00kHz,14.6mJy/beam@10km/s,912.3uJy/beam@native, XX YY]	217.1288884004111	367.15784371426656	ALMA						Milky Way studies show that the molecular ISM is filamentary on few pc scales, including recent discoveries of large-scale galactic filaments, but coarse resolution in extragalactic observations has stifled direct comparisons beyond the Milky Way. We propose observations to enable this comparison with complete mapping of M33's inner star-forming disc (25 kpc2) to resolve filamentary molecular clouds on 4 pc scales, down to masses of 900 Msol (5-sigma). We will efficiently detect widespread 12CO & 13CO(2-1) to (1) identify how galactic structure shapes the molecular ISM morphology in different environments (centre vs. spiral arms vs. inter-arms); (2) trace molecular clouds from formation to dispersal, building a resolved view of the molecular cloud lifecycle; (3) resolve whether filamentary morphology influences where massive star form, testing predictions from competing star formation theories. This survey enters a new regime in molecular cloud studies by resolving similar scales to Galactic plane surveys acr	m33_bric_ac_06_7M	Zhang, Qizhou; Konietzka, Ralf; Williams, Benjamin; Kepley, Amanda; Jeffreson, Sarah; Smercina, Adam; Thilker, David; Zucker, Catherine; Henshaw, Jonathan; Sarbadhicary, Sumit; Battersby, Cara; Beane, Angus; Corbelli, Edvige; Schruba, Andreas; Bialy, Shmuel; Goodman, Alyssa; Semenov, Vadim; Leroy, Adam; Sandstrom, Karin; Braine, Jonathan; Williams, Thomas; Foley, Michael; Rosolowsky, Erik;	15.089494830482069	0.5923049440177783	1.8	uid://A001/X2d20/X2a6d	uid://A001/X2d20/X2a70	uid://A002/X10924ab/X836b	Linking the Resolved Filamentary Molecular ISM to Massive Star Formation across M33	S	PHASE WVR	F	32.06565122045067	T		Giant Molecular Clouds (GMC) properties;null	ISM and star formation	ekoch	Koch, Eric	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00403.S	ALMA	JAO	ALMA	uid://A001/X2d20/X2a70.source.J0112+3208.spw.20	cube	2		J0112+3208	18.20972108328526	32.138175694400836	0.01233008774189321	Circle ICRS 18.209721 32.138176 0.006165			1024	1	2	6.164406714785668	60119.464296	60119.505816	423.36	423.36	0.0013638379074753263	0.0013653891433561354	778926.363727093	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X2a70	application/x-votable+xml; content=datalink		2022.1.00403.S	Public	128.190446158207	-30.51491802941016	6	1.7530584072311346E-9	2.5E8	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2024-07-04T19:28:22.000	6.164406714785668	[216.14..218.12GHz,31250.00kHz,15.1mJy/beam@10km/s,908uJy/beam@native, XX YY] U [219.57..219.82GHz,282.23kHz,16.4mJy/beam@10km/s,2.8mJy/beam@native, XX YY] U [220.40..220.65GHz,282.23kHz,18.8mJy/beam@10km/s,3.2mJy/beam@native, XX YY] U [230.42..230.92GHz,282.23kHz,17.5mJy/beam@10km/s,2.2mJy/beam@native, XX YY] U [231.65..233.63GHz,31250.00kHz,14.6mJy/beam@10km/s,912.3uJy/beam@native, XX YY]	219.69044661060747	367.15784371426656	ALMA						Milky Way studies show that the molecular ISM is filamentary on few pc scales, including recent discoveries of large-scale galactic filaments, but coarse resolution in extragalactic observations has stifled direct comparisons beyond the Milky Way. We propose observations to enable this comparison with complete mapping of M33's inner star-forming disc (25 kpc2) to resolve filamentary molecular clouds on 4 pc scales, down to masses of 900 Msol (5-sigma). We will efficiently detect widespread 12CO & 13CO(2-1) to (1) identify how galactic structure shapes the molecular ISM morphology in different environments (centre vs. spiral arms vs. inter-arms); (2) trace molecular clouds from formation to dispersal, building a resolved view of the molecular cloud lifecycle; (3) resolve whether filamentary morphology influences where massive star form, testing predictions from competing star formation theories. This survey enters a new regime in molecular cloud studies by resolving similar scales to Galactic plane surveys acr	m33_bric_ac_06_7M	Zhang, Qizhou; Konietzka, Ralf; Williams, Benjamin; Kepley, Amanda; Jeffreson, Sarah; Smercina, Adam; Thilker, David; Zucker, Catherine; Henshaw, Jonathan; Sarbadhicary, Sumit; Battersby, Cara; Beane, Angus; Corbelli, Edvige; Schruba, Andreas; Bialy, Shmuel; Goodman, Alyssa; Semenov, Vadim; Leroy, Adam; Sandstrom, Karin; Braine, Jonathan; Williams, Thomas; Foley, Michael; Rosolowsky, Erik;	16.360486164574635	0.5923049440177783	1.8	uid://A001/X2d20/X2a6d	uid://A001/X2d20/X2a70	uid://A002/X10924ab/X836b	Linking the Resolved Filamentary Molecular ISM to Massive Star Formation across M33	S	PHASE WVR	F	32.06565122045067	T		Giant Molecular Clouds (GMC) properties;null	ISM and star formation	ekoch	Koch, Eric	282.2265625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2022.1.00403.S	ALMA	JAO	ALMA	uid://A001/X2d20/X2a70.source.J0112+3208.spw.22	cube	2		J0112+3208	18.20972108328526	32.138175694400836	0.01233008774189321	Circle ICRS 18.209721 32.138176 0.006165			2048	1	2	6.164406714785668	60119.464296	60119.505816	423.36	423.36	0.0012982264395855721	0.0013010418555310422	816522.0030906043	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2d20/X2a70	application/x-votable+xml; content=datalink		2022.1.00403.S	Public	128.190446158207	-30.51491802941016	6	1.590079729785347E-9	5.0E8	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2024-07-04T19:28:22.000	6.164406714785668	[216.14..218.12GHz,31250.00kHz,15.1mJy/beam@10km/s,908uJy/beam@native, XX YY] U [219.57..219.82GHz,282.23kHz,16.4mJy/beam@10km/s,2.8mJy/beam@native, XX YY] U [220.40..220.65GHz,282.23kHz,18.8mJy/beam@10km/s,3.2mJy/beam@native, XX YY] U [230.42..230.92GHz,282.23kHz,17.5mJy/beam@10km/s,2.2mJy/beam@native, XX YY] U [231.65..233.63GHz,31250.00kHz,14.6mJy/beam@10km/s,912.3uJy/beam@native, XX YY]	230.6747712723272	367.15784371426656	ALMA						Milky Way studies show that the molecular ISM is filamentary on few pc scales, including recent discoveries of large-scale galactic filaments, but coarse resolution in extragalactic observations has stifled direct comparisons beyond the Milky Way. We propose observations to enable this comparison with complete mapping of M33's inner star-forming disc (25 kpc2) to resolve filamentary molecular clouds on 4 pc scales, down to masses of 900 Msol (5-sigma). We will efficiently detect widespread 12CO & 13CO(2-1) to (1) identify how galactic structure shapes the molecular ISM morphology in different environments (centre vs. spiral arms vs. inter-arms); (2) trace molecular clouds from formation to dispersal, building a resolved view of the molecular cloud lifecycle; (3) resolve whether filamentary morphology influences where massive star form, testing predictions from competing star formation theories. This survey enters a new regime in molecular cloud studies by resolving similar scales to Galactic plane surveys acr	m33_bric_ac_06_7M	Zhang, Qizhou; Konietzka, Ralf; Williams, Benjamin; Kepley, Amanda; Jeffreson, Sarah; Smercina, Adam; Thilker, David; Zucker, Catherine; Henshaw, Jonathan; Sarbadhicary, Sumit; Battersby, Cara; Beane, Angus; Corbelli, Edvige; Schruba, Andreas; Bialy, Shmuel; Goodman, Alyssa; Semenov, Vadim; Leroy, Adam; Sandstrom, Karin; Braine, Jonathan; Williams, Thomas; Foley, Michael; Rosolowsky, Erik;	17.469429504532535	0.5923049440177783	1.8	uid://A001/X2d20/X2a6d	uid://A001/X2d20/X2a70	uid://A002/X10924ab/X836b	Linking the Resolved Filamentary Molecular ISM to Massive Star Formation across M33	S	PHASE WVR	F	32.06565122045067	T		Giant Molecular Clouds (GMC) properties;null	ISM and star formation	ekoch	Koch, Eric	282.2265625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2017.1.01439.S	ALMA	JAO	ALMA	uid://A001/X1296/X654.source.J0444+2813.spw.25	cube	2		J0444+2813	71.03750000001854	28.216944444445737	0.006882674386964548	Circle ICRS 71.037500 28.216944 0.003441			240	1	2	0.16799023879053587	58118.135229	58118.153075	1360.8	1360.8	0.0013097122481091788	0.0013204845799066776	29298.72069501836	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1296/X654	application/x-votable+xml; content=datalink		2017.1.01439.S	Public	172.73452195130062	-11.414930711081096	6	4.50662484023454E-8	1.875E9	A007:DV05 A015:DA64 A022:DV23 A024:DA49 A027:DV06 A033:DA53 A042:DV08 A043:DA60 A045:DV01 A047:DV15 A060:DV17 A062:DV10 A068:DA65 A069:DV16 A070:DV22 A072:DV20 A073:DA54 A074:DV09 A075:DA52 A076:DA59 A082:DV24 A083:DA48 A085:DA63 A087:DV25 A088:DV04 A089:DA61 A090:DA56 A091:DA58 A092:DV14 A093:DA57 A094:DV19 A096:PM01 A101:DA62 A104:DA51 A105:DV02 A108:DA50 A111:DA46 A115:DA43 A116:DV07 A120:DA44 A121:DA55 A122:DV11 A123:DA42 A128:DV13 A134:DV03 A135:DA45	F	2019-01-26T17:52:00.000	0.16799023879053587	[225.07..226.94GHz,7812.01kHz,603.4uJy/beam@10km/s,38.3uJy/beam@native, XX YY] U [227.03..228.90GHz,7812.01kHz,601.4uJy/beam@10km/s,38.3uJy/beam@native, XX YY] U [241.27..243.14GHz,7812.01kHz,528.5uJy/beam@10km/s,34.7uJy/beam@native, XX YY] U [243.08..244.94GHz,7812.01kHz,527.1uJy/beam@10km/s,34.7uJy/beam@native, XX YY]	227.965818894408	9635.536064282831	ALMA	BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100-200 pc BASS. XXXIV. A Catalog of the Nuclear Millimeter-wave Continuum Emission Properties of AGNs Constrained on Scales ≤ 100-200 pc Hard X-Ray Irradiation Potentially Drives Negative AGN Feedback by Altering Molecular Gas Properties NGC 2992: Interplay between the multiphase disc, wind, and radio bubbles The IBISCO survey. I. Multiphase discs and winds in the Seyfert galaxy Markarian 509	Kawamuro, Taiki Zanchettin, M. V.	Kawamuro, Taiki; Ricci, Claudio; Imanishi, Masatoshi; Mushotzky, Richard F.; Izumi, Takuma; Ricci, Federica; Bauer, Franz E.; Koss, Michael J.; Trakhtenbrot, Benny; Ichikawa, Kohei; Rojas, Alejandra F.; Smith, Krista Lynne; Shimizu, Taro; Oh, Kyuseok; den Brok, Jakob S.; Baba, Shunsuke; Baloković, Mislav; Chang, Chin-Shin; Kakkad, Darshan; Pfeifle, Ryan W.; Privon, George C.; Temple, Matthew J.; Ueda, Yoshihiro; Harrison, Fiona; Powell, Meredith C.; Stern, Daniel; Urry, Meg; Sanders, David B. Kawamuro, Taiki; Ricci, Claudio; Izumi, Takuma; Imanishi, Masatoshi; Baba, Shunsuke; Nguyen, Dieu D.; Onishi, Kyoko Kawamuro, Taiki; Ricci, Claudio; Mushotzky, Richard F.; Imanishi, Masatoshi; Bauer, Franz E.; Ricci, Federica; Koss, Michael J.; Privon, George C.; Trakhtenbrot, Benny; Izumi, Takuma; Ichikawa, Kohei; Rojas, Alejandra F.; Smith, Krista Lynne; Shimizu, Taro; Oh, Kyuseok; den Brok, Jakob S.; Baba, Shunsuke; Baloković, Mislav; Chang, Chin-Shin; Kakkad, Darshan; Pfeifle, Ryan W.; Temple, Matthew J.; Ueda, Yoshi	To investigate the role of active galactic nucleus (AGN) X-ray irradiation on the interstellar medium (ISM), we systematically analyzed Chandra and Atacama Large Millimeter/submillimeter Array CO (J = 2-1) data for 26 hard X-ray (&gt;10 keV) selected AGNs at redshifts below 0.05. While Chandra unveils the distribution of X-ray-irradiated gas via Fe-Kα emission, the CO (J = 2-1) observations reveal that of cold molecular gas. At high resolutions ≲1″, we derive Fe-Kα and CO (J = 2-1) maps for the nuclear 2″ region and for the external annular region of 2″-4″, where 2″ is ~100-600 pc for most of our AGNs. First, focusing on the external regions, we find the Fe-Kα emission for six AGNs above 2σ. Their large equivalent widths (≳1 keV) suggest a fluorescent process as their origin. Moreover, by comparing the 6-7 keV/3-6 keV ratio, as a proxy of Fe-Kα, and CO (J = 2-1) images for three AGNs with the highest significant Fe-Kα detections, we find a possible spatial separation. These suggest the presence of X-ray-irrad	2021	We have recently undertaken a survey of molecular gas in an unbiased sample of AGN, drawn from the INTEGRAL IBIS hard X-ray AGN catalog to have z<0.05,Lbol>10^43 erg/s, and measured black hole masses. IBISCO survey @IRAM/30m is delivering H2 masses, their correlations with AGN properties (Lbol, MBH, Eddington ratio, obscuration), and host galaxy properties (stellar mass, colors, SFR). We propose to extend the single-dish investigation by mapping at 50-100 pc resolution the CO(2-1) emission in all the IBISCO galaxies with CO(2-1) detection, and visible from ALMA. We aim at a) mapping the kinematics of the molecular gas in the inner kpc around the AGN, identify molecular disks or circumnuclear disks, derive the dynamical masses; and b) detecting and mapping non circular motions, including molecular outflows and inflows, and their interaction with the molecular disks. We will use the broad, asymmetric and high velocity CO line profiles to identify outflowing molecular gas, and derive outflow velocity, mass, mass	J0444+28_a_06_TM1	Bischetti, Manuela; Malizia, Angela; Fiore, Fabrizio; Tombesi, Francesco; Bongiorno, Angela; Ceccarelli, Cecilia; Molina, Manuela; Piconcelli, Enrico;	0.6013967291698271	0.01818214790020759	0.9669683	uid://A001/X1296/X653	uid://A001/X1296/X654	uid://A002/Xc89480/X12d1	IBISCO-south: mapping feeding and feedback in an unbiased sample of local AGN	S	TARGET	T	2.989022597897862	T	2021A&A...655A..25Z 2021ApJS..257...64K 2022ApJ...938...87K 2023A&A...679A..88Z 2023ApJS..269...24K	Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	cferuglio	Feruglio, Chiara	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2017.1.01439.S	ALMA	JAO	ALMA	uid://A001/X1296/X654.source.J0444+2813.spw.31	cube	2		J0444+2813	71.03750000001854	28.216944444445737	0.006882674386964548	Circle ICRS 71.037500 28.216944 0.003441			240	1	2	0.16799023879053587	58118.135229	58118.153075	1360.8	1360.8	0.001223928869495336	0.0012333312192510718	31113.21010060621	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1296/X654	application/x-votable+xml; content=datalink		2017.1.01439.S	Public	172.73452195130062	-11.414930711081096	6	3.933490330813196E-8	1.875E9	A007:DV05 A015:DA64 A022:DV23 A024:DA49 A027:DV06 A033:DA53 A042:DV08 A043:DA60 A045:DV01 A047:DV15 A060:DV17 A062:DV10 A068:DA65 A069:DV16 A070:DV22 A072:DV20 A073:DA54 A074:DV09 A075:DA52 A076:DA59 A082:DV24 A083:DA48 A085:DA63 A087:DV25 A088:DV04 A089:DA61 A090:DA56 A091:DA58 A092:DV14 A093:DA57 A094:DV19 A096:PM01 A101:DA62 A104:DA51 A105:DV02 A108:DA50 A111:DA46 A115:DA43 A116:DV07 A120:DA44 A121:DA55 A122:DV11 A123:DA42 A128:DV13 A134:DV03 A135:DA45	F	2019-01-26T17:52:00.000	0.16799023879053587	[225.07..226.94GHz,7812.01kHz,603.4uJy/beam@10km/s,38.3uJy/beam@native, XX YY] U [227.03..228.90GHz,7812.01kHz,601.4uJy/beam@10km/s,38.3uJy/beam@native, XX YY] U [241.27..243.14GHz,7812.01kHz,528.5uJy/beam@10km/s,34.7uJy/beam@native, XX YY] U [243.08..244.94GHz,7812.01kHz,527.1uJy/beam@10km/s,34.7uJy/beam@native, XX YY]	244.00904787955915	9635.536064282831	ALMA	BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100-200 pc BASS. XXXIV. A Catalog of the Nuclear Millimeter-wave Continuum Emission Properties of AGNs Constrained on Scales ≤ 100-200 pc Hard X-Ray Irradiation Potentially Drives Negative AGN Feedback by Altering Molecular Gas Properties NGC 2992: Interplay between the multiphase disc, wind, and radio bubbles The IBISCO survey. I. Multiphase discs and winds in the Seyfert galaxy Markarian 509	Kawamuro, Taiki Zanchettin, M. V.	Kawamuro, Taiki; Ricci, Claudio; Imanishi, Masatoshi; Mushotzky, Richard F.; Izumi, Takuma; Ricci, Federica; Bauer, Franz E.; Koss, Michael J.; Trakhtenbrot, Benny; Ichikawa, Kohei; Rojas, Alejandra F.; Smith, Krista Lynne; Shimizu, Taro; Oh, Kyuseok; den Brok, Jakob S.; Baba, Shunsuke; Baloković, Mislav; Chang, Chin-Shin; Kakkad, Darshan; Pfeifle, Ryan W.; Privon, George C.; Temple, Matthew J.; Ueda, Yoshihiro; Harrison, Fiona; Powell, Meredith C.; Stern, Daniel; Urry, Meg; Sanders, David B. Kawamuro, Taiki; Ricci, Claudio; Izumi, Takuma; Imanishi, Masatoshi; Baba, Shunsuke; Nguyen, Dieu D.; Onishi, Kyoko Kawamuro, Taiki; Ricci, Claudio; Mushotzky, Richard F.; Imanishi, Masatoshi; Bauer, Franz E.; Ricci, Federica; Koss, Michael J.; Privon, George C.; Trakhtenbrot, Benny; Izumi, Takuma; Ichikawa, Kohei; Rojas, Alejandra F.; Smith, Krista Lynne; Shimizu, Taro; Oh, Kyuseok; den Brok, Jakob S.; Baba, Shunsuke; Baloković, Mislav; Chang, Chin-Shin; Kakkad, Darshan; Pfeifle, Ryan W.; Temple, Matthew J.; Ueda, Yoshi	To investigate the role of active galactic nucleus (AGN) X-ray irradiation on the interstellar medium (ISM), we systematically analyzed Chandra and Atacama Large Millimeter/submillimeter Array CO (J = 2-1) data for 26 hard X-ray (&gt;10 keV) selected AGNs at redshifts below 0.05. While Chandra unveils the distribution of X-ray-irradiated gas via Fe-Kα emission, the CO (J = 2-1) observations reveal that of cold molecular gas. At high resolutions ≲1″, we derive Fe-Kα and CO (J = 2-1) maps for the nuclear 2″ region and for the external annular region of 2″-4″, where 2″ is ~100-600 pc for most of our AGNs. First, focusing on the external regions, we find the Fe-Kα emission for six AGNs above 2σ. Their large equivalent widths (≳1 keV) suggest a fluorescent process as their origin. Moreover, by comparing the 6-7 keV/3-6 keV ratio, as a proxy of Fe-Kα, and CO (J = 2-1) images for three AGNs with the highest significant Fe-Kα detections, we find a possible spatial separation. These suggest the presence of X-ray-irrad	2021	We have recently undertaken a survey of molecular gas in an unbiased sample of AGN, drawn from the INTEGRAL IBIS hard X-ray AGN catalog to have z<0.05,Lbol>10^43 erg/s, and measured black hole masses. IBISCO survey @IRAM/30m is delivering H2 masses, their correlations with AGN properties (Lbol, MBH, Eddington ratio, obscuration), and host galaxy properties (stellar mass, colors, SFR). We propose to extend the single-dish investigation by mapping at 50-100 pc resolution the CO(2-1) emission in all the IBISCO galaxies with CO(2-1) detection, and visible from ALMA. We aim at a) mapping the kinematics of the molecular gas in the inner kpc around the AGN, identify molecular disks or circumnuclear disks, derive the dynamical masses; and b) detecting and mapping non circular motions, including molecular outflows and inflows, and their interaction with the molecular disks. We will use the broad, asymmetric and high velocity CO line profiles to identify outflowing molecular gas, and derive outflow velocity, mass, mass	J0444+28_a_06_TM1	Bischetti, Manuela; Malizia, Angela; Fiore, Fabrizio; Tombesi, Francesco; Bongiorno, Angela; Ceccarelli, Cecilia; Molina, Manuela; Piconcelli, Enrico;	0.5270748997150971	0.01818214790020759	0.9669683	uid://A001/X1296/X653	uid://A001/X1296/X654	uid://A002/Xc89480/X12d1	IBISCO-south: mapping feeding and feedback in an unbiased sample of local AGN	S	TARGET	T	2.989022597897862	T	2021A&A...655A..25Z 2021ApJS..257...64K 2022ApJ...938...87K 2023A&A...679A..88Z 2023ApJS..269...24K	Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	cferuglio	Feruglio, Chiara	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2017.1.01439.S	ALMA	JAO	ALMA	uid://A001/X1296/X654.source.J0444+2813.spw.27	cube	2		J0444+2813	71.03750000001854	28.216944444445737	0.006882674386964548	Circle ICRS 71.037500 28.216944 0.003441			240	1	2	0.16799023879053587	58118.135229	58118.153075	1360.8	1360.8	0.0013210130234941548	0.0013319728319612719	29048.0810300393	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1296/X654	application/x-votable+xml; content=datalink		2017.1.01439.S	Public	172.73452195130062	-11.414930711081096	6	4.585056050129261E-8	1.875E9	A007:DV05 A015:DA64 A022:DV23 A024:DA49 A027:DV06 A033:DA53 A042:DV08 A043:DA60 A045:DV01 A047:DV15 A060:DV17 A062:DV10 A068:DA65 A069:DV16 A070:DV22 A072:DV20 A073:DA54 A074:DV09 A075:DA52 A076:DA59 A082:DV24 A083:DA48 A085:DA63 A087:DV25 A088:DV04 A089:DA61 A090:DA56 A091:DA58 A092:DV14 A093:DA57 A094:DV19 A096:PM01 A101:DA62 A104:DA51 A105:DV02 A108:DA50 A111:DA46 A115:DA43 A116:DV07 A120:DA44 A121:DA55 A122:DV11 A123:DA42 A128:DV13 A134:DV03 A135:DA45	F	2019-01-26T17:52:00.000	0.16799023879053587	[225.07..226.94GHz,7812.01kHz,603.4uJy/beam@10km/s,38.3uJy/beam@native, XX YY] U [227.03..228.90GHz,7812.01kHz,601.4uJy/beam@10km/s,38.3uJy/beam@native, XX YY] U [241.27..243.14GHz,7812.01kHz,528.5uJy/beam@10km/s,34.7uJy/beam@native, XX YY] U [243.08..244.94GHz,7812.01kHz,527.1uJy/beam@10km/s,34.7uJy/beam@native, XX YY]	226.00766889110878	9635.536064282831	ALMA	BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100-200 pc BASS. XXXIV. A Catalog of the Nuclear Millimeter-wave Continuum Emission Properties of AGNs Constrained on Scales ≤ 100-200 pc Hard X-Ray Irradiation Potentially Drives Negative AGN Feedback by Altering Molecular Gas Properties NGC 2992: Interplay between the multiphase disc, wind, and radio bubbles The IBISCO survey. I. Multiphase discs and winds in the Seyfert galaxy Markarian 509	Kawamuro, Taiki Zanchettin, M. V.	Kawamuro, Taiki; Ricci, Claudio; Imanishi, Masatoshi; Mushotzky, Richard F.; Izumi, Takuma; Ricci, Federica; Bauer, Franz E.; Koss, Michael J.; Trakhtenbrot, Benny; Ichikawa, Kohei; Rojas, Alejandra F.; Smith, Krista Lynne; Shimizu, Taro; Oh, Kyuseok; den Brok, Jakob S.; Baba, Shunsuke; Baloković, Mislav; Chang, Chin-Shin; Kakkad, Darshan; Pfeifle, Ryan W.; Privon, George C.; Temple, Matthew J.; Ueda, Yoshihiro; Harrison, Fiona; Powell, Meredith C.; Stern, Daniel; Urry, Meg; Sanders, David B. Kawamuro, Taiki; Ricci, Claudio; Izumi, Takuma; Imanishi, Masatoshi; Baba, Shunsuke; Nguyen, Dieu D.; Onishi, Kyoko Kawamuro, Taiki; Ricci, Claudio; Mushotzky, Richard F.; Imanishi, Masatoshi; Bauer, Franz E.; Ricci, Federica; Koss, Michael J.; Privon, George C.; Trakhtenbrot, Benny; Izumi, Takuma; Ichikawa, Kohei; Rojas, Alejandra F.; Smith, Krista Lynne; Shimizu, Taro; Oh, Kyuseok; den Brok, Jakob S.; Baba, Shunsuke; Baloković, Mislav; Chang, Chin-Shin; Kakkad, Darshan; Pfeifle, Ryan W.; Temple, Matthew J.; Ueda, Yoshi	To investigate the role of active galactic nucleus (AGN) X-ray irradiation on the interstellar medium (ISM), we systematically analyzed Chandra and Atacama Large Millimeter/submillimeter Array CO (J = 2-1) data for 26 hard X-ray (&gt;10 keV) selected AGNs at redshifts below 0.05. While Chandra unveils the distribution of X-ray-irradiated gas via Fe-Kα emission, the CO (J = 2-1) observations reveal that of cold molecular gas. At high resolutions ≲1″, we derive Fe-Kα and CO (J = 2-1) maps for the nuclear 2″ region and for the external annular region of 2″-4″, where 2″ is ~100-600 pc for most of our AGNs. First, focusing on the external regions, we find the Fe-Kα emission for six AGNs above 2σ. Their large equivalent widths (≳1 keV) suggest a fluorescent process as their origin. Moreover, by comparing the 6-7 keV/3-6 keV ratio, as a proxy of Fe-Kα, and CO (J = 2-1) images for three AGNs with the highest significant Fe-Kα detections, we find a possible spatial separation. These suggest the presence of X-ray-irrad	2021	We have recently undertaken a survey of molecular gas in an unbiased sample of AGN, drawn from the INTEGRAL IBIS hard X-ray AGN catalog to have z<0.05,Lbol>10^43 erg/s, and measured black hole masses. IBISCO survey @IRAM/30m is delivering H2 masses, their correlations with AGN properties (Lbol, MBH, Eddington ratio, obscuration), and host galaxy properties (stellar mass, colors, SFR). We propose to extend the single-dish investigation by mapping at 50-100 pc resolution the CO(2-1) emission in all the IBISCO galaxies with CO(2-1) detection, and visible from ALMA. We aim at a) mapping the kinematics of the molecular gas in the inner kpc around the AGN, identify molecular disks or circumnuclear disks, derive the dynamical masses; and b) detecting and mapping non circular motions, including molecular outflows and inflows, and their interaction with the molecular disks. We will use the broad, asymmetric and high velocity CO line profiles to identify outflowing molecular gas, and derive outflow velocity, mass, mass	J0444+28_a_06_TM1	Bischetti, Manuela; Malizia, Angela; Fiore, Fabrizio; Tombesi, Francesco; Bongiorno, Angela; Ceccarelli, Cecilia; Molina, Manuela; Piconcelli, Enrico;	0.6034070589274115	0.01818214790020759	0.9669683	uid://A001/X1296/X653	uid://A001/X1296/X654	uid://A002/Xc89480/X12d1	IBISCO-south: mapping feeding and feedback in an unbiased sample of local AGN	S	TARGET	T	2.989022597897862	T	2021A&A...655A..25Z 2021ApJS..257...64K 2022ApJ...938...87K 2023A&A...679A..88Z 2023ApJS..269...24K	Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	cferuglio	Feruglio, Chiara	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2017.1.01439.S	ALMA	JAO	ALMA	uid://A001/X1296/X654.source.J0444+2813.spw.29	cube	2		J0444+2813	71.03750000001854	28.216944444445737	0.006882674386964548	Circle ICRS 71.037500 28.216944 0.003441			240	1	2	0.16799023879053587	58118.135229	58118.153075	1360.8	1360.8	0.001232994012497388	0.0012425366997614446	30882.704193415502	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1296/X654	application/x-votable+xml; content=datalink		2017.1.01439.S	Public	172.73452195130062	-11.414930711081096	6	3.992200785791932E-8	1.875E9	A007:DV05 A015:DA64 A022:DV23 A024:DA49 A027:DV06 A033:DA53 A042:DV08 A043:DA60 A045:DV01 A047:DV15 A060:DV17 A062:DV10 A068:DA65 A069:DV16 A070:DV22 A072:DV20 A073:DA54 A074:DV09 A075:DA52 A076:DA59 A082:DV24 A083:DA48 A085:DA63 A087:DV25 A088:DV04 A089:DA61 A090:DA56 A091:DA58 A092:DV14 A093:DA57 A094:DV19 A096:PM01 A101:DA62 A104:DA51 A105:DV02 A108:DA50 A111:DA46 A115:DA43 A116:DV07 A120:DA44 A121:DA55 A122:DV11 A123:DA42 A128:DV13 A134:DV03 A135:DA45	F	2019-01-26T17:52:00.000	0.16799023879053587	[225.07..226.94GHz,7812.01kHz,603.4uJy/beam@10km/s,38.3uJy/beam@native, XX YY] U [227.03..228.90GHz,7812.01kHz,601.4uJy/beam@10km/s,38.3uJy/beam@native, XX YY] U [241.27..243.14GHz,7812.01kHz,528.5uJy/beam@10km/s,34.7uJy/beam@native, XX YY] U [243.08..244.94GHz,7812.01kHz,527.1uJy/beam@10km/s,34.7uJy/beam@native, XX YY]	242.2081950777344	9635.536064282831	ALMA	BASS XXXII: Studying the Nuclear Millimeter-wave Continuum Emission of AGNs with ALMA at Scales ≲100-200 pc BASS. XXXIV. A Catalog of the Nuclear Millimeter-wave Continuum Emission Properties of AGNs Constrained on Scales ≤ 100-200 pc Hard X-Ray Irradiation Potentially Drives Negative AGN Feedback by Altering Molecular Gas Properties NGC 2992: Interplay between the multiphase disc, wind, and radio bubbles The IBISCO survey. I. Multiphase discs and winds in the Seyfert galaxy Markarian 509	Kawamuro, Taiki Zanchettin, M. V.	Kawamuro, Taiki; Ricci, Claudio; Imanishi, Masatoshi; Mushotzky, Richard F.; Izumi, Takuma; Ricci, Federica; Bauer, Franz E.; Koss, Michael J.; Trakhtenbrot, Benny; Ichikawa, Kohei; Rojas, Alejandra F.; Smith, Krista Lynne; Shimizu, Taro; Oh, Kyuseok; den Brok, Jakob S.; Baba, Shunsuke; Baloković, Mislav; Chang, Chin-Shin; Kakkad, Darshan; Pfeifle, Ryan W.; Privon, George C.; Temple, Matthew J.; Ueda, Yoshihiro; Harrison, Fiona; Powell, Meredith C.; Stern, Daniel; Urry, Meg; Sanders, David B. Kawamuro, Taiki; Ricci, Claudio; Izumi, Takuma; Imanishi, Masatoshi; Baba, Shunsuke; Nguyen, Dieu D.; Onishi, Kyoko Kawamuro, Taiki; Ricci, Claudio; Mushotzky, Richard F.; Imanishi, Masatoshi; Bauer, Franz E.; Ricci, Federica; Koss, Michael J.; Privon, George C.; Trakhtenbrot, Benny; Izumi, Takuma; Ichikawa, Kohei; Rojas, Alejandra F.; Smith, Krista Lynne; Shimizu, Taro; Oh, Kyuseok; den Brok, Jakob S.; Baba, Shunsuke; Baloković, Mislav; Chang, Chin-Shin; Kakkad, Darshan; Pfeifle, Ryan W.; Temple, Matthew J.; Ueda, Yoshi	To investigate the role of active galactic nucleus (AGN) X-ray irradiation on the interstellar medium (ISM), we systematically analyzed Chandra and Atacama Large Millimeter/submillimeter Array CO (J = 2-1) data for 26 hard X-ray (&gt;10 keV) selected AGNs at redshifts below 0.05. While Chandra unveils the distribution of X-ray-irradiated gas via Fe-Kα emission, the CO (J = 2-1) observations reveal that of cold molecular gas. At high resolutions ≲1″, we derive Fe-Kα and CO (J = 2-1) maps for the nuclear 2″ region and for the external annular region of 2″-4″, where 2″ is ~100-600 pc for most of our AGNs. First, focusing on the external regions, we find the Fe-Kα emission for six AGNs above 2σ. Their large equivalent widths (≳1 keV) suggest a fluorescent process as their origin. Moreover, by comparing the 6-7 keV/3-6 keV ratio, as a proxy of Fe-Kα, and CO (J = 2-1) images for three AGNs with the highest significant Fe-Kα detections, we find a possible spatial separation. These suggest the presence of X-ray-irrad	2021	We have recently undertaken a survey of molecular gas in an unbiased sample of AGN, drawn from the INTEGRAL IBIS hard X-ray AGN catalog to have z<0.05,Lbol>10^43 erg/s, and measured black hole masses. IBISCO survey @IRAM/30m is delivering H2 masses, their correlations with AGN properties (Lbol, MBH, Eddington ratio, obscuration), and host galaxy properties (stellar mass, colors, SFR). We propose to extend the single-dish investigation by mapping at 50-100 pc resolution the CO(2-1) emission in all the IBISCO galaxies with CO(2-1) detection, and visible from ALMA. We aim at a) mapping the kinematics of the molecular gas in the inner kpc around the AGN, identify molecular disks or circumnuclear disks, derive the dynamical masses; and b) detecting and mapping non circular motions, including molecular outflows and inflows, and their interaction with the molecular disks. We will use the broad, asymmetric and high velocity CO line profiles to identify outflowing molecular gas, and derive outflow velocity, mass, mass	J0444+28_a_06_TM1	Bischetti, Manuela; Malizia, Angela; Fiore, Fabrizio; Tombesi, Francesco; Bongiorno, Angela; Ceccarelli, Cecilia; Molina, Manuela; Piconcelli, Enrico;	0.5285222707091822	0.01818214790020759	0.9669683	uid://A001/X1296/X653	uid://A001/X1296/X654	uid://A002/Xc89480/X12d1	IBISCO-south: mapping feeding and feedback in an unbiased sample of local AGN	S	TARGET	T	2.989022597897862	T	2021A&A...655A..25Z 2021ApJS..257...64K 2022ApJ...938...87K 2023A&A...679A..88Z 2023ApJS..269...24K	Active Galactic Nuclei (AGN)/Quasars (QSO);null	Active galaxies	cferuglio	Feruglio, Chiara	7812.01171875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.00257.S	ALMA	JAO	ALMA	uid://A001/X3819/X186.source.011.917-00.612_OFF_0.spw.23	cube	2		011.917-00.612_OFF_0	276.56666666670014	-18.245555555567744	0.004598403904199614	Polygon ICRS 276.569012 -18.244984 276.569068 -18.245844 276.568788 -18.246663 276.568532 -18.247021 276.568090 -18.247416 276.567269 -18.247783 276.566363 -18.247837 276.565500 -18.247570 276.565009 -18.247232 276.564708 -18.246907 276.564322 -18.246127 276.564265 -18.245267 276.564416 -18.244709 276.564623 -18.244324 276.565244 -18.243695 276.566065 -18.243329 276.566970 -18.243274 276.567833 -18.243541 276.568532 -18.244090 276.568857 -18.244577			4096	1	2	16.55422590928296	61182.377435	61197.161541	506.88	506.88	8.33869635309514E-4	8.386303241989256E-4	366131.2498920157	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3819/X186	application/x-votable+xml; content=datalink		2024.1.00257.S	Proprietary	13.87399833078299	-2.872729357259227	7	2.277970324559791E-9	2.0E9	T701:PM04 T702:PM03 T703:PM01	F	3000-01-01T00:00:00.000	14.942752590680195	[343.98..346.02GHz,976.56kHz,83.1mJy/beam@10km/s,6.3mJy/beam@native, XX YY] U [346.65..347.65GHz,488.28kHz,78.6mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [356.00..357.00GHz,488.28kHz,93.4mJy/beam@10km/s,10.2mJy/beam@native, XX YY] U [357.48..359.52GHz,976.56kHz,112mJy/beam@10km/s,8.7mJy/beam@native, XX YY]	358.49912619539714	411.1454483319606	ALMA						Recent ALMA high-resolution observations have revealed a wealth of substructures in the inner regions of high-mass YSOs. One of the most interesting features are streamers, which have the power to feed protostars at the predicted high accretion rates. In this proposal we plan to find how frequent these substructures are and reveal their connection to the large scale reservoir. To achieve this, we propose to observe a large sample of sources (71 high-mass YSOs) in band 7 to trace infall at different scales using molecular tracers like HCO+ and CH3OH. The proposed observations will resolve scales of ~300 au with the 12m array and recover the large scale fluxes with ACA+TP. If successful, this project has potential to increase the number of known infall streamers by a factor ~5.	014.449-_a_07_TP	Morii, Kaho; Sanhueza, Patricio; Oya, Yoko; Chen, Vivien;	111.96158384514402	4.011269477930484	0.8077025	uid://A001/X3819/X17f	uid://A001/X3819/X186	uid://A002/X13b0edc/X58e0	Feeding high-mass protostars	S	TARGET	T	264.8680587716	F		High-mass star formation;null	ISM and star formation	folguinch	Olguin, Fernando	976.5625	2026-06-09T00:06:12.258
ADS/JAO.ALMA#2024.1.00257.S	ALMA	JAO	ALMA	uid://A001/X3819/X186.source.011.917-00.612_OFF_0.spw.17	cube	2		011.917-00.612_OFF_0	276.56666666670014	-18.245555555567744	0.004598403904199614	Polygon ICRS 276.569012 -18.244984 276.569068 -18.245844 276.568788 -18.246663 276.568532 -18.247021 276.568090 -18.247416 276.567269 -18.247783 276.566363 -18.247837 276.565500 -18.247570 276.565009 -18.247232 276.564708 -18.246907 276.564322 -18.246127 276.564265 -18.245267 276.564416 -18.244709 276.564623 -18.244324 276.565244 -18.243695 276.566065 -18.243329 276.566970 -18.243274 276.567833 -18.243541 276.568532 -18.244090 276.568857 -18.244577			4096	1	2	16.55422590928296	61182.377435	61197.161541	506.88	506.88	8.663986644268851E-4	8.715420857236596E-4	354361.62685402523	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3819/X186	application/x-votable+xml; content=datalink		2024.1.00257.S	Proprietary	13.87399833078299	-2.872729357259227	7	2.4597188994861777E-9	2.0E9	T701:PM04 T702:PM03 T703:PM01	F	3000-01-01T00:00:00.000	14.942752590680195	[343.98..346.02GHz,976.56kHz,83.1mJy/beam@10km/s,6.3mJy/beam@native, XX YY] U [346.65..347.65GHz,488.28kHz,78.6mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [356.00..357.00GHz,488.28kHz,93.4mJy/beam@10km/s,10.2mJy/beam@native, XX YY] U [357.48..359.52GHz,976.56kHz,112mJy/beam@10km/s,8.7mJy/beam@native, XX YY]	345.00035027852755	411.1454483319606	ALMA						Recent ALMA high-resolution observations have revealed a wealth of substructures in the inner regions of high-mass YSOs. One of the most interesting features are streamers, which have the power to feed protostars at the predicted high accretion rates. In this proposal we plan to find how frequent these substructures are and reveal their connection to the large scale reservoir. To achieve this, we propose to observe a large sample of sources (71 high-mass YSOs) in band 7 to trace infall at different scales using molecular tracers like HCO+ and CH3OH. The proposed observations will resolve scales of ~300 au with the 12m array and recover the large scale fluxes with ACA+TP. If successful, this project has potential to increase the number of known infall streamers by a factor ~5.	014.449-_a_07_TP	Morii, Kaho; Sanhueza, Patricio; Oya, Yoko; Chen, Vivien;	83.08166991100904	4.011269477930484	0.8077025	uid://A001/X3819/X17f	uid://A001/X3819/X186	uid://A002/X13b0edc/X58e0	Feeding high-mass protostars	S	TARGET	T	264.8680587716	F		High-mass star formation;null	ISM and star formation	folguinch	Olguin, Fernando	976.5625	2026-06-09T00:06:12.258
ADS/JAO.ALMA#2024.1.00257.S	ALMA	JAO	ALMA	uid://A001/X3819/X186.source.011.917-00.612_OFF_0.spw.21	cube	2		011.917-00.612_OFF_0	276.56666666670014	-18.245555555567744	0.004598403904199614	Polygon ICRS 276.569012 -18.244984 276.569068 -18.245844 276.568788 -18.246663 276.568532 -18.247021 276.568090 -18.247416 276.567269 -18.247783 276.566363 -18.247837 276.565500 -18.247570 276.565009 -18.247232 276.564708 -18.246907 276.564322 -18.246127 276.564265 -18.245267 276.564416 -18.244709 276.564623 -18.244324 276.565244 -18.243695 276.566065 -18.243329 276.566970 -18.243274 276.567833 -18.243541 276.568532 -18.244090 276.568857 -18.244577			4096	1	2	16.55422590928296	61182.377435	61197.161541	506.88	506.88	8.397527718145219E-4	8.421120003256553E-4	729163.9958955505	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3819/X186	application/x-votable+xml; content=datalink		2024.1.00257.S	Proprietary	13.87399833078299	-2.872729357259227	7	1.1517829544398144E-9	1.0E9	T701:PM04 T702:PM03 T703:PM01	F	3000-01-01T00:00:00.000	14.942752590680195	[343.98..346.02GHz,976.56kHz,83.1mJy/beam@10km/s,6.3mJy/beam@native, XX YY] U [346.65..347.65GHz,488.28kHz,78.6mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [356.00..357.00GHz,488.28kHz,93.4mJy/beam@10km/s,10.2mJy/beam@native, XX YY] U [357.48..359.52GHz,976.56kHz,112mJy/beam@10km/s,8.7mJy/beam@native, XX YY]	356.50077564786676	411.1454483319606	ALMA						Recent ALMA high-resolution observations have revealed a wealth of substructures in the inner regions of high-mass YSOs. One of the most interesting features are streamers, which have the power to feed protostars at the predicted high accretion rates. In this proposal we plan to find how frequent these substructures are and reveal their connection to the large scale reservoir. To achieve this, we propose to observe a large sample of sources (71 high-mass YSOs) in band 7 to trace infall at different scales using molecular tracers like HCO+ and CH3OH. The proposed observations will resolve scales of ~300 au with the 12m array and recover the large scale fluxes with ACA+TP. If successful, this project has potential to increase the number of known infall streamers by a factor ~5.	014.449-_a_07_TP	Morii, Kaho; Sanhueza, Patricio; Oya, Yoko; Chen, Vivien;	93.37015123756295	4.011269477930484	0.8077025	uid://A001/X3819/X17f	uid://A001/X3819/X186	uid://A002/X13b0edc/X58e0	Feeding high-mass protostars	S	TARGET	T	264.8680587716	F		High-mass star formation;null	ISM and star formation	folguinch	Olguin, Fernando	488.28125	2026-06-09T00:06:12.258
ADS/JAO.ALMA#2024.1.00257.S	ALMA	JAO	ALMA	uid://A001/X3819/X186.source.011.917-00.612_OFF_0.spw.19	cube	2		011.917-00.612_OFF_0	276.56666666670014	-18.245555555567744	0.004598403904199614	Polygon ICRS 276.569012 -18.244984 276.569068 -18.245844 276.568788 -18.246663 276.568532 -18.247021 276.568090 -18.247416 276.567269 -18.247783 276.566363 -18.247837 276.565500 -18.247570 276.565009 -18.247232 276.564708 -18.246907 276.564322 -18.246127 276.564265 -18.245267 276.564416 -18.244709 276.564623 -18.244324 276.565244 -18.243695 276.566065 -18.243329 276.566970 -18.243274 276.567833 -18.243541 276.568532 -18.244090 276.568857 -18.244577			4096	1	2	16.55422590928296	61182.377435	61197.161541	506.88	506.88	8.623336464080149E-4	8.648238061810625E-4	712061.4877080505	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3819/X186	application/x-votable+xml; content=datalink		2024.1.00257.S	Proprietary	13.87399833078299	-2.872729357259227	7	1.2146532386140435E-9	1.0E9	T701:PM04 T702:PM03 T703:PM01	F	3000-01-01T00:00:00.000	14.942752590680195	[343.98..346.02GHz,976.56kHz,83.1mJy/beam@10km/s,6.3mJy/beam@native, XX YY] U [346.65..347.65GHz,488.28kHz,78.6mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [356.00..357.00GHz,488.28kHz,93.4mJy/beam@10km/s,10.2mJy/beam@native, XX YY] U [357.48..359.52GHz,976.56kHz,112mJy/beam@10km/s,8.7mJy/beam@native, XX YY]	347.1519990591247	411.1454483319606	ALMA						Recent ALMA high-resolution observations have revealed a wealth of substructures in the inner regions of high-mass YSOs. One of the most interesting features are streamers, which have the power to feed protostars at the predicted high accretion rates. In this proposal we plan to find how frequent these substructures are and reveal their connection to the large scale reservoir. To achieve this, we propose to observe a large sample of sources (71 high-mass YSOs) in band 7 to trace infall at different scales using molecular tracers like HCO+ and CH3OH. The proposed observations will resolve scales of ~300 au with the 12m array and recover the large scale fluxes with ACA+TP. If successful, this project has potential to increase the number of known infall streamers by a factor ~5.	014.449-_a_07_TP	Morii, Kaho; Sanhueza, Patricio; Oya, Yoko; Chen, Vivien;	78.58608863665572	4.011269477930484	0.8077025	uid://A001/X3819/X17f	uid://A001/X3819/X186	uid://A002/X13b0edc/X58e0	Feeding high-mass protostars	S	TARGET	T	264.8680587716	F		High-mass star formation;null	ISM and star formation	folguinch	Olguin, Fernando	488.28125	2026-06-09T00:06:12.258
ADS/JAO.ALMA#2021.1.00705.S	ALMA	JAO	ALMA	uid://A001/X15bc/X98f.source.COS.0169.spw.11	image	2		COS.0169	149.9493750000203	1.6163055555556944	0.011153709239791759	Polygon ICRS 149.949375 1.610729 149.947321 1.611120 149.945556 1.612240 149.944327 1.613931 149.943971 1.614919 149.943796 1.616306 149.943971 1.617692 149.944327 1.618680 149.945556 1.620371 149.947321 1.621491 149.949375 1.621882 149.951429 1.621491 149.953194 1.620371 149.954423 1.618680 149.954779 1.617692 149.954954 1.616306 149.954562 1.614253 149.953889 1.613028 149.953194 1.612240 149.951429 1.611120			128	1	2	1.087197509709421	59706.991797	59707.022546	52.416	52.416	0.0019595562298461103	0.0019853106563535792	4831.577999996801	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X15bc/X98f	application/x-votable+xml; content=datalink		2021.1.00705.S	Public	237.33285644260081	41.64010667475675	4	4.055230294558401E-7	2.0E9	A001:DA57 A002:DA52 A003:DV18 A005:DV13 A006:DV17 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A017:DV16 A019:DV14 A022:DV02 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A033:DV01 A035:DA63 A036:DV08 A039:DV23 A040:DA50 A042:DA60 A043:DA55 A045:DA58 A047:DA42 A049:DA44 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A067:DA46 A068:DA54 A070:DA48 A072:DA53 A073:DA43 A074:DA56 A075:DV09 A076:DA51 A082:DA41 A083:DV22 A085:DA59 A088:DV11	F	2023-05-13T16:44:29.000	1.087197509709421	[137.05..139.03GHz,31250.00kHz,4.5mJy/beam@10km/s,215uJy/beam@native, XX YY] U [138.94..140.93GHz,31250.00kHz,4.2mJy/beam@10km/s,204.6uJy/beam@native, XX YY] U [149.05..151.03GHz,31250.00kHz,4.5mJy/beam@10km/s,225uJy/beam@native, XX YY] U [151.01..152.99GHz,31250.00kHz,4.8mJy/beam@10km/s,243.1uJy/beam@native, XX YY]	151.99764407851552	62048.56011849514	ALMA	A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z <SUB>ph</SUB> > 7 A photo-z cautionary tale: Redshift confirmation of COSBO-7 at z = 2.625 ALMACAL. XI. Over-densities as signposts for proto-clusters? A cautionary tale Resolved ALMA [C II] 158 μm Observations at Cosmic Noon: Interstellar Medium Structure and Dynamics of the Starbursting QSO SDSS J1000 The ALPINE-CRISTAL-JWST Survey: JWST/IFU Optical Observations for 18 Main-sequence Galaxies at z = 4─6	Chen, Jianhang Faisst, A. L. Jin, Shuowen Ling, Chenxiaoji Rooney, Christopher	Chen, Jianhang; Ivison, R. J.; Zwaan, Martin A.; Klitsch, Anne; Péroux, Céline; Lovell, Christopher C.; Lagos, Claudia del P.; Biggs, Andrew D.; Bollo, Victoria Faisst, A. L.; Fujimoto, S.; Tsujita, A.; Wang, W.; Nezhad, N.; Loiacono, F.; Übler, H.; Béthermin, M.; Cassata, P.; Dessauges-Zavadsky, M.; Herrera-Camus, R.; Schaerer, D.; Silverman, J. D.; Yan, L.; Aravena, M.; De Looze, I.; Förster Schreiber, N. M.; González-López, J.; Spilker, J.; Tadaki, K.; Casey, C. M.; Franco, M.; Harish, S.; McCracken, H. J.; Kartaltepe, J. S.; Koekemoer, A. M.; Khostovan, A. A.; Liu, D.; Rhodes, J.; Robertson, B. E.; Amorin, R.; Assef, R. J.; Battisti, A. J.; Birkin, J. E.; Boquien, M.; Da Cunha, E.; Dam, P.; Davies, R. L.; Gómez-Espinoza, D. A.; Ferrara, A.; Fudamoto, Y.; Gillman, S.; Ginolfi, M.; Gozaliasl, G.; Gruppioni, C.; Hadi, A.; Hathi, N.; Ibar, E.; Ikeda, R.; Inami, H.; Jones, G. C.; Kohandel, M.; Li, Y.; Lin, Y.-H.; Liu, Z.; Liu, L.-J.; Long, A. S.; Magdis, G.; Maraston, C.; Martin, C. L.; Mitsuhashi, I.; Mobashe	It may be unsurprising that the most common approach to finding proto-clusters is to search for over-densities of galaxies. Upgrades to submillimetre (submm) interferometers and the advent of the James Webb Space Telescope will soon offer the opportunity to find more distant candidate proto-clusters in deep sky surveys without any spectroscopic confirmation. In this Letter, we report the serendipitous discovery of an extremely dense region centred on the blazar, J0217−0820, at z = 0.6 in the ALMACAL sky survey. Its density is eight times higher than that predicted by blind submm surveys. Among the seven submm-bright galaxies, three are as bright as conventional single-dish submm galaxies, with S<SUB>870 μm</SUB> &gt; 3 mJy. The over-density is thus comparable to the densest known and confirmed proto-cluster cores. However, their spectra betray a wide range of redshifts. We investigate the likelihood of line-of-sight projection effects using light cones from cosmological simulations, finding that the deeper we	2023	Dusty Star-Forming Galaxies dominate cosmic star-formation at its peak (z~2) and yet little is known of their volume density toward higher redshifts, where their existence may place interesting constraints on the formation of massive galaxies (M*>10^11Msun). Empirical modeling suggests that 2mm imaging of existing, bright samples of DSFGs selected at 850um-1mm can quickly and easily separate DSFGs by redshift, isolating the `needle in the haystack' DSFGs that sit at z>4 or beyond. We propose 2mm dust continuum observations of a sample of 414/453 of the brightest SCUBA-2 850um-selected DSFGs (S850>5mJy) (the other 39 targets were observed in Cycle 7) with the goal of: (1) identifying the highest redshift candidate DSFGs for future follow-up with ALMA spectral scans and JWST, (2) inferring the volume density of z>3 DSFGs using the population's distribution in 2mm flux density combined with our models of (sub)mm emission from obscured galaxies, and (3) refining measurements of beta, the dust emissivity spectral	COS.0018_a_04_TM1	Sanders, David; da Cunha, Elisabete; Drew, Patrick; Long, Arianna; Spilker, Justin; Scoville, Nick; Champagne, Jaclyn; Staguhn, Johannes; Casey, Caitlin; Manning, Sinclaire; Zavala, Jorge; Hodge, Jacqueline; Kartaltepe, Jeyhan;	4.82822871814835	0.11030188003089186	2.976112	uid://A001/X15bc/X98e	uid://A001/X15bc/X98f	uid://A002/Xf89be2/Xac9d	Needle in a haystack: Identifying the highest-redshift candidate DSFGs using 2mm imaging	S	TARGET	T	12.521798584022807	T	2023A&A...675L..10C 2024A&A...690L..16J 2024ApJ...969L..28L 2025ApJ...987...61R 2026ApJS..282...19F	Sub-mm Galaxies (SMG);Galaxy structure & evolution	Galaxy evolution	ocooper	Cooper, Olivia	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00705.S	ALMA	JAO	ALMA	uid://A001/X15bc/X98f.source.COS.0169.spw.5	image	2		COS.0169	149.9493750000203	1.6163055555556944	0.011153709239791759	Polygon ICRS 149.949375 1.610729 149.947321 1.611120 149.945556 1.612240 149.944327 1.613931 149.943971 1.614919 149.943796 1.616306 149.943971 1.617692 149.944327 1.618680 149.945556 1.620371 149.947321 1.621491 149.949375 1.621882 149.951429 1.621491 149.953194 1.620371 149.954423 1.618680 149.954779 1.617692 149.954954 1.616306 149.954562 1.614253 149.953889 1.613028 149.953194 1.612240 149.951429 1.611120			128	1	2	1.087197509709421	59706.991797	59707.022546	52.416	52.416	0.0021563108424702665	0.002187537951736464	4448.421999996801	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X15bc/X98f	application/x-votable+xml; content=datalink		2021.1.00705.S	Public	237.33285644260081	41.64010667475675	4	4.916955544755291E-7	2.0E9	A001:DA57 A002:DA52 A003:DV18 A005:DV13 A006:DV17 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A017:DV16 A019:DV14 A022:DV02 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A033:DV01 A035:DA63 A036:DV08 A039:DV23 A040:DA50 A042:DA60 A043:DA55 A045:DA58 A047:DA42 A049:DA44 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A067:DA46 A068:DA54 A070:DA48 A072:DA53 A073:DA43 A074:DA56 A075:DV09 A076:DA51 A082:DA41 A083:DV22 A085:DA59 A088:DV11	F	2023-05-13T16:44:29.000	1.087197509709421	[137.05..139.03GHz,31250.00kHz,4.5mJy/beam@10km/s,215uJy/beam@native, XX YY] U [138.94..140.93GHz,31250.00kHz,4.2mJy/beam@10km/s,204.6uJy/beam@native, XX YY] U [149.05..151.03GHz,31250.00kHz,4.5mJy/beam@10km/s,225uJy/beam@native, XX YY] U [151.01..152.99GHz,31250.00kHz,4.8mJy/beam@10km/s,243.1uJy/beam@native, XX YY]	138.03793178865942	62048.56011849514	ALMA	A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z <SUB>ph</SUB> > 7 A photo-z cautionary tale: Redshift confirmation of COSBO-7 at z = 2.625 ALMACAL. XI. Over-densities as signposts for proto-clusters? A cautionary tale Resolved ALMA [C II] 158 μm Observations at Cosmic Noon: Interstellar Medium Structure and Dynamics of the Starbursting QSO SDSS J1000 The ALPINE-CRISTAL-JWST Survey: JWST/IFU Optical Observations for 18 Main-sequence Galaxies at z = 4─6	Chen, Jianhang Faisst, A. L. Jin, Shuowen Ling, Chenxiaoji Rooney, Christopher	Chen, Jianhang; Ivison, R. J.; Zwaan, Martin A.; Klitsch, Anne; Péroux, Céline; Lovell, Christopher C.; Lagos, Claudia del P.; Biggs, Andrew D.; Bollo, Victoria Faisst, A. L.; Fujimoto, S.; Tsujita, A.; Wang, W.; Nezhad, N.; Loiacono, F.; Übler, H.; Béthermin, M.; Cassata, P.; Dessauges-Zavadsky, M.; Herrera-Camus, R.; Schaerer, D.; Silverman, J. D.; Yan, L.; Aravena, M.; De Looze, I.; Förster Schreiber, N. M.; González-López, J.; Spilker, J.; Tadaki, K.; Casey, C. M.; Franco, M.; Harish, S.; McCracken, H. J.; Kartaltepe, J. S.; Koekemoer, A. M.; Khostovan, A. A.; Liu, D.; Rhodes, J.; Robertson, B. E.; Amorin, R.; Assef, R. J.; Battisti, A. J.; Birkin, J. E.; Boquien, M.; Da Cunha, E.; Dam, P.; Davies, R. L.; Gómez-Espinoza, D. A.; Ferrara, A.; Fudamoto, Y.; Gillman, S.; Ginolfi, M.; Gozaliasl, G.; Gruppioni, C.; Hadi, A.; Hathi, N.; Ibar, E.; Ikeda, R.; Inami, H.; Jones, G. C.; Kohandel, M.; Li, Y.; Lin, Y.-H.; Liu, Z.; Liu, L.-J.; Long, A. S.; Magdis, G.; Maraston, C.; Martin, C. L.; Mitsuhashi, I.; Mobashe	It may be unsurprising that the most common approach to finding proto-clusters is to search for over-densities of galaxies. Upgrades to submillimetre (submm) interferometers and the advent of the James Webb Space Telescope will soon offer the opportunity to find more distant candidate proto-clusters in deep sky surveys without any spectroscopic confirmation. In this Letter, we report the serendipitous discovery of an extremely dense region centred on the blazar, J0217−0820, at z = 0.6 in the ALMACAL sky survey. Its density is eight times higher than that predicted by blind submm surveys. Among the seven submm-bright galaxies, three are as bright as conventional single-dish submm galaxies, with S<SUB>870 μm</SUB> &gt; 3 mJy. The over-density is thus comparable to the densest known and confirmed proto-cluster cores. However, their spectra betray a wide range of redshifts. We investigate the likelihood of line-of-sight projection effects using light cones from cosmological simulations, finding that the deeper we	2023	Dusty Star-Forming Galaxies dominate cosmic star-formation at its peak (z~2) and yet little is known of their volume density toward higher redshifts, where their existence may place interesting constraints on the formation of massive galaxies (M*>10^11Msun). Empirical modeling suggests that 2mm imaging of existing, bright samples of DSFGs selected at 850um-1mm can quickly and easily separate DSFGs by redshift, isolating the `needle in the haystack' DSFGs that sit at z>4 or beyond. We propose 2mm dust continuum observations of a sample of 414/453 of the brightest SCUBA-2 850um-selected DSFGs (S850>5mJy) (the other 39 targets were observed in Cycle 7) with the goal of: (1) identifying the highest redshift candidate DSFGs for future follow-up with ALMA spectral scans and JWST, (2) inferring the volume density of z>3 DSFGs using the population's distribution in 2mm flux density combined with our models of (sub)mm emission from obscured galaxies, and (3) refining measurements of beta, the dust emissivity spectral	COS.0018_a_04_TM1	Sanders, David; da Cunha, Elisabete; Drew, Patrick; Long, Arianna; Spilker, Justin; Scoville, Nick; Champagne, Jaclyn; Staguhn, Johannes; Casey, Caitlin; Manning, Sinclaire; Zavala, Jorge; Hodge, Jacqueline; Kartaltepe, Jeyhan;	4.48084454521752	0.11030188003089186	2.976112	uid://A001/X15bc/X98e	uid://A001/X15bc/X98f	uid://A002/Xf89be2/Xac9d	Needle in a haystack: Identifying the highest-redshift candidate DSFGs using 2mm imaging	S	TARGET	T	12.521798584022807	T	2023A&A...675L..10C 2024A&A...690L..16J 2024ApJ...969L..28L 2025ApJ...987...61R 2026ApJS..282...19F	Sub-mm Galaxies (SMG);Galaxy structure & evolution	Galaxy evolution	ocooper	Cooper, Olivia	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00705.S	ALMA	JAO	ALMA	uid://A001/X15bc/X98f.source.COS.0169.spw.7	image	2		COS.0169	149.9493750000203	1.6163055555556944	0.011153709239791759	Polygon ICRS 149.949375 1.610729 149.947321 1.611120 149.945556 1.612240 149.944327 1.613931 149.943971 1.614919 149.943796 1.616306 149.943971 1.617692 149.944327 1.618680 149.945556 1.620371 149.947321 1.621491 149.949375 1.621882 149.951429 1.621491 149.953194 1.620371 149.954423 1.618680 149.954779 1.617692 149.954954 1.616306 149.954562 1.614253 149.953889 1.613028 149.953194 1.612240 149.951429 1.611120			128	1	2	1.087197509709421	59706.991797	59707.022546	52.416	52.416	0.0021273042050909685	0.0021576909212714444	4509.077999996801	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X15bc/X98f	application/x-votable+xml; content=datalink		2021.1.00705.S	Public	237.33285644260081	41.64010667475675	4	4.784627714545597E-7	2.0E9	A001:DA57 A002:DA52 A003:DV18 A005:DV13 A006:DV17 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A017:DV16 A019:DV14 A022:DV02 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A033:DV01 A035:DA63 A036:DV08 A039:DV23 A040:DA50 A042:DA60 A043:DA55 A045:DA58 A047:DA42 A049:DA44 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A067:DA46 A068:DA54 A070:DA48 A072:DA53 A073:DA43 A074:DA56 A075:DV09 A076:DA51 A082:DA41 A083:DV22 A085:DA59 A088:DV11	F	2023-05-13T16:44:29.000	1.087197509709421	[137.05..139.03GHz,31250.00kHz,4.5mJy/beam@10km/s,215uJy/beam@native, XX YY] U [138.94..140.93GHz,31250.00kHz,4.2mJy/beam@10km/s,204.6uJy/beam@native, XX YY] U [149.05..151.03GHz,31250.00kHz,4.5mJy/beam@10km/s,225uJy/beam@native, XX YY] U [151.01..152.99GHz,31250.00kHz,4.8mJy/beam@10km/s,243.1uJy/beam@native, XX YY]	139.9336643180635	62048.56011849514	ALMA	A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z <SUB>ph</SUB> > 7 A photo-z cautionary tale: Redshift confirmation of COSBO-7 at z = 2.625 ALMACAL. XI. Over-densities as signposts for proto-clusters? A cautionary tale Resolved ALMA [C II] 158 μm Observations at Cosmic Noon: Interstellar Medium Structure and Dynamics of the Starbursting QSO SDSS J1000 The ALPINE-CRISTAL-JWST Survey: JWST/IFU Optical Observations for 18 Main-sequence Galaxies at z = 4─6	Chen, Jianhang Faisst, A. L. Jin, Shuowen Ling, Chenxiaoji Rooney, Christopher	Chen, Jianhang; Ivison, R. J.; Zwaan, Martin A.; Klitsch, Anne; Péroux, Céline; Lovell, Christopher C.; Lagos, Claudia del P.; Biggs, Andrew D.; Bollo, Victoria Faisst, A. L.; Fujimoto, S.; Tsujita, A.; Wang, W.; Nezhad, N.; Loiacono, F.; Übler, H.; Béthermin, M.; Cassata, P.; Dessauges-Zavadsky, M.; Herrera-Camus, R.; Schaerer, D.; Silverman, J. D.; Yan, L.; Aravena, M.; De Looze, I.; Förster Schreiber, N. M.; González-López, J.; Spilker, J.; Tadaki, K.; Casey, C. M.; Franco, M.; Harish, S.; McCracken, H. J.; Kartaltepe, J. S.; Koekemoer, A. M.; Khostovan, A. A.; Liu, D.; Rhodes, J.; Robertson, B. E.; Amorin, R.; Assef, R. J.; Battisti, A. J.; Birkin, J. E.; Boquien, M.; Da Cunha, E.; Dam, P.; Davies, R. L.; Gómez-Espinoza, D. A.; Ferrara, A.; Fudamoto, Y.; Gillman, S.; Ginolfi, M.; Gozaliasl, G.; Gruppioni, C.; Hadi, A.; Hathi, N.; Ibar, E.; Ikeda, R.; Inami, H.; Jones, G. C.; Kohandel, M.; Li, Y.; Lin, Y.-H.; Liu, Z.; Liu, L.-J.; Long, A. S.; Magdis, G.; Maraston, C.; Martin, C. L.; Mitsuhashi, I.; Mobashe	It may be unsurprising that the most common approach to finding proto-clusters is to search for over-densities of galaxies. Upgrades to submillimetre (submm) interferometers and the advent of the James Webb Space Telescope will soon offer the opportunity to find more distant candidate proto-clusters in deep sky surveys without any spectroscopic confirmation. In this Letter, we report the serendipitous discovery of an extremely dense region centred on the blazar, J0217−0820, at z = 0.6 in the ALMACAL sky survey. Its density is eight times higher than that predicted by blind submm surveys. Among the seven submm-bright galaxies, three are as bright as conventional single-dish submm galaxies, with S<SUB>870 μm</SUB> &gt; 3 mJy. The over-density is thus comparable to the densest known and confirmed proto-cluster cores. However, their spectra betray a wide range of redshifts. We investigate the likelihood of line-of-sight projection effects using light cones from cosmological simulations, finding that the deeper we	2023	Dusty Star-Forming Galaxies dominate cosmic star-formation at its peak (z~2) and yet little is known of their volume density toward higher redshifts, where their existence may place interesting constraints on the formation of massive galaxies (M*>10^11Msun). Empirical modeling suggests that 2mm imaging of existing, bright samples of DSFGs selected at 850um-1mm can quickly and easily separate DSFGs by redshift, isolating the `needle in the haystack' DSFGs that sit at z>4 or beyond. We propose 2mm dust continuum observations of a sample of 414/453 of the brightest SCUBA-2 850um-selected DSFGs (S850>5mJy) (the other 39 targets were observed in Cycle 7) with the goal of: (1) identifying the highest redshift candidate DSFGs for future follow-up with ALMA spectral scans and JWST, (2) inferring the volume density of z>3 DSFGs using the population's distribution in 2mm flux density combined with our models of (sub)mm emission from obscured galaxies, and (3) refining measurements of beta, the dust emissivity spectral	COS.0018_a_04_TM1	Sanders, David; da Cunha, Elisabete; Drew, Patrick; Long, Arianna; Spilker, Justin; Scoville, Nick; Champagne, Jaclyn; Staguhn, Johannes; Casey, Caitlin; Manning, Sinclaire; Zavala, Jorge; Hodge, Jacqueline; Kartaltepe, Jeyhan;	4.235964236648698	0.11030188003089186	2.976112	uid://A001/X15bc/X98e	uid://A001/X15bc/X98f	uid://A002/Xf89be2/Xac9d	Needle in a haystack: Identifying the highest-redshift candidate DSFGs using 2mm imaging	S	TARGET	T	12.521798584022807	T	2023A&A...675L..10C 2024A&A...690L..16J 2024ApJ...969L..28L 2025ApJ...987...61R 2026ApJS..282...19F	Sub-mm Galaxies (SMG);Galaxy structure & evolution	Galaxy evolution	ocooper	Cooper, Olivia	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00705.S	ALMA	JAO	ALMA	uid://A001/X15bc/X98f.source.COS.0169.spw.9	image	2		COS.0169	149.9493750000203	1.6163055555556944	0.011153709239791759	Polygon ICRS 149.949375 1.610729 149.947321 1.611120 149.945556 1.612240 149.944327 1.613931 149.943971 1.614919 149.943796 1.616306 149.943971 1.617692 149.944327 1.618680 149.945556 1.620371 149.947321 1.621491 149.949375 1.621882 149.951429 1.621491 149.953194 1.620371 149.954423 1.618680 149.954779 1.617692 149.954954 1.616306 149.954562 1.614253 149.953889 1.613028 149.953194 1.612240 149.951429 1.611120			128	1	2	1.087197509709421	59706.991797	59707.022546	52.416	52.416	0.001984963355949194	0.0020113944598807855	4768.921999996801	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X15bc/X98f	application/x-votable+xml; content=datalink		2021.1.00705.S	Public	237.33285644260081	41.64010667475675	4	4.1617794563799747E-7	2.0E9	A001:DA57 A002:DA52 A003:DV18 A005:DV13 A006:DV17 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A017:DV16 A019:DV14 A022:DV02 A023:DA47 A024:DV06 A025:DV19 A026:DV07 A027:DV03 A033:DV01 A035:DA63 A036:DV08 A039:DV23 A040:DA50 A042:DA60 A043:DA55 A045:DA58 A047:DA42 A049:DA44 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A067:DA46 A068:DA54 A070:DA48 A072:DA53 A073:DA43 A074:DA56 A075:DV09 A076:DA51 A082:DA41 A083:DV22 A085:DA59 A088:DV11	F	2023-05-13T16:44:29.000	1.087197509709421	[137.05..139.03GHz,31250.00kHz,4.5mJy/beam@10km/s,215uJy/beam@native, XX YY] U [138.94..140.93GHz,31250.00kHz,4.2mJy/beam@10km/s,204.6uJy/beam@native, XX YY] U [149.05..151.03GHz,31250.00kHz,4.5mJy/beam@10km/s,225uJy/beam@native, XX YY] U [151.01..152.99GHz,31250.00kHz,4.8mJy/beam@10km/s,243.1uJy/beam@native, XX YY]	150.0394038819589	62048.56011849514	ALMA	A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z <SUB>ph</SUB> > 7 A photo-z cautionary tale: Redshift confirmation of COSBO-7 at z = 2.625 ALMACAL. XI. Over-densities as signposts for proto-clusters? A cautionary tale Resolved ALMA [C II] 158 μm Observations at Cosmic Noon: Interstellar Medium Structure and Dynamics of the Starbursting QSO SDSS J1000 The ALPINE-CRISTAL-JWST Survey: JWST/IFU Optical Observations for 18 Main-sequence Galaxies at z = 4─6	Chen, Jianhang Faisst, A. L. Jin, Shuowen Ling, Chenxiaoji Rooney, Christopher	Chen, Jianhang; Ivison, R. J.; Zwaan, Martin A.; Klitsch, Anne; Péroux, Céline; Lovell, Christopher C.; Lagos, Claudia del P.; Biggs, Andrew D.; Bollo, Victoria Faisst, A. L.; Fujimoto, S.; Tsujita, A.; Wang, W.; Nezhad, N.; Loiacono, F.; Übler, H.; Béthermin, M.; Cassata, P.; Dessauges-Zavadsky, M.; Herrera-Camus, R.; Schaerer, D.; Silverman, J. D.; Yan, L.; Aravena, M.; De Looze, I.; Förster Schreiber, N. M.; González-López, J.; Spilker, J.; Tadaki, K.; Casey, C. M.; Franco, M.; Harish, S.; McCracken, H. J.; Kartaltepe, J. S.; Koekemoer, A. M.; Khostovan, A. A.; Liu, D.; Rhodes, J.; Robertson, B. E.; Amorin, R.; Assef, R. J.; Battisti, A. J.; Birkin, J. E.; Boquien, M.; Da Cunha, E.; Dam, P.; Davies, R. L.; Gómez-Espinoza, D. A.; Ferrara, A.; Fudamoto, Y.; Gillman, S.; Ginolfi, M.; Gozaliasl, G.; Gruppioni, C.; Hadi, A.; Hathi, N.; Ibar, E.; Ikeda, R.; Inami, H.; Jones, G. C.; Kohandel, M.; Li, Y.; Lin, Y.-H.; Liu, Z.; Liu, L.-J.; Long, A. S.; Magdis, G.; Maraston, C.; Martin, C. L.; Mitsuhashi, I.; Mobashe	It may be unsurprising that the most common approach to finding proto-clusters is to search for over-densities of galaxies. Upgrades to submillimetre (submm) interferometers and the advent of the James Webb Space Telescope will soon offer the opportunity to find more distant candidate proto-clusters in deep sky surveys without any spectroscopic confirmation. In this Letter, we report the serendipitous discovery of an extremely dense region centred on the blazar, J0217−0820, at z = 0.6 in the ALMACAL sky survey. Its density is eight times higher than that predicted by blind submm surveys. Among the seven submm-bright galaxies, three are as bright as conventional single-dish submm galaxies, with S<SUB>870 μm</SUB> &gt; 3 mJy. The over-density is thus comparable to the densest known and confirmed proto-cluster cores. However, their spectra betray a wide range of redshifts. We investigate the likelihood of line-of-sight projection effects using light cones from cosmological simulations, finding that the deeper we	2023	Dusty Star-Forming Galaxies dominate cosmic star-formation at its peak (z~2) and yet little is known of their volume density toward higher redshifts, where their existence may place interesting constraints on the formation of massive galaxies (M*>10^11Msun). Empirical modeling suggests that 2mm imaging of existing, bright samples of DSFGs selected at 850um-1mm can quickly and easily separate DSFGs by redshift, isolating the `needle in the haystack' DSFGs that sit at z>4 or beyond. We propose 2mm dust continuum observations of a sample of 414/453 of the brightest SCUBA-2 850um-selected DSFGs (S850>5mJy) (the other 39 targets were observed in Cycle 7) with the goal of: (1) identifying the highest redshift candidate DSFGs for future follow-up with ALMA spectral scans and JWST, (2) inferring the volume density of z>3 DSFGs using the population's distribution in 2mm flux density combined with our models of (sub)mm emission from obscured galaxies, and (3) refining measurements of beta, the dust emissivity spectral	COS.0018_a_04_TM1	Sanders, David; da Cunha, Elisabete; Drew, Patrick; Long, Arianna; Spilker, Justin; Scoville, Nick; Champagne, Jaclyn; Staguhn, Johannes; Casey, Caitlin; Manning, Sinclaire; Zavala, Jorge; Hodge, Jacqueline; Kartaltepe, Jeyhan;	4.497271630176726	0.11030188003089186	2.976112	uid://A001/X15bc/X98e	uid://A001/X15bc/X98f	uid://A002/Xf89be2/Xac9d	Needle in a haystack: Identifying the highest-redshift candidate DSFGs using 2mm imaging	S	TARGET	T	12.521798584022807	T	2023A&A...675L..10C 2024A&A...690L..16J 2024ApJ...969L..28L 2025ApJ...987...61R 2026ApJS..282...19F	Sub-mm Galaxies (SMG);Galaxy structure & evolution	Galaxy evolution	ocooper	Cooper, Olivia	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00811.S	ALMA	JAO	ALMA	uid://A001/X3833/X25f2.source.J0006-0623.spw.25	cube	2		J0006-0623	1.5578875000011079	-6.393148611110001	0.011622139766829735	Circle ICRS 1.557888 -6.393149 0.005811			480	1	2	0.8725578759821971	61166.572796	61166.576296	302.4	302.4	0.0022199419323391117	0.0022511299924984126	34591.14405439768	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X25f2	application/x-votable+xml; content=datalink		2025.1.00811.S	Proprietary	93.50553584430406	-66.646516387736	4	6.508251379506109E-8	1.875E9	A001:DA63 A002:DA45 A006:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV14 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A044:DA57 A045:DA65 A047:DA42 A050:DV10 A058:DV12 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DV09 A073:DA41 A074:DA61 A075:DA50 A076:DA48 A082:DV22 A083:DA56 A086:DV05 A087:DV04 A088:DA46 A092:DA54 A094:DV08	F	2027-05-12T22:41:41.000	0.8725578759821971	[131.18..133.17GHz,31250.00kHz,1.5mJy/beam@10km/s,71.1uJy/beam@native, XX YY] U [133.17..135.05GHz,3904.30kHz,1.5mJy/beam@10km/s,73.5uJy/beam@native, XX YY] U [143.18..145.16GHz,31250.00kHz,1.4mJy/beam@10km/s,71uJy/beam@native, XX YY] U [145.18..147.16GHz,31250.00kHz,1.5mJy/beam@10km/s,76.4uJy/beam@native, XX YY]	134.10969495594446	8666.740178600321	ALMA						Active Galactic Nuclei (AGNs) play a key role in galaxy evolution via feedback processes, yet the impact of different levels of radio emission on cold gas reservoirs of AGN host galaxies remains poorly understood. Preliminary analysis reveals that radio-detected radio-quiet AGNs exhibit systematically lower dust masses compared to that of radio-loud and radio-undetected AGNs, which may indicate lower gas masses in the host galaxies of AGNs with moderate radio activity. To check the connection between the gas content and AGN radio activity, investigating if AGN feedback can expel molecular gas more efficiently with moderate radio activity, we propose here ALMA observations of the 12CO(2-1) line from a sample of 18 AGNs at 0.4	SDSS_J00_a_04_TM1	Ho, Luis; Wen, Yuhan; Wang, Ran; Bauer, Franz; Shangguan, Jinyi;	1.5048799104838324	0.036440892021855874	3.8821287	uid://A001/X3833/X25f1	uid://A001/X3833/X25f2	uid://A002/X13a2059/X52ba	Probing the Feedback on Molecular Gas Content in Quasars with Different Radio Activity Levels	S	BANDPASS FLUX WVR	F	10.59758142976411	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Outflows, jets, feedback	Active galaxies	ezetre	Treister, Ezequiel	3904.296875	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00811.S	ALMA	JAO	ALMA	uid://A001/X3833/X25f2.source.J0006-0623.spw.17	image	2		J0006-0623	1.5578875000011079	-6.393148611110001	0.011622139766829735	Circle ICRS 1.557888 -6.393149 0.005811			128	1	2	0.8725578759821971	61166.572796	61166.576296	302.4	302.4	0.002251263496970152	0.0022853158346658707	4261.603323625225	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X25f2	application/x-votable+xml; content=datalink		2025.1.00811.S	Proprietary	93.50553584430406	-66.646516387736	4	5.362926897779844E-7	2.0E9	A001:DA63 A002:DA45 A006:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV14 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A044:DA57 A045:DA65 A047:DA42 A050:DV10 A058:DV12 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DV09 A073:DA41 A074:DA61 A075:DA50 A076:DA48 A082:DV22 A083:DA56 A086:DV05 A087:DV04 A088:DA46 A092:DA54 A094:DV08	F	2027-05-12T22:41:41.000	0.8725578759821971	[131.18..133.17GHz,31250.00kHz,1.5mJy/beam@10km/s,71.1uJy/beam@native, XX YY] U [133.17..135.05GHz,3904.30kHz,1.5mJy/beam@10km/s,73.5uJy/beam@native, XX YY] U [143.18..145.16GHz,31250.00kHz,1.4mJy/beam@10km/s,71uJy/beam@native, XX YY] U [145.18..147.16GHz,31250.00kHz,1.5mJy/beam@10km/s,76.4uJy/beam@native, XX YY]	132.17419034027404	8666.740178600321	ALMA						Active Galactic Nuclei (AGNs) play a key role in galaxy evolution via feedback processes, yet the impact of different levels of radio emission on cold gas reservoirs of AGN host galaxies remains poorly understood. Preliminary analysis reveals that radio-detected radio-quiet AGNs exhibit systematically lower dust masses compared to that of radio-loud and radio-undetected AGNs, which may indicate lower gas masses in the host galaxies of AGNs with moderate radio activity. To check the connection between the gas content and AGN radio activity, investigating if AGN feedback can expel molecular gas more efficiently with moderate radio activity, we propose here ALMA observations of the 12CO(2-1) line from a sample of 18 AGNs at 0.4	SDSS_J00_a_04_TM1	Ho, Luis; Wen, Yuhan; Wang, Ran; Bauer, Franz; Shangguan, Jinyi;	1.5132846814526517	0.036440892021855874	3.8821287	uid://A001/X3833/X25f1	uid://A001/X3833/X25f2	uid://A002/X13a2059/X52ba	Probing the Feedback on Molecular Gas Content in Quasars with Different Radio Activity Levels	S	BANDPASS FLUX WVR	F	10.59758142976411	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Outflows, jets, feedback	Active galaxies	ezetre	Treister, Ezequiel	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00811.S	ALMA	JAO	ALMA	uid://A001/X3833/X25f2.source.J0006-0623.spw.21	image	2		J0006-0623	1.5578875000011079	-6.393148611110001	0.011622139766829735	Circle ICRS 1.557888 -6.393149 0.005811			128	1	2	0.8725578759821971	61166.572796	61166.576296	302.4	302.4	0.0020651988156043188	0.002093819197064157	4582.053700957723	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X25f2	application/x-votable+xml; content=datalink		2025.1.00811.S	Proprietary	93.50553584430406	-66.646516387736	4	4.5074442444221725E-7	2.0E9	A001:DA63 A002:DA45 A006:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV14 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A044:DA57 A045:DA65 A047:DA42 A050:DV10 A058:DV12 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DV09 A073:DA41 A074:DA61 A075:DA50 A076:DA48 A082:DV22 A083:DA56 A086:DV05 A087:DV04 A088:DA46 A092:DA54 A094:DV08	F	2027-05-12T22:41:41.000	0.8725578759821971	[131.18..133.17GHz,31250.00kHz,1.5mJy/beam@10km/s,71.1uJy/beam@native, XX YY] U [133.17..135.05GHz,3904.30kHz,1.5mJy/beam@10km/s,73.5uJy/beam@native, XX YY] U [143.18..145.16GHz,31250.00kHz,1.4mJy/beam@10km/s,71uJy/beam@native, XX YY] U [145.18..147.16GHz,31250.00kHz,1.5mJy/beam@10km/s,76.4uJy/beam@native, XX YY]	144.17184755720828	8666.740178600321	ALMA						Active Galactic Nuclei (AGNs) play a key role in galaxy evolution via feedback processes, yet the impact of different levels of radio emission on cold gas reservoirs of AGN host galaxies remains poorly understood. Preliminary analysis reveals that radio-detected radio-quiet AGNs exhibit systematically lower dust masses compared to that of radio-loud and radio-undetected AGNs, which may indicate lower gas masses in the host galaxies of AGNs with moderate radio activity. To check the connection between the gas content and AGN radio activity, investigating if AGN feedback can expel molecular gas more efficiently with moderate radio activity, we propose here ALMA observations of the 12CO(2-1) line from a sample of 18 AGNs at 0.4	SDSS_J00_a_04_TM1	Ho, Luis; Wen, Yuhan; Wang, Ran; Bauer, Franz; Shangguan, Jinyi;	1.4472987691823544	0.036440892021855874	3.8821287	uid://A001/X3833/X25f1	uid://A001/X3833/X25f2	uid://A002/X13a2059/X52ba	Probing the Feedback on Molecular Gas Content in Quasars with Different Radio Activity Levels	S	BANDPASS FLUX WVR	F	10.59758142976411	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Outflows, jets, feedback	Active galaxies	ezetre	Treister, Ezequiel	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00811.S	ALMA	JAO	ALMA	uid://A001/X3833/X25f2.source.J0006-0623.spw.23	image	2		J0006-0623	1.5578875000011079	-6.393148611110001	0.011622139766829735	Circle ICRS 1.557888 -6.393149 0.005811			128	1	2	0.8725578759821971	61166.572796	61166.576296	302.4	302.4	0.0020371375842100597	0.002064980238469908	4646.045430513672	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X25f2	application/x-votable+xml; content=datalink		2025.1.00811.S	Proprietary	93.50553584430406	-66.646516387736	4	4.3849594342093383E-7	2.0E9	A001:DA63 A002:DA45 A006:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV14 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A040:DV24 A044:DA57 A045:DA65 A047:DA42 A050:DV10 A058:DV12 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DV09 A073:DA41 A074:DA61 A075:DA50 A076:DA48 A082:DV22 A083:DA56 A086:DV05 A087:DV04 A088:DA46 A092:DA54 A094:DV08	F	2027-05-12T22:41:41.000	0.8725578759821971	[131.18..133.17GHz,31250.00kHz,1.5mJy/beam@10km/s,71.1uJy/beam@native, XX YY] U [133.17..135.05GHz,3904.30kHz,1.5mJy/beam@10km/s,73.5uJy/beam@native, XX YY] U [143.18..145.16GHz,31250.00kHz,1.4mJy/beam@10km/s,71uJy/beam@native, XX YY] U [145.18..147.16GHz,31250.00kHz,1.5mJy/beam@10km/s,76.4uJy/beam@native, XX YY]	146.17145709338064	8666.740178600321	ALMA						Active Galactic Nuclei (AGNs) play a key role in galaxy evolution via feedback processes, yet the impact of different levels of radio emission on cold gas reservoirs of AGN host galaxies remains poorly understood. Preliminary analysis reveals that radio-detected radio-quiet AGNs exhibit systematically lower dust masses compared to that of radio-loud and radio-undetected AGNs, which may indicate lower gas masses in the host galaxies of AGNs with moderate radio activity. To check the connection between the gas content and AGN radio activity, investigating if AGN feedback can expel molecular gas more efficiently with moderate radio activity, we propose here ALMA observations of the 12CO(2-1) line from a sample of 18 AGNs at 0.4	SDSS_J00_a_04_TM1	Ho, Luis; Wen, Yuhan; Wang, Ran; Bauer, Franz; Shangguan, Jinyi;	1.5472889336322073	0.036440892021855874	3.8821287	uid://A001/X3833/X25f1	uid://A001/X3833/X25f2	uid://A002/X13a2059/X52ba	Probing the Feedback on Molecular Gas Content in Quasars with Different Radio Activity Levels	S	BANDPASS FLUX WVR	F	10.59758142976411	T		Active Galactic Nuclei (AGN)/Quasars (QSO);Outflows, jets, feedback	Active galaxies	ezetre	Treister, Ezequiel	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00383.L	ALMA	JAO	ALMA	uid://A001/X3833/X65a6.source.AG326.7806-0.2413.spw.19	cube	2		AG326.7806-0.2413	237.22098303839275	-54.670830204575125	0.018426929401962725	Polygon ICRS 237.231141 -54.677929 237.225908 -54.679593 237.219982 -54.680025 237.217020 -54.679754 237.213306 -54.678904 237.208705 -54.676702 237.206565 -54.674752 237.205550 -54.673121 237.205176 -54.669674 237.207023 -54.666391 237.210829 -54.663731 237.216061 -54.662068 237.221983 -54.661635 237.227765 -54.662493 237.230346 -54.663376 237.233258 -54.664957 237.235398 -54.666906 237.236414 -54.668538 237.236791 -54.671984 237.234947 -54.675268			1024	1	2	66.33684210724057	61068.390607	61093.298537	1505.28	1505.28	0.003450155998673306	0.003452641841104172	1231629.493893182	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X65a6	application/x-votable+xml; content=datalink		2025.1.00383.L	Proprietary	326.7805933445276	-0.2327648556082027	3	2.8035444955166685E-9	6.25E7	T702:PM03 T703:PM01	F	2027-02-24T13:15:19.000	59.879273406535745	[86.32..86.39GHz,70.56kHz,38.5mJy/beam@10km/s,8.3mJy/beam@native, XX YY] U [86.74..86.80GHz,35.28kHz,38.3mJy/beam@10km/s,8.2mJy/beam@native, XX YY] U [86.83..86.89GHz,70.56kHz,39.5mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [87.07..87.14GHz,70.56kHz,37mJy/beam@10km/s,8mJy/beam@native, XX YY] U [88.61..88.68GHz,70.56kHz,36.8mJy/beam@10km/s,8mJy/beam@native, XX YY] U [89.17..89.23GHz,35.28kHz,38.6mJy/beam@10km/s,8.4mJy/beam@native, XX YY]	86.86115509617568	118.51157980460516	ALMA						Star formation is a multi-scale process that spans many orders of magnitude in spatial scales and gas densities. Among the hierarchy of the various interstellar structures that exist, the formation of clumps, i.e. the parsec-scale progenitors of star clusters, has been identified as a pivotal stage of the star formation process. The study of molecular gas propertes on clump to cloud scale indeed showed that clumps are dynamically decoupled from the rest of their parent molecular clouds. Understanding the origin of this decoupling, along with its impact on the determination of the core and stellar mass functions, must therefore be at the centre of any research that attempts to solve the star cluster formation puzzle. Here we popose to map the density structure and velocity field of 259 clumps, all located at a distance of 2.5 to 5kpc, for which uniform datasets on both larger-scale (parent molecular clouds) and smaller-scale (cores) exist. The proposed ALMA observations will threfore provide, for the first tim	AG323.74_b_03_TP	Bronfman, Leonardo; Wyrowski, Friedrich; Molinari, Sergio; Elia, Davide; Anderson, Michael; Lebreuilly, Ugo; Giannetti, Andrea; De Angelis, Fabrizio; Ramkumar, Ria; Beuther, Henrik; Schilke, Peter; Watkins, Elizabeth; Koch, Patrick; Benedettini, Milena; Fuller, Gary; Williams, Gwenllian; Ginsburg, Adam; Zhang, Qizhou; Kim, Wonju; Beltran, Maite; Walker, Daniel; Soler, Juan; Nucara, Alice; Allande, Jofre; Riley, Huw; Avison, Adam; Barnes, Peter; Neupane, Sudeep; Csengeri, Timea; Motte, Frederique; Sanchez-Monge, Alvaro; Sottie, Stephen; Leurini, Silvia; Coletta, Alessandro; Lee, Min-Young; Ragan, Sarah; Hennebelle, Patrick; Ngo, Duy Tung; Figueira Sebastião, Miguel; Yang, Aiyuan; Urquhart, James; Brogan, Crystal; Zhou, Jixuan; Colombo, Dario; Das, Swagat; Rigby, Andrew; Duarte Cabral, Ana; Henning, Thomas; Anderson, Loren; Jones, Beth; Cunningham, Nichol; Priestley, Felix; Arzoumanian, Doris; Dann, Eleonore; Schisano, Eugenio; Eden, David; Kauffmann, Jens; Klessen, Ralf; Colman, Tine; González, Matthias; Batte	39.54967250823538	3.3594570655806084	2.1471107	uid://A001/X3833/X65a1	uid://A001/X3833/X65a6	uid://A002/X1359e83/Xa3bb	Panta Rei: Following the flow of star cluster formation	L	TARGET	T	1061.3911314040772	T		High-mass star formation;null	ISM and star formation	nperetto	Peretto, Nicolas	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00383.L	ALMA	JAO	ALMA	uid://A001/X3833/X65a6.source.AG326.7806-0.2413.spw.17	cube	2		AG326.7806-0.2413	237.22098303839275	-54.670830204575125	0.018426929401962725	Polygon ICRS 237.231141 -54.677929 237.225908 -54.679593 237.219982 -54.680025 237.217020 -54.679754 237.213306 -54.678904 237.208705 -54.676702 237.206565 -54.674752 237.205550 -54.673121 237.205176 -54.669674 237.207023 -54.666391 237.210829 -54.663731 237.216061 -54.662068 237.221983 -54.661635 237.227765 -54.662493 237.230346 -54.663376 237.233258 -54.664957 237.235398 -54.666906 237.236414 -54.668538 237.236791 -54.671984 237.234947 -54.675268			1024	1	2	66.33684210724057	61068.390607	61093.298537	1505.28	1505.28	0.003470416648709523	0.00347293155884386	1224439.1824744968	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X65a6	application/x-votable+xml; content=datalink		2025.1.00383.L	Proprietary	326.7805933445276	-0.2327648556082027	3	2.8365799886234936E-9	6.25E7	T702:PM03 T703:PM01	F	2027-02-24T13:15:19.000	59.879273406535745	[86.32..86.39GHz,70.56kHz,38.5mJy/beam@10km/s,8.3mJy/beam@native, XX YY] U [86.74..86.80GHz,35.28kHz,38.3mJy/beam@10km/s,8.2mJy/beam@native, XX YY] U [86.83..86.89GHz,70.56kHz,39.5mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [87.07..87.14GHz,70.56kHz,37mJy/beam@10km/s,8mJy/beam@native, XX YY] U [88.61..88.68GHz,70.56kHz,36.8mJy/beam@10km/s,8mJy/beam@native, XX YY] U [89.17..89.23GHz,35.28kHz,38.6mJy/beam@10km/s,8.4mJy/beam@native, XX YY]	86.35387089019042	118.51157980460516	ALMA						Star formation is a multi-scale process that spans many orders of magnitude in spatial scales and gas densities. Among the hierarchy of the various interstellar structures that exist, the formation of clumps, i.e. the parsec-scale progenitors of star clusters, has been identified as a pivotal stage of the star formation process. The study of molecular gas propertes on clump to cloud scale indeed showed that clumps are dynamically decoupled from the rest of their parent molecular clouds. Understanding the origin of this decoupling, along with its impact on the determination of the core and stellar mass functions, must therefore be at the centre of any research that attempts to solve the star cluster formation puzzle. Here we popose to map the density structure and velocity field of 259 clumps, all located at a distance of 2.5 to 5kpc, for which uniform datasets on both larger-scale (parent molecular clouds) and smaller-scale (cores) exist. The proposed ALMA observations will threfore provide, for the first tim	AG323.74_b_03_TP	Bronfman, Leonardo; Wyrowski, Friedrich; Molinari, Sergio; Elia, Davide; Anderson, Michael; Lebreuilly, Ugo; Giannetti, Andrea; De Angelis, Fabrizio; Ramkumar, Ria; Beuther, Henrik; Schilke, Peter; Watkins, Elizabeth; Koch, Patrick; Benedettini, Milena; Fuller, Gary; Williams, Gwenllian; Ginsburg, Adam; Zhang, Qizhou; Kim, Wonju; Beltran, Maite; Walker, Daniel; Soler, Juan; Nucara, Alice; Allande, Jofre; Riley, Huw; Avison, Adam; Barnes, Peter; Neupane, Sudeep; Csengeri, Timea; Motte, Frederique; Sanchez-Monge, Alvaro; Sottie, Stephen; Leurini, Silvia; Coletta, Alessandro; Lee, Min-Young; Ragan, Sarah; Hennebelle, Patrick; Ngo, Duy Tung; Figueira Sebastião, Miguel; Yang, Aiyuan; Urquhart, James; Brogan, Crystal; Zhou, Jixuan; Colombo, Dario; Das, Swagat; Rigby, Andrew; Duarte Cabral, Ana; Henning, Thomas; Anderson, Loren; Jones, Beth; Cunningham, Nichol; Priestley, Felix; Arzoumanian, Doris; Dann, Eleonore; Schisano, Eugenio; Eden, David; Kauffmann, Jens; Klessen, Ralf; Colman, Tine; González, Matthias; Batte	38.53574776296905	3.3594570655806084	2.1471107	uid://A001/X3833/X65a1	uid://A001/X3833/X65a6	uid://A002/X1359e83/Xa3bb	Panta Rei: Following the flow of star cluster formation	L	TARGET	T	1061.3911314040772	T		High-mass star formation;null	ISM and star formation	nperetto	Peretto, Nicolas	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00383.L	ALMA	JAO	ALMA	uid://A001/X3833/X65a6.source.AG326.7806-0.2413.spw.21	cube	2		AG326.7806-0.2413	237.22098303839275	-54.670830204575125	0.018426929401962725	Polygon ICRS 237.231141 -54.677929 237.225908 -54.679593 237.219982 -54.680025 237.217020 -54.679754 237.213306 -54.678904 237.208705 -54.676702 237.206565 -54.674752 237.205550 -54.673121 237.205176 -54.669674 237.207023 -54.666391 237.210829 -54.663731 237.216061 -54.662068 237.221983 -54.661635 237.227765 -54.662493 237.230346 -54.663376 237.233258 -54.664957 237.235398 -54.666906 237.236414 -54.668538 237.236791 -54.671984 237.234947 -54.675268			2048	1	2	66.33684210724057	61068.390607	61093.298537	1505.28	1505.28	0.003453837868337867	0.0034563301965012594	2460633.1227344605	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X65a6	application/x-votable+xml; content=datalink		2025.1.00383.L	Proprietary	326.7805933445276	-0.2327648556082027	3	1.4047672334842936E-9	6.25E7	T702:PM03 T703:PM01	F	2027-02-24T13:15:19.000	59.879273406535745	[86.32..86.39GHz,70.56kHz,38.5mJy/beam@10km/s,8.3mJy/beam@native, XX YY] U [86.74..86.80GHz,35.28kHz,38.3mJy/beam@10km/s,8.2mJy/beam@native, XX YY] U [86.83..86.89GHz,70.56kHz,39.5mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [87.07..87.14GHz,70.56kHz,37mJy/beam@10km/s,8mJy/beam@native, XX YY] U [88.61..88.68GHz,70.56kHz,36.8mJy/beam@10km/s,8mJy/beam@native, XX YY] U [89.17..89.23GHz,35.28kHz,38.6mJy/beam@10km/s,8.4mJy/beam@native, XX YY]	86.76851103650426	118.51157980460516	ALMA						Star formation is a multi-scale process that spans many orders of magnitude in spatial scales and gas densities. Among the hierarchy of the various interstellar structures that exist, the formation of clumps, i.e. the parsec-scale progenitors of star clusters, has been identified as a pivotal stage of the star formation process. The study of molecular gas propertes on clump to cloud scale indeed showed that clumps are dynamically decoupled from the rest of their parent molecular clouds. Understanding the origin of this decoupling, along with its impact on the determination of the core and stellar mass functions, must therefore be at the centre of any research that attempts to solve the star cluster formation puzzle. Here we popose to map the density structure and velocity field of 259 clumps, all located at a distance of 2.5 to 5kpc, for which uniform datasets on both larger-scale (parent molecular clouds) and smaller-scale (cores) exist. The proposed ALMA observations will threfore provide, for the first tim	AG323.74_b_03_TP	Bronfman, Leonardo; Wyrowski, Friedrich; Molinari, Sergio; Elia, Davide; Anderson, Michael; Lebreuilly, Ugo; Giannetti, Andrea; De Angelis, Fabrizio; Ramkumar, Ria; Beuther, Henrik; Schilke, Peter; Watkins, Elizabeth; Koch, Patrick; Benedettini, Milena; Fuller, Gary; Williams, Gwenllian; Ginsburg, Adam; Zhang, Qizhou; Kim, Wonju; Beltran, Maite; Walker, Daniel; Soler, Juan; Nucara, Alice; Allande, Jofre; Riley, Huw; Avison, Adam; Barnes, Peter; Neupane, Sudeep; Csengeri, Timea; Motte, Frederique; Sanchez-Monge, Alvaro; Sottie, Stephen; Leurini, Silvia; Coletta, Alessandro; Lee, Min-Young; Ragan, Sarah; Hennebelle, Patrick; Ngo, Duy Tung; Figueira Sebastião, Miguel; Yang, Aiyuan; Urquhart, James; Brogan, Crystal; Zhou, Jixuan; Colombo, Dario; Das, Swagat; Rigby, Andrew; Duarte Cabral, Ana; Henning, Thomas; Anderson, Loren; Jones, Beth; Cunningham, Nichol; Priestley, Felix; Arzoumanian, Doris; Dann, Eleonore; Schisano, Eugenio; Eden, David; Kauffmann, Jens; Klessen, Ralf; Colman, Tine; González, Matthias; Batte	38.28880981548503	3.3594570655806084	2.1471107	uid://A001/X3833/X65a1	uid://A001/X3833/X65a6	uid://A002/X1359e83/Xa3bb	Panta Rei: Following the flow of star cluster formation	L	TARGET	T	1061.3911314040772	T		High-mass star formation;null	ISM and star formation	nperetto	Peretto, Nicolas	35.2783203125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00383.L	ALMA	JAO	ALMA	uid://A001/X3833/X65a6.source.AG326.7806-0.2413.spw.25	cube	2		AG326.7806-0.2413	237.22098303839275	-54.670830204575125	0.018426929401962725	Polygon ICRS 237.231141 -54.677929 237.225908 -54.679593 237.219982 -54.680025 237.217020 -54.679754 237.213306 -54.678904 237.208705 -54.676702 237.206565 -54.674752 237.205550 -54.673121 237.205176 -54.669674 237.207023 -54.666391 237.210829 -54.663731 237.216061 -54.662068 237.221983 -54.661635 237.227765 -54.662493 237.230346 -54.663376 237.233258 -54.664957 237.235398 -54.666906 237.236414 -54.668538 237.236791 -54.671984 237.234947 -54.675268			1024	1	2	66.33684210724057	61068.390607	61093.298537	1505.28	1505.28	0.0034404896963853753	0.0034429617302665877	1235089.8122322822	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X65a6	application/x-votable+xml; content=datalink		2025.1.00383.L	Proprietary	326.7805933445276	-0.2327648556082027	3	2.7878515786820466E-9	6.25E7	T702:PM03 T703:PM01	F	2027-02-24T13:15:19.000	59.879273406535745	[86.32..86.39GHz,70.56kHz,38.5mJy/beam@10km/s,8.3mJy/beam@native, XX YY] U [86.74..86.80GHz,35.28kHz,38.3mJy/beam@10km/s,8.2mJy/beam@native, XX YY] U [86.83..86.89GHz,70.56kHz,39.5mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [87.07..87.14GHz,70.56kHz,37mJy/beam@10km/s,8mJy/beam@native, XX YY] U [88.61..88.68GHz,70.56kHz,36.8mJy/beam@10km/s,8mJy/beam@native, XX YY] U [89.17..89.23GHz,35.28kHz,38.6mJy/beam@10km/s,8.4mJy/beam@native, XX YY]	87.10528427763853	118.51157980460516	ALMA						Star formation is a multi-scale process that spans many orders of magnitude in spatial scales and gas densities. Among the hierarchy of the various interstellar structures that exist, the formation of clumps, i.e. the parsec-scale progenitors of star clusters, has been identified as a pivotal stage of the star formation process. The study of molecular gas propertes on clump to cloud scale indeed showed that clumps are dynamically decoupled from the rest of their parent molecular clouds. Understanding the origin of this decoupling, along with its impact on the determination of the core and stellar mass functions, must therefore be at the centre of any research that attempts to solve the star cluster formation puzzle. Here we popose to map the density structure and velocity field of 259 clumps, all located at a distance of 2.5 to 5kpc, for which uniform datasets on both larger-scale (parent molecular clouds) and smaller-scale (cores) exist. The proposed ALMA observations will threfore provide, for the first tim	AG323.74_b_03_TP	Bronfman, Leonardo; Wyrowski, Friedrich; Molinari, Sergio; Elia, Davide; Anderson, Michael; Lebreuilly, Ugo; Giannetti, Andrea; De Angelis, Fabrizio; Ramkumar, Ria; Beuther, Henrik; Schilke, Peter; Watkins, Elizabeth; Koch, Patrick; Benedettini, Milena; Fuller, Gary; Williams, Gwenllian; Ginsburg, Adam; Zhang, Qizhou; Kim, Wonju; Beltran, Maite; Walker, Daniel; Soler, Juan; Nucara, Alice; Allande, Jofre; Riley, Huw; Avison, Adam; Barnes, Peter; Neupane, Sudeep; Csengeri, Timea; Motte, Frederique; Sanchez-Monge, Alvaro; Sottie, Stephen; Leurini, Silvia; Coletta, Alessandro; Lee, Min-Young; Ragan, Sarah; Hennebelle, Patrick; Ngo, Duy Tung; Figueira Sebastião, Miguel; Yang, Aiyuan; Urquhart, James; Brogan, Crystal; Zhou, Jixuan; Colombo, Dario; Das, Swagat; Rigby, Andrew; Duarte Cabral, Ana; Henning, Thomas; Anderson, Loren; Jones, Beth; Cunningham, Nichol; Priestley, Felix; Arzoumanian, Doris; Dann, Eleonore; Schisano, Eugenio; Eden, David; Kauffmann, Jens; Klessen, Ralf; Colman, Tine; González, Matthias; Batte	36.96240931295522	3.3594570655806084	2.1471107	uid://A001/X3833/X65a1	uid://A001/X3833/X65a6	uid://A002/X1359e83/Xa3bb	Panta Rei: Following the flow of star cluster formation	L	TARGET	T	1061.3911314040772	T		High-mass star formation;null	ISM and star formation	nperetto	Peretto, Nicolas	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00383.L	ALMA	JAO	ALMA	uid://A001/X3833/X65a6.source.AG326.7806-0.2413.spw.27	cube	2		AG326.7806-0.2413	237.22098303839275	-54.670830204575125	0.018426929401962725	Polygon ICRS 237.231141 -54.677929 237.225908 -54.679593 237.219982 -54.680025 237.217020 -54.679754 237.213306 -54.678904 237.208705 -54.676702 237.206565 -54.674752 237.205550 -54.673121 237.205176 -54.669674 237.207023 -54.666391 237.210829 -54.663731 237.216061 -54.662068 237.221983 -54.661635 237.227765 -54.662493 237.230346 -54.663376 237.233258 -54.664957 237.235398 -54.666906 237.236414 -54.668538 237.236791 -54.671984 237.234947 -54.675268			2048	1	2	66.33684210724057	61068.390607	61093.298537	1505.28	1505.28	0.003359609372715142	0.0033619685256963483	2529646.9635649105	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X65a6	application/x-votable+xml; content=datalink		2025.1.00383.L	Proprietary	326.7805933445276	-0.2327648556082027	3	1.3291366199317157E-9	6.25E7	T702:PM03 T703:PM01	F	2027-02-24T13:15:19.000	59.879273406535745	[86.32..86.39GHz,70.56kHz,38.5mJy/beam@10km/s,8.3mJy/beam@native, XX YY] U [86.74..86.80GHz,35.28kHz,38.3mJy/beam@10km/s,8.2mJy/beam@native, XX YY] U [86.83..86.89GHz,70.56kHz,39.5mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [87.07..87.14GHz,70.56kHz,37mJy/beam@10km/s,8mJy/beam@native, XX YY] U [88.61..88.68GHz,70.56kHz,36.8mJy/beam@10km/s,8mJy/beam@native, XX YY] U [89.17..89.23GHz,35.28kHz,38.6mJy/beam@10km/s,8.4mJy/beam@native, XX YY]	89.2030113946313	118.51157980460516	ALMA						Star formation is a multi-scale process that spans many orders of magnitude in spatial scales and gas densities. Among the hierarchy of the various interstellar structures that exist, the formation of clumps, i.e. the parsec-scale progenitors of star clusters, has been identified as a pivotal stage of the star formation process. The study of molecular gas propertes on clump to cloud scale indeed showed that clumps are dynamically decoupled from the rest of their parent molecular clouds. Understanding the origin of this decoupling, along with its impact on the determination of the core and stellar mass functions, must therefore be at the centre of any research that attempts to solve the star cluster formation puzzle. Here we popose to map the density structure and velocity field of 259 clumps, all located at a distance of 2.5 to 5kpc, for which uniform datasets on both larger-scale (parent molecular clouds) and smaller-scale (cores) exist. The proposed ALMA observations will threfore provide, for the first tim	AG323.74_b_03_TP	Bronfman, Leonardo; Wyrowski, Friedrich; Molinari, Sergio; Elia, Davide; Anderson, Michael; Lebreuilly, Ugo; Giannetti, Andrea; De Angelis, Fabrizio; Ramkumar, Ria; Beuther, Henrik; Schilke, Peter; Watkins, Elizabeth; Koch, Patrick; Benedettini, Milena; Fuller, Gary; Williams, Gwenllian; Ginsburg, Adam; Zhang, Qizhou; Kim, Wonju; Beltran, Maite; Walker, Daniel; Soler, Juan; Nucara, Alice; Allande, Jofre; Riley, Huw; Avison, Adam; Barnes, Peter; Neupane, Sudeep; Csengeri, Timea; Motte, Frederique; Sanchez-Monge, Alvaro; Sottie, Stephen; Leurini, Silvia; Coletta, Alessandro; Lee, Min-Young; Ragan, Sarah; Hennebelle, Patrick; Ngo, Duy Tung; Figueira Sebastião, Miguel; Yang, Aiyuan; Urquhart, James; Brogan, Crystal; Zhou, Jixuan; Colombo, Dario; Das, Swagat; Rigby, Andrew; Duarte Cabral, Ana; Henning, Thomas; Anderson, Loren; Jones, Beth; Cunningham, Nichol; Priestley, Felix; Arzoumanian, Doris; Dann, Eleonore; Schisano, Eugenio; Eden, David; Kauffmann, Jens; Klessen, Ralf; Colman, Tine; González, Matthias; Batte	38.5844206800402	3.3594570655806084	2.1471107	uid://A001/X3833/X65a1	uid://A001/X3833/X65a6	uid://A002/X1359e83/Xa3bb	Panta Rei: Following the flow of star cluster formation	L	TARGET	T	1061.3911314040772	T		High-mass star formation;null	ISM and star formation	nperetto	Peretto, Nicolas	35.2783203125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.00383.L	ALMA	JAO	ALMA	uid://A001/X3833/X65a6.source.AG326.7806-0.2413.spw.23	cube	2		AG326.7806-0.2413	237.22098303839275	-54.670830204575125	0.018426929401962725	Polygon ICRS 237.231141 -54.677929 237.225908 -54.679593 237.219982 -54.680025 237.217020 -54.679754 237.213306 -54.678904 237.208705 -54.676702 237.206565 -54.674752 237.205550 -54.673121 237.205176 -54.669674 237.207023 -54.666391 237.210829 -54.663731 237.216061 -54.662068 237.221983 -54.661635 237.227765 -54.662493 237.230346 -54.663376 237.233258 -54.664957 237.235398 -54.666906 237.236414 -54.668538 237.236791 -54.671984 237.234947 -54.675268			1024	1	2	66.33684210724057	61068.390607	61093.298537	1505.28	1505.28	0.0033807060846737257	0.0033830935712337046	1256930.6426821093	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3833/X65a6	application/x-votable+xml; content=datalink		2025.1.00383.L	Proprietary	326.7805933445276	-0.2327648556082027	3	2.691774142988126E-9	6.25E7	T702:PM03 T703:PM01	F	2027-02-24T13:15:19.000	59.879273406535745	[86.32..86.39GHz,70.56kHz,38.5mJy/beam@10km/s,8.3mJy/beam@native, XX YY] U [86.74..86.80GHz,35.28kHz,38.3mJy/beam@10km/s,8.2mJy/beam@native, XX YY] U [86.83..86.89GHz,70.56kHz,39.5mJy/beam@10km/s,8.5mJy/beam@native, XX YY] U [87.07..87.14GHz,70.56kHz,37mJy/beam@10km/s,8mJy/beam@native, XX YY] U [88.61..88.68GHz,70.56kHz,36.8mJy/beam@10km/s,8mJy/beam@native, XX YY] U [89.17..89.23GHz,35.28kHz,38.6mJy/beam@10km/s,8.4mJy/beam@native, XX YY]	88.64617836242147	118.51157980460516	ALMA						Star formation is a multi-scale process that spans many orders of magnitude in spatial scales and gas densities. Among the hierarchy of the various interstellar structures that exist, the formation of clumps, i.e. the parsec-scale progenitors of star clusters, has been identified as a pivotal stage of the star formation process. The study of molecular gas propertes on clump to cloud scale indeed showed that clumps are dynamically decoupled from the rest of their parent molecular clouds. Understanding the origin of this decoupling, along with its impact on the determination of the core and stellar mass functions, must therefore be at the centre of any research that attempts to solve the star cluster formation puzzle. Here we popose to map the density structure and velocity field of 259 clumps, all located at a distance of 2.5 to 5kpc, for which uniform datasets on both larger-scale (parent molecular clouds) and smaller-scale (cores) exist. The proposed ALMA observations will threfore provide, for the first tim	AG323.74_b_03_TP	Bronfman, Leonardo; Wyrowski, Friedrich; Molinari, Sergio; Elia, Davide; Anderson, Michael; Lebreuilly, Ugo; Giannetti, Andrea; De Angelis, Fabrizio; Ramkumar, Ria; Beuther, Henrik; Schilke, Peter; Watkins, Elizabeth; Koch, Patrick; Benedettini, Milena; Fuller, Gary; Williams, Gwenllian; Ginsburg, Adam; Zhang, Qizhou; Kim, Wonju; Beltran, Maite; Walker, Daniel; Soler, Juan; Nucara, Alice; Allande, Jofre; Riley, Huw; Avison, Adam; Barnes, Peter; Neupane, Sudeep; Csengeri, Timea; Motte, Frederique; Sanchez-Monge, Alvaro; Sottie, Stephen; Leurini, Silvia; Coletta, Alessandro; Lee, Min-Young; Ragan, Sarah; Hennebelle, Patrick; Ngo, Duy Tung; Figueira Sebastião, Miguel; Yang, Aiyuan; Urquhart, James; Brogan, Crystal; Zhou, Jixuan; Colombo, Dario; Das, Swagat; Rigby, Andrew; Duarte Cabral, Ana; Henning, Thomas; Anderson, Loren; Jones, Beth; Cunningham, Nichol; Priestley, Felix; Arzoumanian, Doris; Dann, Eleonore; Schisano, Eugenio; Eden, David; Kauffmann, Jens; Klessen, Ralf; Colman, Tine; González, Matthias; Batte	36.78572150310336	3.3594570655806084	2.1471107	uid://A001/X3833/X65a1	uid://A001/X3833/X65a6	uid://A002/X1359e83/Xa3bb	Panta Rei: Following the flow of star cluster formation	L	TARGET	T	1061.3911314040772	T		High-mass star formation;null	ISM and star formation	nperetto	Peretto, Nicolas	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.01115.S	ALMA	JAO	ALMA	uid://A001/X133f/X1d2.source.J0103-6439.spw.22	cube	2		J0103-6439	15.89059026673098	-64.65213476670343	0.012200837933907685	Circle ICRS 15.890590 -64.652135 0.006100			4096	1	2	5.696465331123022	58432.140747	58432.184977	483.84	483.84	0.001360377986897885	0.0013611499303010617	3610309.344988575	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133f/X1d2	application/x-votable+xml; content=datalink		2018.1.01115.S	Public	300.8043854174813	-52.426050860288555	6	3.769857365585245E-10	1.25E8	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2019-11-20T20:16:45.000	5.696465331123022	[219.22..219.72GHz,244.14kHz,10mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [220.25..220.37GHz,61.04kHz,13.5mJy/beam@10km/s,3.3mJy/beam@native, XX YY] U [230.38..230.51GHz,61.04kHz,12.3mJy/beam@10km/s,3mJy/beam@native, XX YY] U [233.31..235.31GHz,976.56kHz,10.7mJy/beam@10km/s,671.6uJy/beam@native, XX YY]	220.3118918786832	79.42982247020859	ALMA	Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates	Nakano, Satoya	Nakano, Satoya; Tachihara, Kengo; Tamashiro, Mao	We present identifications and kinematic analysis of 7426 massive (≥8M<SUB>⊙</SUB>) stars in the Small Magellanic Cloud (SMC), using Gaia DR3 data. We used the Gaia (G<SUB>BP</SUB> ‑ G<SUB>RP</SUB>, G) color–magnitude diagram to select the population of massive stars, and parallax to omit foreground objects. The spatial distribution of the 7426 massive star candidates is generally consistent with the spatial distribution of the interstellar medium, such as Hα and H I emission. The identified massive stars show inhomogeneous distributions over the galaxy, showing several superstructures formed by massive stars with a several hundred parsec scale. The stellar superstructures defined by the surface density have opposite mean proper motions in the east and west, moving away from each other. Similarly, the mean line-of-sight velocities of the superstructures are larger to the southeast and smaller to the northwest. The different east–west properties of the superstructures' proper-motion, line-of-sight velocity ind	2025	The Small Magellanic Cloud (SMC) is the only laboratory to study the low metallicity ISM at high spatial resolution, and yet we still do not know where the CO emission exists. We propose to use the ACA in standalone mode to map a 1.0 x 0.5 degree (1 kpc x 500 pc) region of the SW Bar of the SMC in 12CO, 13CO, C18O (2-1) covering a large fraction of the recent star formation, dust, and HI gas. With this new map we will be able to catalog CO clouds and clumps down to a mass of ~1000 solar masses and with a factor of ~15x increase in luminosity sensitivity over the existing large-scale single-dish APEX map. With only the ACA and the minimum integration time per pointing, we will produce a map of extragalactic CO with the greatest mass sensitivity and covering ~1.5 pc to 1 kpc scales. Once we have an accurate account of the CO-emitting gas we will be able to measure the CO luminosity function, the dynamical state, how CO brightness relates to environmental properties, and variations in X(CO). Further analysis of	Tile_016_a_06_7M	Federrath, Christoph; Bolatto, Alberto; Staveley-Smith, Lister; Onishi, Toshikazu; Dickey, John; Rubio, Monica; Meixner, Margaret; Hughes, Annie; Johnson, Lent; Krumholz, Mark; Tarantino, Elizabeth; Saldaño, Hugo; McClure-Griffiths, Naomi; Tachihara, Kengo; Kemper, Ciska; Galametz, Maud; Stanimirovic, Snezana; Leroy, Adam; Sandstrom, Karin; Kawamura, Akiko; Indebetouw, Remy; Roman-Duval, Julia;	13.474429068070402	0.5674880228170619	1.8	uid://A001/X133f/X1d1	uid://A001/X133f/X1d2	uid://A002/Xd4f832/X3689	A Large Unbiased and Complete Survey of CO in the Small Magellanic Cloud	S	PHASE WVR	F	31.677007008429293	T	2025ApJS..277...62N	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	kjameson	Jameson, Katherine	61.03515625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.01115.S	ALMA	JAO	ALMA	uid://A001/X133f/X1d2.source.J0103-6439.spw.18	cube	2		J0103-6439	15.89059026673098	-64.65213476670343	0.012200837933907685	Circle ICRS 15.890590 -64.652135 0.006100			4096	1	2	5.696465331123022	58432.140747	58432.184977	483.84	483.84	0.0012740456786102564	0.0012849655206314365	238887.020700014	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133f/X1d2	application/x-votable+xml; content=datalink		2018.1.01115.S	Public	300.8043854174813	-52.426050860288555	6	5.33280635667859E-9	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2019-11-20T20:16:45.000	5.696465331123022	[219.22..219.72GHz,244.14kHz,10mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [220.25..220.37GHz,61.04kHz,13.5mJy/beam@10km/s,3.3mJy/beam@native, XX YY] U [230.38..230.51GHz,61.04kHz,12.3mJy/beam@10km/s,3mJy/beam@native, XX YY] U [233.31..235.31GHz,976.56kHz,10.7mJy/beam@10km/s,671.6uJy/beam@native, XX YY]	234.30762408330995	79.42982247020859	ALMA	Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates	Nakano, Satoya	Nakano, Satoya; Tachihara, Kengo; Tamashiro, Mao	We present identifications and kinematic analysis of 7426 massive (≥8M<SUB>⊙</SUB>) stars in the Small Magellanic Cloud (SMC), using Gaia DR3 data. We used the Gaia (G<SUB>BP</SUB> ‑ G<SUB>RP</SUB>, G) color–magnitude diagram to select the population of massive stars, and parallax to omit foreground objects. The spatial distribution of the 7426 massive star candidates is generally consistent with the spatial distribution of the interstellar medium, such as Hα and H I emission. The identified massive stars show inhomogeneous distributions over the galaxy, showing several superstructures formed by massive stars with a several hundred parsec scale. The stellar superstructures defined by the surface density have opposite mean proper motions in the east and west, moving away from each other. Similarly, the mean line-of-sight velocities of the superstructures are larger to the southeast and smaller to the northwest. The different east–west properties of the superstructures' proper-motion, line-of-sight velocity ind	2025	The Small Magellanic Cloud (SMC) is the only laboratory to study the low metallicity ISM at high spatial resolution, and yet we still do not know where the CO emission exists. We propose to use the ACA in standalone mode to map a 1.0 x 0.5 degree (1 kpc x 500 pc) region of the SW Bar of the SMC in 12CO, 13CO, C18O (2-1) covering a large fraction of the recent star formation, dust, and HI gas. With this new map we will be able to catalog CO clouds and clumps down to a mass of ~1000 solar masses and with a factor of ~15x increase in luminosity sensitivity over the existing large-scale single-dish APEX map. With only the ACA and the minimum integration time per pointing, we will produce a map of extragalactic CO with the greatest mass sensitivity and covering ~1.5 pc to 1 kpc scales. Once we have an accurate account of the CO-emitting gas we will be able to measure the CO luminosity function, the dynamical state, how CO brightness relates to environmental properties, and variations in X(CO). Further analysis of	Tile_016_a_06_7M	Federrath, Christoph; Bolatto, Alberto; Staveley-Smith, Lister; Onishi, Toshikazu; Dickey, John; Rubio, Monica; Meixner, Margaret; Hughes, Annie; Johnson, Lent; Krumholz, Mark; Tarantino, Elizabeth; Saldaño, Hugo; McClure-Griffiths, Naomi; Tachihara, Kengo; Kemper, Ciska; Galametz, Maud; Stanimirovic, Snezana; Leroy, Adam; Sandstrom, Karin; Kawamura, Akiko; Indebetouw, Remy; Roman-Duval, Julia;	10.742858358758616	0.5674880228170619	1.8	uid://A001/X133f/X1d1	uid://A001/X133f/X1d2	uid://A002/Xd4f832/X3689	A Large Unbiased and Complete Survey of CO in the Small Magellanic Cloud	S	PHASE WVR	F	31.677007008429293	T	2025ApJS..277...62N	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	kjameson	Jameson, Katherine	976.5625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.01115.S	ALMA	JAO	ALMA	uid://A001/X133f/X1d2.source.J0103-6439.spw.20	cube	2		J0103-6439	15.89059026673098	-64.65213476670343	0.012200837933907685	Circle ICRS 15.890590 -64.652135 0.006100			4096	1	2	5.696465331123022	58432.140747	58432.184977	483.84	483.84	0.0013644043880858157	0.0013675157844928892	899913.8015278195	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133f/X1d2	application/x-votable+xml; content=datalink		2018.1.01115.S	Public	300.8043854174813	-52.426050860288555	6	1.5194793574489506E-9	5.0E8	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2019-11-20T20:16:45.000	5.696465331123022	[219.22..219.72GHz,244.14kHz,10mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [220.25..220.37GHz,61.04kHz,13.5mJy/beam@10km/s,3.3mJy/beam@native, XX YY] U [230.38..230.51GHz,61.04kHz,12.3mJy/beam@10km/s,3mJy/beam@native, XX YY] U [233.31..235.31GHz,976.56kHz,10.7mJy/beam@10km/s,671.6uJy/beam@native, XX YY]	219.4740899617259	79.42982247020859	ALMA	Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates	Nakano, Satoya	Nakano, Satoya; Tachihara, Kengo; Tamashiro, Mao	We present identifications and kinematic analysis of 7426 massive (≥8M<SUB>⊙</SUB>) stars in the Small Magellanic Cloud (SMC), using Gaia DR3 data. We used the Gaia (G<SUB>BP</SUB> ‑ G<SUB>RP</SUB>, G) color–magnitude diagram to select the population of massive stars, and parallax to omit foreground objects. The spatial distribution of the 7426 massive star candidates is generally consistent with the spatial distribution of the interstellar medium, such as Hα and H I emission. The identified massive stars show inhomogeneous distributions over the galaxy, showing several superstructures formed by massive stars with a several hundred parsec scale. The stellar superstructures defined by the surface density have opposite mean proper motions in the east and west, moving away from each other. Similarly, the mean line-of-sight velocities of the superstructures are larger to the southeast and smaller to the northwest. The different east–west properties of the superstructures' proper-motion, line-of-sight velocity ind	2025	The Small Magellanic Cloud (SMC) is the only laboratory to study the low metallicity ISM at high spatial resolution, and yet we still do not know where the CO emission exists. We propose to use the ACA in standalone mode to map a 1.0 x 0.5 degree (1 kpc x 500 pc) region of the SW Bar of the SMC in 12CO, 13CO, C18O (2-1) covering a large fraction of the recent star formation, dust, and HI gas. With this new map we will be able to catalog CO clouds and clumps down to a mass of ~1000 solar masses and with a factor of ~15x increase in luminosity sensitivity over the existing large-scale single-dish APEX map. With only the ACA and the minimum integration time per pointing, we will produce a map of extragalactic CO with the greatest mass sensitivity and covering ~1.5 pc to 1 kpc scales. Once we have an accurate account of the CO-emitting gas we will be able to measure the CO luminosity function, the dynamical state, how CO brightness relates to environmental properties, and variations in X(CO). Further analysis of	Tile_016_a_06_7M	Federrath, Christoph; Bolatto, Alberto; Staveley-Smith, Lister; Onishi, Toshikazu; Dickey, John; Rubio, Monica; Meixner, Margaret; Hughes, Annie; Johnson, Lent; Krumholz, Mark; Tarantino, Elizabeth; Saldaño, Hugo; McClure-Griffiths, Naomi; Tachihara, Kengo; Kemper, Ciska; Galametz, Maud; Stanimirovic, Snezana; Leroy, Adam; Sandstrom, Karin; Kawamura, Akiko; Indebetouw, Remy; Roman-Duval, Julia;	9.97500913158596	0.5674880228170619	1.8	uid://A001/X133f/X1d1	uid://A001/X133f/X1d2	uid://A002/Xd4f832/X3689	A Large Unbiased and Complete Survey of CO in the Small Magellanic Cloud	S	PHASE WVR	F	31.677007008429293	T	2025ApJS..277...62N	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	kjameson	Jameson, Katherine	244.140625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.1.01115.S	ALMA	JAO	ALMA	uid://A001/X133f/X1d2.source.J0103-6439.spw.16	cube	2		J0103-6439	15.89059026673098	-64.65213476670343	0.012200837933907685	Circle ICRS 15.890590 -64.652135 0.006100			4096	1	2	5.696465331123022	58432.140747	58432.184977	483.84	483.84	0.0013005629156121869	0.0013012684499667834	3774306.031118751	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X133f/X1d2	application/x-votable+xml; content=datalink		2018.1.01115.S	Public	300.8043854174813	-52.426050860288555	6	3.4455426037766644E-10	1.25E8	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N603:CM09 N604:CM11 N605:CM04 N606:CM06	F	2019-11-20T20:16:45.000	5.696465331123022	[219.22..219.72GHz,244.14kHz,10mJy/beam@10km/s,1.2mJy/beam@native, XX YY] U [220.25..220.37GHz,61.04kHz,13.5mJy/beam@10km/s,3.3mJy/beam@native, XX YY] U [230.38..230.51GHz,61.04kHz,12.3mJy/beam@10km/s,3mJy/beam@native, XX YY] U [233.31..235.31GHz,976.56kHz,10.7mJy/beam@10km/s,671.6uJy/beam@native, XX YY]	230.44727956664784	79.42982247020859	ALMA	Evidence of Galactic Interaction in the Small Magellanic Cloud Probed by Gaia-selected Massive Star Candidates	Nakano, Satoya	Nakano, Satoya; Tachihara, Kengo; Tamashiro, Mao	We present identifications and kinematic analysis of 7426 massive (≥8M<SUB>⊙</SUB>) stars in the Small Magellanic Cloud (SMC), using Gaia DR3 data. We used the Gaia (G<SUB>BP</SUB> ‑ G<SUB>RP</SUB>, G) color–magnitude diagram to select the population of massive stars, and parallax to omit foreground objects. The spatial distribution of the 7426 massive star candidates is generally consistent with the spatial distribution of the interstellar medium, such as Hα and H I emission. The identified massive stars show inhomogeneous distributions over the galaxy, showing several superstructures formed by massive stars with a several hundred parsec scale. The stellar superstructures defined by the surface density have opposite mean proper motions in the east and west, moving away from each other. Similarly, the mean line-of-sight velocities of the superstructures are larger to the southeast and smaller to the northwest. The different east–west properties of the superstructures' proper-motion, line-of-sight velocity ind	2025	The Small Magellanic Cloud (SMC) is the only laboratory to study the low metallicity ISM at high spatial resolution, and yet we still do not know where the CO emission exists. We propose to use the ACA in standalone mode to map a 1.0 x 0.5 degree (1 kpc x 500 pc) region of the SW Bar of the SMC in 12CO, 13CO, C18O (2-1) covering a large fraction of the recent star formation, dust, and HI gas. With this new map we will be able to catalog CO clouds and clumps down to a mass of ~1000 solar masses and with a factor of ~15x increase in luminosity sensitivity over the existing large-scale single-dish APEX map. With only the ACA and the minimum integration time per pointing, we will produce a map of extragalactic CO with the greatest mass sensitivity and covering ~1.5 pc to 1 kpc scales. Once we have an accurate account of the CO-emitting gas we will be able to measure the CO luminosity function, the dynamical state, how CO brightness relates to environmental properties, and variations in X(CO). Further analysis of	Tile_016_a_06_7M	Federrath, Christoph; Bolatto, Alberto; Staveley-Smith, Lister; Onishi, Toshikazu; Dickey, John; Rubio, Monica; Meixner, Margaret; Hughes, Annie; Johnson, Lent; Krumholz, Mark; Tarantino, Elizabeth; Saldaño, Hugo; McClure-Griffiths, Naomi; Tachihara, Kengo; Kemper, Ciska; Galametz, Maud; Stanimirovic, Snezana; Leroy, Adam; Sandstrom, Karin; Kawamura, Akiko; Indebetouw, Remy; Roman-Duval, Julia;	12.28277036262747	0.5674880228170619	1.8	uid://A001/X133f/X1d1	uid://A001/X133f/X1d2	uid://A002/Xd4f832/X3689	A Large Unbiased and Complete Survey of CO in the Small Magellanic Cloud	S	PHASE WVR	F	31.677007008429293	T	2025ApJS..277...62N	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	kjameson	Jameson, Katherine	61.03515625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01074.S	ALMA	JAO	ALMA	uid://A001/X3788/X9c55.source.J0519-4546.spw.18	image	2		J0519-4546	79.95717984574434	-45.77884811113823	0.04027822636329081	Circle ICRS 79.957180 -45.778848 0.020139			128	1	2	0.14069674288162412	60915.327302	60915.330802	302.4	302.4	0.007110773297123494	0.007461999348558009	1285.5939999983998	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3788/X9c55	application/x-votable+xml; content=datalink		2024.1.01074.S	Proprietary	251.5967349391583	-34.63430443340226	1	5.530970707291693E-6	2.0E9	A091:DA59 A094:DV07 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A108:DV24 A110:DA51 A111:DV19 A116:DA57 A118:DV13 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A124:DV01 A125:DV02 A127:DA65 A128:DA60 A129:DA42 A132:DV25 A135:DV15 P401:DA52 P404:DA41 P408:DV08 P409:DA48 P411:DA56 P412:DV14 S301:DV21 S303:DV22 S305:DV04 S306:DA58 S308:DA50 S309:DV09 W201:DA46 W202:DA64 W204:DA54 W207:DA61 W208:DA43 W209:DV05 W210:DV23	F	2026-09-02T23:10:01.000	0.14069674288162412	[36.22..38.20GHz,31250.00kHz,1.6mJy/beam@10km/s,39.9uJy/beam@native, XX YY] U [38.16..40.14GHz,31250.00kHz,1.6mJy/beam@10km/s,41.4uJy/beam@native, XX YY] U [40.18..42.16GHz,31250.00kHz,1.7mJy/beam@10km/s,45.1uJy/beam@native, XX YY] U [42.11..44.10GHz,31250.00kHz,1.8mJy/beam@10km/s,49.5uJy/beam@native, XX YY]	41.168103148438	222464.9694198371	ALMA						We propose to catalog every ultra-compact HII regions in the LMC with Band 1 observations of the Spitzer Massive Young Stellar Object catalog reaching 0.03-0.1 pc scales that match UCHII sizes in the Milky Way (0.13-0.4\arcsec at d=50 kpc). With ALMA's new Band 1 capabilities, we can efficiently detect these HII regions from their free-free emission while a single pointing covers a typical molecular cloud diameter (30 pc). By pin-pointing the current location of every recently formed >18 Msol star capable of producing a UCHII region, we will resolve three open questions: -What are the Spitzer catalog sources: are they single/few MYSOs or low-mass stellar clusters? -Do "gold-standard" Galactic and extragalactic star formation rates agree on scales of individual MYSOs? -In which environments have massive stars recently formed in the LMC? This proposal will provide a contaminant-free, complete sample of the most recently formed >18 Msol stars across the LMC with broad implications for interpreting massive star f	YSO_Clus_h_01_TM1	Zhang, Qizhou; Indebetouw, Remy; Rosolowsky, Erik;	1.719536317529788	0.02176473665828118	0.51955664	uid://A001/X3788/X9c54	uid://A001/X3788/X9c55	uid://A002/X12de9a8/X432b	ALMA reveals the ultra-compact UCHII region population from Spitzer MYSOs in the LMC	S	BANDPASS FLUX WVR	F	2.404305554679706	T		Magellanic Clouds;null	Local Universe	ekoch	Koch, Eric	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01074.S	ALMA	JAO	ALMA	uid://A001/X3788/X9c55.source.J0519-4546.spw.7	image	2		J0519-4546	79.95717984574434	-45.77884811113823	0.04027822636329081	Circle ICRS 79.957180 -45.778848 0.020139			128	1	2	0.14069674288162412	60915.327302	60915.330802	302.4	302.4	0.007468715181667076	0.007857157030505005	1220.9379999983998	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3788/X9c55	application/x-votable+xml; content=datalink		2024.1.01074.S	Proprietary	251.5967349391583	-34.63430443340226	1	6.117030552357464E-6	2.0E9	A091:DA59 A094:DV07 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A108:DV24 A110:DA51 A111:DV19 A116:DA57 A118:DV13 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A124:DV01 A125:DV02 A127:DA65 A128:DA60 A129:DA42 A132:DV25 A135:DV15 P401:DA52 P404:DA41 P408:DV08 P409:DA48 P411:DA56 P412:DV14 S301:DV21 S303:DV22 S305:DV04 S306:DA58 S308:DA50 S309:DV09 W201:DA46 W202:DA64 W204:DA54 W207:DA61 W208:DA43 W209:DV05 W210:DV23	F	2026-09-02T23:10:01.000	0.14069674288162412	[36.22..38.20GHz,31250.00kHz,1.6mJy/beam@10km/s,39.9uJy/beam@native, XX YY] U [38.16..40.14GHz,31250.00kHz,1.6mJy/beam@10km/s,41.4uJy/beam@native, XX YY] U [40.18..42.16GHz,31250.00kHz,1.7mJy/beam@10km/s,45.1uJy/beam@native, XX YY] U [42.11..44.10GHz,31250.00kHz,1.8mJy/beam@10km/s,49.5uJy/beam@native, XX YY]	39.14754900527673	222464.9694198371	ALMA						We propose to catalog every ultra-compact HII regions in the LMC with Band 1 observations of the Spitzer Massive Young Stellar Object catalog reaching 0.03-0.1 pc scales that match UCHII sizes in the Milky Way (0.13-0.4\arcsec at d=50 kpc). With ALMA's new Band 1 capabilities, we can efficiently detect these HII regions from their free-free emission while a single pointing covers a typical molecular cloud diameter (30 pc). By pin-pointing the current location of every recently formed >18 Msol star capable of producing a UCHII region, we will resolve three open questions: -What are the Spitzer catalog sources: are they single/few MYSOs or low-mass stellar clusters? -Do "gold-standard" Galactic and extragalactic star formation rates agree on scales of individual MYSOs? -In which environments have massive stars recently formed in the LMC? This proposal will provide a contaminant-free, complete sample of the most recently formed >18 Msol stars across the LMC with broad implications for interpreting massive star f	YSO_Clus_h_01_TM1	Zhang, Qizhou; Indebetouw, Remy; Rosolowsky, Erik;	1.6201055939048798	0.02176473665828118	0.51955664	uid://A001/X3788/X9c54	uid://A001/X3788/X9c55	uid://A002/X12de9a8/X432b	ALMA reveals the ultra-compact UCHII region population from Spitzer MYSOs in the LMC	S	BANDPASS FLUX WVR	F	2.404305554679706	T		Magellanic Clouds;null	Local Universe	ekoch	Koch, Eric	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01074.S	ALMA	JAO	ALMA	uid://A001/X3788/X9c55.source.J0519-4546.spw.11	image	2		J0519-4546	79.95717984574434	-45.77884811113823	0.04027822636329081	Circle ICRS 79.957180 -45.778848 0.020139			128	1	2	0.14069674288162412	60915.327302	60915.330802	302.4	302.4	0.006798343406257149	0.007118688262569836	1347.5939999983998	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3788/X9c55	application/x-votable+xml; content=datalink		2024.1.01074.S	Proprietary	251.5967349391583	-34.63430443340226	1	5.044665705349586E-6	2.0E9	A091:DA59 A094:DV07 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A108:DV24 A110:DA51 A111:DV19 A116:DA57 A118:DV13 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A124:DV01 A125:DV02 A127:DA65 A128:DA60 A129:DA42 A132:DV25 A135:DV15 P401:DA52 P404:DA41 P408:DV08 P409:DA48 P411:DA56 P412:DV14 S301:DV21 S303:DV22 S305:DV04 S306:DA58 S308:DA50 S309:DV09 W201:DA46 W202:DA64 W204:DA54 W207:DA61 W208:DA43 W209:DV05 W210:DV23	F	2026-09-02T23:10:01.000	0.14069674288162412	[36.22..38.20GHz,31250.00kHz,1.6mJy/beam@10km/s,39.9uJy/beam@native, XX YY] U [38.16..40.14GHz,31250.00kHz,1.6mJy/beam@10km/s,41.4uJy/beam@native, XX YY] U [40.18..42.16GHz,31250.00kHz,1.7mJy/beam@10km/s,45.1uJy/beam@native, XX YY] U [42.11..44.10GHz,31250.00kHz,1.8mJy/beam@10km/s,49.5uJy/beam@native, XX YY]	43.105655067455544	222464.9694198371	ALMA						We propose to catalog every ultra-compact HII regions in the LMC with Band 1 observations of the Spitzer Massive Young Stellar Object catalog reaching 0.03-0.1 pc scales that match UCHII sizes in the Milky Way (0.13-0.4\arcsec at d=50 kpc). With ALMA's new Band 1 capabilities, we can efficiently detect these HII regions from their free-free emission while a single pointing covers a typical molecular cloud diameter (30 pc). By pin-pointing the current location of every recently formed >18 Msol star capable of producing a UCHII region, we will resolve three open questions: -What are the Spitzer catalog sources: are they single/few MYSOs or low-mass stellar clusters? -Do "gold-standard" Galactic and extragalactic star formation rates agree on scales of individual MYSOs? -In which environments have massive stars recently formed in the LMC? This proposal will provide a contaminant-free, complete sample of the most recently formed >18 Msol stars across the LMC with broad implications for interpreting massive star f	YSO_Clus_h_01_TM1	Zhang, Qizhou; Indebetouw, Remy; Rosolowsky, Erik;	1.8459886347676528	0.02176473665828118	0.51955664	uid://A001/X3788/X9c54	uid://A001/X3788/X9c55	uid://A002/X12de9a8/X432b	ALMA reveals the ultra-compact UCHII region population from Spitzer MYSOs in the LMC	S	BANDPASS FLUX WVR	F	2.404305554679706	T		Magellanic Clouds;null	Local Universe	ekoch	Koch, Eric	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2024.1.01074.S	ALMA	JAO	ALMA	uid://A001/X3788/X9c55.source.J0519-4546.spw.15	image	2		J0519-4546	79.95717984574434	-45.77884811113823	0.04027822636329081	Circle ICRS 79.957180 -45.778848 0.020139			128	1	2	0.14069674288162412	60915.327302	60915.330802	302.4	302.4	0.007847515858072722	0.008277493352113217	1158.9379999984	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3788/X9c55	application/x-votable+xml; content=datalink		2024.1.01074.S	Proprietary	251.5967349391583	-34.63430443340226	1	6.771117673701619E-6	2.0E9	A091:DA59 A094:DV07 A096:DA45 A101:DA55 A104:DV16 A105:DV06 A108:DV24 A110:DA51 A111:DV19 A116:DA57 A118:DV13 A120:DV17 A121:DA44 A122:DA63 A123:DV11 A124:DV01 A125:DV02 A127:DA65 A128:DA60 A129:DA42 A132:DV25 A135:DV15 P401:DA52 P404:DA41 P408:DV08 P409:DA48 P411:DA56 P412:DV14 S301:DV21 S303:DV22 S305:DV04 S306:DA58 S308:DA50 S309:DV09 W201:DA46 W202:DA64 W204:DA54 W207:DA61 W208:DA43 W209:DV05 W210:DV23	F	2026-09-02T23:10:01.000	0.14069674288162412	[36.22..38.20GHz,31250.00kHz,1.6mJy/beam@10km/s,39.9uJy/beam@native, XX YY] U [38.16..40.14GHz,31250.00kHz,1.6mJy/beam@10km/s,41.4uJy/beam@native, XX YY] U [40.18..42.16GHz,31250.00kHz,1.7mJy/beam@10km/s,45.1uJy/beam@native, XX YY] U [42.11..44.10GHz,31250.00kHz,1.8mJy/beam@10km/s,49.5uJy/beam@native, XX YY]	37.20999708625918	222464.9694198371	ALMA						We propose to catalog every ultra-compact HII regions in the LMC with Band 1 observations of the Spitzer Massive Young Stellar Object catalog reaching 0.03-0.1 pc scales that match UCHII sizes in the Milky Way (0.13-0.4\arcsec at d=50 kpc). With ALMA's new Band 1 capabilities, we can efficiently detect these HII regions from their free-free emission while a single pointing covers a typical molecular cloud diameter (30 pc). By pin-pointing the current location of every recently formed >18 Msol star capable of producing a UCHII region, we will resolve three open questions: -What are the Spitzer catalog sources: are they single/few MYSOs or low-mass stellar clusters? -Do "gold-standard" Galactic and extragalactic star formation rates agree on scales of individual MYSOs? -In which environments have massive stars recently formed in the LMC? This proposal will provide a contaminant-free, complete sample of the most recently formed >18 Msol stars across the LMC with broad implications for interpreting massive star f	YSO_Clus_h_01_TM1	Zhang, Qizhou; Indebetouw, Remy; Rosolowsky, Erik;	1.6034320950143004	0.02176473665828118	0.51955664	uid://A001/X3788/X9c54	uid://A001/X3788/X9c55	uid://A002/X12de9a8/X432b	ALMA reveals the ultra-compact UCHII region population from Spitzer MYSOs in the LMC	S	BANDPASS FLUX WVR	F	2.404305554679706	T		Magellanic Clouds;null	Local Universe	ekoch	Koch, Eric	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.2.00060.S	ALMA	JAO	ALMA	uid://A001/X124a/X16e.source.J0006-0623.spw.18	image	2		J0006-0623	1.557887500002359	-6.393148611112185	0.00807308435525197	Polygon ICRS 1.558397 -6.389144 1.559844 -6.389611 1.561017 -6.390576 1.561750 -6.391901 1.561941 -6.392895 1.561917 -6.393655 1.561447 -6.395093 1.561017 -6.395722 1.560275 -6.396414 1.558898 -6.397058 1.557378 -6.397153 1.555931 -6.396686 1.554758 -6.395722 1.554024 -6.394396 1.553858 -6.393655 1.553858 -6.392643 1.554025 -6.391901 1.554458 -6.390986 1.555500 -6.389883 1.556877 -6.389239			128	1	2	3.430895017190135	57953.309379	57959.427561	12216.96	12216.96	8.833055786674135E-4	8.885050785981449E-4	10861.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X124a/X16e	application/x-votable+xml; content=datalink		2016.2.00060.S	Public	93.50553584430446	-66.64651638773849	7	8.180883470975174E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N605:CM04 N606:CM06	F	2018-08-10T16:05:42.000	3.430895017190135	[335.47..337.46GHz,31250.00kHz,9.6mJy/beam@10km/s,716.5uJy/beam@native, XX YY] U [337.41..339.40GHz,31250.00kHz,8.6mJy/beam@10km/s,644.7uJy/beam@native, XX YY] U [347.47..349.46GHz,31250.00kHz,9.1mJy/beam@10km/s,691.2uJy/beam@native, XX YY] U [349.47..351.46GHz,31250.00kHz,10.3mJy/beam@10km/s,790.4uJy/beam@native, XX YY]	338.4052788185517	26805.294176996144	ALMA	ALMA High-Level Data Products: submillimetre counterparts of SDSS quasars in the ALMA footprint Evidence of Gas Depletion in Quasars with Moderate Radio Emission On the multiplicity of ALMA Compact Array counterparts of far-infrared bright quasars	Hatziminaoglou, E. Wen, Yuhan Wong, A.	Hatziminaoglou, E.; Farrah, D.; Humphreys, E.; Manrique, A.; Pérez-Fournon, I.; Pitchford, L. K.; Salvador-Solé, E.; Wang, L. Wen, Yuhan; Wang, Ran; Ho, Luis C.; Shangguan, Jinyi; Treister, Ezequiel; Li, Guodong; Bauer, Franz E. Wong, A.; Hatziminaoglou, E.; Borkar, A.; Popping, G.; Pérez-Fournon, I.; Poidevin, F.; Stoehr, F.; Messias, H.	The Atacama Large Millimetre/submillimetre Array (ALMA) is the world's most advanced radio interferometric facility, producing science data with an average rate of about 1 TB per day. After a process of calibration, imaging and quality assurance, the scientific data are stored in the ALMA Science Archive (ASA), along with the corresponding raw data, making the ASA an invaluable resource for original astronomical research. Due to their complexity, each ALMA data set has the potential for scientific results that go well beyond the ideas behind the original proposal that led to each observation. For this reason, the European ALMA Regional Centre initiated the High-Level Data Products initiative to develop science-oriented data products derived from data sets publicly available in the ASA, that go beyond the formal ALMA deliverables. The first instance of this initiative is the creation of a catalogue of submillimetre (submm) detections of Sloan Digital Sky Survey (SDSS) quasars from the SDSS Data Release 14 that	2018	We propose band 7 continuum ACA stand-alone observations of the most infrared-luminous type 1 quasar hosts in the Herschel HerS and HeLMS fields. The proposed observations will establish whether the Herschel-SPIRE fluxes come from a single component alone, placing the hosts of these type 1 quasars among the most extreme star formers in the Universe with SED-derived star formation rates (SFRs) above 1000 solar masses per year, that will immediately chanllenge the models for galaxy assembly. If not, we will resolve the SPIRE fluxes into multiple components, allowing for revised SFRs. Such multiplicity could either be the result of unrelated sources lying closely to one another in projection but far apart in redshift, or real oversensities, in which case we will have immediately identified a sample of high-redshift overdense region candidates around type 1 quasars, hosting multiple starbursts, that will be ideal targets for follow up observations.	SDSS_J00_a_07_7M	Wang, Lingyu; Pitchford, Lura; Farrah, Duncan;	8.581196343274469	0.35249884010890475	0.91	uid://A001/X124a/X16d	uid://A001/X124a/X16e	uid://A002/Xc23361/X9546	How extreme are the extreme star-forming hosts of optically-bright quasars at 2 < z < 4?	S	BANDPASS PHASE WVR	F	22.938436734069292	T	2018MNRAS.480.4974H 2023MNRAS.523...23W 2026ApJ...998..323W	Starbursts, star formation;Active Galactic Nuclei (AGN)/Quasars (QSO)	Active galaxies	ehatzimi	Hatziminaoglou, Evanthia	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.2.00060.S	ALMA	JAO	ALMA	uid://A001/X124a/X16e.source.J0006-0623.spw.16	image	2		J0006-0623	1.557887500002359	-6.393148611112185	0.00807308435525197	Polygon ICRS 1.558397 -6.389144 1.559844 -6.389611 1.561017 -6.390576 1.561750 -6.391901 1.561941 -6.392895 1.561917 -6.393655 1.561447 -6.395093 1.561017 -6.395722 1.560275 -6.396414 1.558898 -6.397058 1.557378 -6.397153 1.555931 -6.396686 1.554758 -6.395722 1.554024 -6.394396 1.553858 -6.393655 1.553858 -6.392643 1.554025 -6.391901 1.554458 -6.390986 1.555500 -6.389883 1.556877 -6.389239			128	1	2	3.430895017190135	57953.309379	57959.427561	12216.96	12216.96	8.883766058863497E-4	8.936361258094972E-4	10799.5764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X124a/X16e	application/x-votable+xml; content=datalink		2016.2.00060.S	Public	93.50553584430446	-66.64651638773849	7	8.275364831143327E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N605:CM04 N606:CM06	F	2018-08-10T16:05:42.000	3.430895017190135	[335.47..337.46GHz,31250.00kHz,9.6mJy/beam@10km/s,716.5uJy/beam@native, XX YY] U [337.41..339.40GHz,31250.00kHz,8.6mJy/beam@10km/s,644.7uJy/beam@native, XX YY] U [347.47..349.46GHz,31250.00kHz,9.1mJy/beam@10km/s,691.2uJy/beam@native, XX YY] U [349.47..351.46GHz,31250.00kHz,10.3mJy/beam@10km/s,790.4uJy/beam@native, XX YY]	336.46793224100884	26805.294176996144	ALMA	ALMA High-Level Data Products: submillimetre counterparts of SDSS quasars in the ALMA footprint Evidence of Gas Depletion in Quasars with Moderate Radio Emission On the multiplicity of ALMA Compact Array counterparts of far-infrared bright quasars	Hatziminaoglou, E. Wen, Yuhan Wong, A.	Hatziminaoglou, E.; Farrah, D.; Humphreys, E.; Manrique, A.; Pérez-Fournon, I.; Pitchford, L. K.; Salvador-Solé, E.; Wang, L. Wen, Yuhan; Wang, Ran; Ho, Luis C.; Shangguan, Jinyi; Treister, Ezequiel; Li, Guodong; Bauer, Franz E. Wong, A.; Hatziminaoglou, E.; Borkar, A.; Popping, G.; Pérez-Fournon, I.; Poidevin, F.; Stoehr, F.; Messias, H.	The Atacama Large Millimetre/submillimetre Array (ALMA) is the world's most advanced radio interferometric facility, producing science data with an average rate of about 1 TB per day. After a process of calibration, imaging and quality assurance, the scientific data are stored in the ALMA Science Archive (ASA), along with the corresponding raw data, making the ASA an invaluable resource for original astronomical research. Due to their complexity, each ALMA data set has the potential for scientific results that go well beyond the ideas behind the original proposal that led to each observation. For this reason, the European ALMA Regional Centre initiated the High-Level Data Products initiative to develop science-oriented data products derived from data sets publicly available in the ASA, that go beyond the formal ALMA deliverables. The first instance of this initiative is the creation of a catalogue of submillimetre (submm) detections of Sloan Digital Sky Survey (SDSS) quasars from the SDSS Data Release 14 that	2018	We propose band 7 continuum ACA stand-alone observations of the most infrared-luminous type 1 quasar hosts in the Herschel HerS and HeLMS fields. The proposed observations will establish whether the Herschel-SPIRE fluxes come from a single component alone, placing the hosts of these type 1 quasars among the most extreme star formers in the Universe with SED-derived star formation rates (SFRs) above 1000 solar masses per year, that will immediately chanllenge the models for galaxy assembly. If not, we will resolve the SPIRE fluxes into multiple components, allowing for revised SFRs. Such multiplicity could either be the result of unrelated sources lying closely to one another in projection but far apart in redshift, or real oversensities, in which case we will have immediately identified a sample of high-redshift overdense region candidates around type 1 quasars, hosting multiple starbursts, that will be ideal targets for follow up observations.	SDSS_J00_a_07_7M	Wang, Lingyu; Pitchford, Lura; Farrah, Duncan;	9.564480132743263	0.35249884010890475	0.91	uid://A001/X124a/X16d	uid://A001/X124a/X16e	uid://A002/Xc23361/X9546	How extreme are the extreme star-forming hosts of optically-bright quasars at 2 < z < 4?	S	BANDPASS PHASE WVR	F	22.938436734069292	T	2018MNRAS.480.4974H 2023MNRAS.523...23W 2026ApJ...998..323W	Starbursts, star formation;Active Galactic Nuclei (AGN)/Quasars (QSO)	Active galaxies	ehatzimi	Hatziminaoglou, Evanthia	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.2.00060.S	ALMA	JAO	ALMA	uid://A001/X124a/X16e.source.J0006-0623.spw.20	image	2		J0006-0623	1.557887500002359	-6.393148611112185	0.00807308435525197	Polygon ICRS 1.558397 -6.389144 1.559844 -6.389611 1.561017 -6.390576 1.561750 -6.391901 1.561941 -6.392895 1.561917 -6.393655 1.561447 -6.395093 1.561017 -6.395722 1.560275 -6.396414 1.558898 -6.397058 1.557378 -6.397153 1.555931 -6.396686 1.554758 -6.395722 1.554024 -6.394396 1.553858 -6.393655 1.553858 -6.392643 1.554025 -6.391901 1.554458 -6.390986 1.555500 -6.389883 1.556877 -6.389239			128	1	2	3.430895017190135	57953.309379	57959.427561	12216.96	12216.96	8.578732494948864E-4	8.6277696082113E-4	11120.0764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X124a/X16e	application/x-votable+xml; content=datalink		2016.2.00060.S	Public	93.50553584430446	-66.64651638773849	7	7.715267421030164E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N605:CM04 N606:CM06	F	2018-08-10T16:05:42.000	3.430895017190135	[335.47..337.46GHz,31250.00kHz,9.6mJy/beam@10km/s,716.5uJy/beam@native, XX YY] U [337.41..339.40GHz,31250.00kHz,8.6mJy/beam@10km/s,644.7uJy/beam@native, XX YY] U [347.47..349.46GHz,31250.00kHz,9.1mJy/beam@10km/s,691.2uJy/beam@native, XX YY] U [349.47..351.46GHz,31250.00kHz,10.3mJy/beam@10km/s,790.4uJy/beam@native, XX YY]	348.46698201159666	26805.294176996144	ALMA	ALMA High-Level Data Products: submillimetre counterparts of SDSS quasars in the ALMA footprint Evidence of Gas Depletion in Quasars with Moderate Radio Emission On the multiplicity of ALMA Compact Array counterparts of far-infrared bright quasars	Hatziminaoglou, E. Wen, Yuhan Wong, A.	Hatziminaoglou, E.; Farrah, D.; Humphreys, E.; Manrique, A.; Pérez-Fournon, I.; Pitchford, L. K.; Salvador-Solé, E.; Wang, L. Wen, Yuhan; Wang, Ran; Ho, Luis C.; Shangguan, Jinyi; Treister, Ezequiel; Li, Guodong; Bauer, Franz E. Wong, A.; Hatziminaoglou, E.; Borkar, A.; Popping, G.; Pérez-Fournon, I.; Poidevin, F.; Stoehr, F.; Messias, H.	The Atacama Large Millimetre/submillimetre Array (ALMA) is the world's most advanced radio interferometric facility, producing science data with an average rate of about 1 TB per day. After a process of calibration, imaging and quality assurance, the scientific data are stored in the ALMA Science Archive (ASA), along with the corresponding raw data, making the ASA an invaluable resource for original astronomical research. Due to their complexity, each ALMA data set has the potential for scientific results that go well beyond the ideas behind the original proposal that led to each observation. For this reason, the European ALMA Regional Centre initiated the High-Level Data Products initiative to develop science-oriented data products derived from data sets publicly available in the ASA, that go beyond the formal ALMA deliverables. The first instance of this initiative is the creation of a catalogue of submillimetre (submm) detections of Sloan Digital Sky Survey (SDSS) quasars from the SDSS Data Release 14 that	2018	We propose band 7 continuum ACA stand-alone observations of the most infrared-luminous type 1 quasar hosts in the Herschel HerS and HeLMS fields. The proposed observations will establish whether the Herschel-SPIRE fluxes come from a single component alone, placing the hosts of these type 1 quasars among the most extreme star formers in the Universe with SED-derived star formation rates (SFRs) above 1000 solar masses per year, that will immediately chanllenge the models for galaxy assembly. If not, we will resolve the SPIRE fluxes into multiple components, allowing for revised SFRs. Such multiplicity could either be the result of unrelated sources lying closely to one another in projection but far apart in redshift, or real oversensities, in which case we will have immediately identified a sample of high-redshift overdense region candidates around type 1 quasars, hosting multiple starbursts, that will be ideal targets for follow up observations.	SDSS_J00_a_07_7M	Wang, Lingyu; Pitchford, Lura; Farrah, Duncan;	9.066661533223273	0.35249884010890475	0.91	uid://A001/X124a/X16d	uid://A001/X124a/X16e	uid://A002/Xc23361/X9546	How extreme are the extreme star-forming hosts of optically-bright quasars at 2 < z < 4?	S	BANDPASS PHASE WVR	F	22.938436734069292	T	2018MNRAS.480.4974H 2023MNRAS.523...23W 2026ApJ...998..323W	Starbursts, star formation;Active Galactic Nuclei (AGN)/Quasars (QSO)	Active galaxies	ehatzimi	Hatziminaoglou, Evanthia	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.2.00060.S	ALMA	JAO	ALMA	uid://A001/X124a/X16e.source.J0006-0623.spw.22	image	2		J0006-0623	1.557887500002359	-6.393148611112185	0.00807308435525197	Polygon ICRS 1.558397 -6.389144 1.559844 -6.389611 1.561017 -6.390576 1.561750 -6.391901 1.561941 -6.392895 1.561917 -6.393655 1.561447 -6.395093 1.561017 -6.395722 1.560275 -6.396414 1.558898 -6.397058 1.557378 -6.397153 1.555931 -6.396686 1.554758 -6.395722 1.554024 -6.394396 1.553858 -6.393655 1.553858 -6.392643 1.554025 -6.391901 1.554458 -6.390986 1.555500 -6.389883 1.556877 -6.389239			128	1	2	3.430895017190135	57953.309379	57959.427561	12216.96	12216.96	8.529918522929367E-4	8.57839787332888E-4	11184.0764	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X124a/X16e	application/x-votable+xml; content=datalink		2016.2.00060.S	Public	93.50553584430446	-66.64651638773849	7	7.627467870285565E-8	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N605:CM04 N606:CM06	F	2018-08-10T16:05:42.000	3.430895017190135	[335.47..337.46GHz,31250.00kHz,9.6mJy/beam@10km/s,716.5uJy/beam@native, XX YY] U [337.41..339.40GHz,31250.00kHz,8.6mJy/beam@10km/s,644.7uJy/beam@native, XX YY] U [347.47..349.46GHz,31250.00kHz,9.1mJy/beam@10km/s,691.2uJy/beam@native, XX YY] U [349.47..351.46GHz,31250.00kHz,10.3mJy/beam@10km/s,790.4uJy/beam@native, XX YY]	350.466823640028	26805.294176996144	ALMA	ALMA High-Level Data Products: submillimetre counterparts of SDSS quasars in the ALMA footprint Evidence of Gas Depletion in Quasars with Moderate Radio Emission On the multiplicity of ALMA Compact Array counterparts of far-infrared bright quasars	Hatziminaoglou, E. Wen, Yuhan Wong, A.	Hatziminaoglou, E.; Farrah, D.; Humphreys, E.; Manrique, A.; Pérez-Fournon, I.; Pitchford, L. K.; Salvador-Solé, E.; Wang, L. Wen, Yuhan; Wang, Ran; Ho, Luis C.; Shangguan, Jinyi; Treister, Ezequiel; Li, Guodong; Bauer, Franz E. Wong, A.; Hatziminaoglou, E.; Borkar, A.; Popping, G.; Pérez-Fournon, I.; Poidevin, F.; Stoehr, F.; Messias, H.	The Atacama Large Millimetre/submillimetre Array (ALMA) is the world's most advanced radio interferometric facility, producing science data with an average rate of about 1 TB per day. After a process of calibration, imaging and quality assurance, the scientific data are stored in the ALMA Science Archive (ASA), along with the corresponding raw data, making the ASA an invaluable resource for original astronomical research. Due to their complexity, each ALMA data set has the potential for scientific results that go well beyond the ideas behind the original proposal that led to each observation. For this reason, the European ALMA Regional Centre initiated the High-Level Data Products initiative to develop science-oriented data products derived from data sets publicly available in the ASA, that go beyond the formal ALMA deliverables. The first instance of this initiative is the creation of a catalogue of submillimetre (submm) detections of Sloan Digital Sky Survey (SDSS) quasars from the SDSS Data Release 14 that	2018	We propose band 7 continuum ACA stand-alone observations of the most infrared-luminous type 1 quasar hosts in the Herschel HerS and HeLMS fields. The proposed observations will establish whether the Herschel-SPIRE fluxes come from a single component alone, placing the hosts of these type 1 quasars among the most extreme star formers in the Universe with SED-derived star formation rates (SFRs) above 1000 solar masses per year, that will immediately chanllenge the models for galaxy assembly. If not, we will resolve the SPIRE fluxes into multiple components, allowing for revised SFRs. Such multiplicity could either be the result of unrelated sources lying closely to one another in projection but far apart in redshift, or real oversensities, in which case we will have immediately identified a sample of high-redshift overdense region candidates around type 1 quasars, hosting multiple starbursts, that will be ideal targets for follow up observations.	SDSS_J00_a_07_7M	Wang, Lingyu; Pitchford, Lura; Farrah, Duncan;	10.338199487742301	0.35249884010890475	0.91	uid://A001/X124a/X16d	uid://A001/X124a/X16e	uid://A002/Xc23361/X9546	How extreme are the extreme star-forming hosts of optically-bright quasars at 2 < z < 4?	S	BANDPASS PHASE WVR	F	22.938436734069292	T	2018MNRAS.480.4974H 2023MNRAS.523...23W 2026ApJ...998..323W	Starbursts, star formation;Active Galactic Nuclei (AGN)/Quasars (QSO)	Active galaxies	ehatzimi	Hatziminaoglou, Evanthia	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.01676.S	ALMA	JAO	ALMA	uid://A001/X1590/X111.source.J0348-2749.spw.17	image	2		J0348-2749	57.15893572085781	-27.820434911128164	0.006892789436223833	Circle ICRS 57.158936 -27.820435 0.003446			128	1	2	0.4882968686370478	59584.195292	59584.209564	120.96	120.96	0.0013206458386503756	0.0013322935551673438	7263.281230263771	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X111	application/x-votable+xml; content=datalink		2021.1.01676.S	Public	224.52662474860176	-50.90930929109048	6	1.8340687579652053E-7	2.0E9	A001:DA57 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A015:DV21 A016:DA46 A022:DV02 A024:DV06 A025:DV19 A027:DV03 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A040:DA50 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A070:DA51 A072:DA53 A073:DA41 A074:DV09 A075:DA59 A076:DA48 A082:DV22 A083:DV18 A085:DA56 A086:DV17 A087:DV23 A088:DV11 A089:DA52 A090:DV16 A091:DA61 A092:DV13 A093:DV05 A094:DV14	F	2023-01-10T17:52:29.000	0.4882968686370478	[225.02..227.00GHz,31250.00kHz,1.8mJy/beam@10km/s,112.6uJy/beam@native, XX YY] U [226.52..228.50GHz,31250.00kHz,1.7mJy/beam@10km/s,103.9uJy/beam@native, XX YY] U [240.88..242.75GHz,1128.91kHz,1.8mJy/beam@10km/s,117.2uJy/beam@native, XX YY] U [242.43..244.31GHz,1128.91kHz,1.8mJy/beam@10km/s,117.3uJy/beam@native, XX YY]	226.01212658128856	1396.1705167728144	ALMA						Observations of redshifted CO in distant sub-mm selected galaxies (SMGs) probe the physical conditions in which new stars form. When CO is collisionally de-excited from the Jth to the J-1th rotational energy level, the result is a photon whose frequency is J*115GHz. The ground-state CO(1-0) line is perhaps the most direct tracer of the total molecular gas mass in galaxies, via the alpha_CO conversion factor. However 1-0 is observationally expensive to obtain, and thus most molecular gas surveys target higher-J lines (e.g. 3-2), which are brighter and redshifted to more favourable atmospheric windows. Such surveys must be down-converted to 1-0 via an assumed CO spectral line energy distribution (SLED) in order to measure total gas masses. No such template yet exists in SMGs, and as a result template SLEDs from low-redshift ULIRGs are often used, introducing large uncertainties in the derived properties of SMGs. This survey aims to conduct the first reliable CO SLED survey, using a sample of unlensed SMGs which	ALESS087_a_06_TM1	Dannerbauer, Helmut; Birkin, Jack; Jin, Shuowen; Smail, Ian; Emonts, Bjorn;	1.8336416240480677	0.05617267391262366	0.69911313	uid://A001/X1590/X110	uid://A001/X1590/X111	uid://A002/Xf49cca/X86d8	A CO census of high-redshift submillimetre galaxies in ECDFS	S	PHASE WVR	F	6.5756511726913685	T		Starburst galaxies;Sub-mm Galaxies (SMG)	Active galaxies	apthomson	Thomson, Alasdair	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.01676.S	ALMA	JAO	ALMA	uid://A001/X1590/X111.source.J0348-2749.spw.27	cube	2		J0348-2749	57.15893572085781	-27.820434911128164	0.006892789436223833	Circle ICRS 57.158936 -27.820435 0.003446			1920	1	2	0.4882968686370478	59584.195292	59584.209564	120.96	120.96	0.0012271128916192414	0.0012365996845016814	214724.81648800094	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X111	application/x-votable+xml; content=datalink		2021.1.01676.S	Public	224.52662474860176	-50.90930929109048	6	5.7141393143910026E-9	1.875E9	A001:DA57 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A015:DV21 A016:DA46 A022:DV02 A024:DV06 A025:DV19 A027:DV03 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A040:DA50 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A070:DA51 A072:DA53 A073:DA41 A074:DV09 A075:DA59 A076:DA48 A082:DV22 A083:DV18 A085:DA56 A086:DV17 A087:DV23 A088:DV11 A089:DA52 A090:DV16 A091:DA61 A092:DV13 A093:DV05 A094:DV14	F	2023-01-10T17:52:29.000	0.4882968686370478	[225.02..227.00GHz,31250.00kHz,1.8mJy/beam@10km/s,112.6uJy/beam@native, XX YY] U [226.52..228.50GHz,31250.00kHz,1.7mJy/beam@10km/s,103.9uJy/beam@native, XX YY] U [240.88..242.75GHz,1128.91kHz,1.8mJy/beam@10km/s,117.2uJy/beam@native, XX YY] U [242.43..244.31GHz,1128.91kHz,1.8mJy/beam@10km/s,117.3uJy/beam@native, XX YY]	243.3700311070324	1396.1705167728144	ALMA						Observations of redshifted CO in distant sub-mm selected galaxies (SMGs) probe the physical conditions in which new stars form. When CO is collisionally de-excited from the Jth to the J-1th rotational energy level, the result is a photon whose frequency is J*115GHz. The ground-state CO(1-0) line is perhaps the most direct tracer of the total molecular gas mass in galaxies, via the alpha_CO conversion factor. However 1-0 is observationally expensive to obtain, and thus most molecular gas surveys target higher-J lines (e.g. 3-2), which are brighter and redshifted to more favourable atmospheric windows. Such surveys must be down-converted to 1-0 via an assumed CO spectral line energy distribution (SLED) in order to measure total gas masses. No such template yet exists in SMGs, and as a result template SLEDs from low-redshift ULIRGs are often used, introducing large uncertainties in the derived properties of SMGs. This survey aims to conduct the first reliable CO SLED survey, using a sample of unlensed SMGs which	ALESS087_a_06_TM1	Dannerbauer, Helmut; Birkin, Jack; Jin, Shuowen; Smail, Ian; Emonts, Bjorn;	1.7829224620203492	0.05617267391262366	0.69911313	uid://A001/X1590/X110	uid://A001/X1590/X111	uid://A002/Xf49cca/X86d8	A CO census of high-redshift submillimetre galaxies in ECDFS	S	PHASE WVR	F	6.5756511726913685	T		Starburst galaxies;Sub-mm Galaxies (SMG)	Active galaxies	apthomson	Thomson, Alasdair	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.01676.S	ALMA	JAO	ALMA	uid://A001/X1590/X111.source.J0348-2749.spw.25	cube	2		J0348-2749	57.15893572085781	-27.820434911128164	0.006892789436223833	Circle ICRS 57.158936 -27.820435 0.003446			1920	1	2	0.4882968686370478	59584.195292	59584.209564	120.96	120.96	0.0012349838849532698	0.0012445932457405158	213345.7185570355	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X111	application/x-votable+xml; content=datalink		2021.1.01676.S	Public	224.52662474860176	-50.90930929109048	6	5.787965115398099E-9	1.875E9	A001:DA57 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A015:DV21 A016:DA46 A022:DV02 A024:DV06 A025:DV19 A027:DV03 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A040:DA50 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A070:DA51 A072:DA53 A073:DA41 A074:DV09 A075:DA59 A076:DA48 A082:DV22 A083:DV18 A085:DA56 A086:DV17 A087:DV23 A088:DV11 A089:DA52 A090:DV16 A091:DA61 A092:DV13 A093:DV05 A094:DV14	F	2023-01-10T17:52:29.000	0.4882968686370478	[225.02..227.00GHz,31250.00kHz,1.8mJy/beam@10km/s,112.6uJy/beam@native, XX YY] U [226.52..228.50GHz,31250.00kHz,1.7mJy/beam@10km/s,103.9uJy/beam@native, XX YY] U [240.88..242.75GHz,1128.91kHz,1.8mJy/beam@10km/s,117.2uJy/beam@native, XX YY] U [242.43..244.31GHz,1128.91kHz,1.8mJy/beam@10km/s,117.3uJy/beam@native, XX YY]	241.81297436903697	1396.1705167728144	ALMA						Observations of redshifted CO in distant sub-mm selected galaxies (SMGs) probe the physical conditions in which new stars form. When CO is collisionally de-excited from the Jth to the J-1th rotational energy level, the result is a photon whose frequency is J*115GHz. The ground-state CO(1-0) line is perhaps the most direct tracer of the total molecular gas mass in galaxies, via the alpha_CO conversion factor. However 1-0 is observationally expensive to obtain, and thus most molecular gas surveys target higher-J lines (e.g. 3-2), which are brighter and redshifted to more favourable atmospheric windows. Such surveys must be down-converted to 1-0 via an assumed CO spectral line energy distribution (SLED) in order to measure total gas masses. No such template yet exists in SMGs, and as a result template SLEDs from low-redshift ULIRGs are often used, introducing large uncertainties in the derived properties of SMGs. This survey aims to conduct the first reliable CO SLED survey, using a sample of unlensed SMGs which	ALESS087_a_06_TM1	Dannerbauer, Helmut; Birkin, Jack; Jin, Shuowen; Smail, Ian; Emonts, Bjorn;	1.7871702046116444	0.05617267391262366	0.69911313	uid://A001/X1590/X110	uid://A001/X1590/X111	uid://A002/Xf49cca/X86d8	A CO census of high-redshift submillimetre galaxies in ECDFS	S	PHASE WVR	F	6.5756511726913685	T		Starburst galaxies;Sub-mm Galaxies (SMG)	Active galaxies	apthomson	Thomson, Alasdair	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.01676.S	ALMA	JAO	ALMA	uid://A001/X1590/X111.source.J0348-2749.spw.19	image	2		J0348-2749	57.15893572085781	-27.820434911128164	0.006892789436223833	Circle ICRS 57.158936 -27.820435 0.003446			128	1	2	0.4882968686370478	59584.195292	59584.209564	120.96	120.96	0.0013119760971504913	0.0013234707208547012	7311.278118960234	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X111	application/x-votable+xml; content=datalink		2021.1.01676.S	Public	224.52662474860176	-50.90930929109048	6	1.809962509797255E-7	2.0E9	A001:DA57 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A015:DV21 A016:DA46 A022:DV02 A024:DV06 A025:DV19 A027:DV03 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A040:DA50 A043:DA55 A044:DV12 A045:DA58 A047:DA42 A048:DV10 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A070:DA51 A072:DA53 A073:DA41 A074:DV09 A075:DA59 A076:DA48 A082:DV22 A083:DV18 A085:DA56 A086:DV17 A087:DV23 A088:DV11 A089:DA52 A090:DV16 A091:DA61 A092:DV13 A093:DV05 A094:DV14	F	2023-01-10T17:52:29.000	0.4882968686370478	[225.02..227.00GHz,31250.00kHz,1.8mJy/beam@10km/s,112.6uJy/beam@native, XX YY] U [226.52..228.50GHz,31250.00kHz,1.7mJy/beam@10km/s,103.9uJy/beam@native, XX YY] U [240.88..242.75GHz,1128.91kHz,1.8mJy/beam@10km/s,117.2uJy/beam@native, XX YY] U [242.43..244.31GHz,1128.91kHz,1.8mJy/beam@10km/s,117.3uJy/beam@native, XX YY]	227.51220706744817	1396.1705167728144	ALMA						Observations of redshifted CO in distant sub-mm selected galaxies (SMGs) probe the physical conditions in which new stars form. When CO is collisionally de-excited from the Jth to the J-1th rotational energy level, the result is a photon whose frequency is J*115GHz. The ground-state CO(1-0) line is perhaps the most direct tracer of the total molecular gas mass in galaxies, via the alpha_CO conversion factor. However 1-0 is observationally expensive to obtain, and thus most molecular gas surveys target higher-J lines (e.g. 3-2), which are brighter and redshifted to more favourable atmospheric windows. Such surveys must be down-converted to 1-0 via an assumed CO spectral line energy distribution (SLED) in order to measure total gas masses. No such template yet exists in SMGs, and as a result template SLEDs from low-redshift ULIRGs are often used, introducing large uncertainties in the derived properties of SMGs. This survey aims to conduct the first reliable CO SLED survey, using a sample of unlensed SMGs which	ALESS087_a_06_TM1	Dannerbauer, Helmut; Birkin, Jack; Jin, Shuowen; Smail, Ian; Emonts, Bjorn;	1.687201573838889	0.05617267391262366	0.69911313	uid://A001/X1590/X110	uid://A001/X1590/X111	uid://A002/Xf49cca/X86d8	A CO census of high-redshift submillimetre galaxies in ECDFS	S	PHASE WVR	F	6.5756511726913685	T		Starburst galaxies;Sub-mm Galaxies (SMG)	Active galaxies	apthomson	Thomson, Alasdair	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2012.1.00208.S	ALMA	JAO	ALMA	uid://A002/X628157/X5.source.WLM-NW.spw.13	cube	2		WLM-NW	0.4888333333333333	-15.447083333333333	0.014195746733542222	Circle ICRS 0.488833 -15.447083 0.007098			3840	1	2	0.4819788557799018	56481.344414	56750.50545	2903.04	2903.04	0.0025943511657506636	0.0026049151003088105	473354.3971302662	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A002/X628157/X5	application/x-votable+xml; content=datalink		2012.1.00208.S	Public	75.8875326896972	-73.61179583104362	3	5.503534373279811E-9	4.6875E8	A001:DA64 A006:DV07 A007:DV23 A010:DV12 A011:DV22 A016:DA62 A018:DA60 A020:DV20 A021:DA59 A025:DV14 A026:DA47 A029:DA49 A031:DV11 A033:DV18 A037:DV06 A038:DA53 A038:DV24 A042:DV15 A045:DA50 A046:DA48 A054:DA55 A056:DV25 A058:DA46 A060:DV09 A062:DV05 A063:DA54 A064:DA56 A066:DA43 A067:DA46 A067:DV13 A068:DA44 A069:DV16 A070:DA45 A071:DV10 A072:DV13 A074:DA47 A074:DV15 A075:DA43 A075:DA61 A077:DV02 A077:DV19 A078:DV04 A079:DA41 A080:DV18 A081:DA42 A081:DV01 A082:DV05 A087:DA58 A096:DV07 A106:DV25 A117:DV19 A131:DV24 A137:DA55 A137:DV03 A138:DV17 T703:PM04 T704:PM01	F	2015-07-02T14:09:15.000	0.4819788557799018	[112.33..114.31GHz,31250.00kHz,1.6mJy/beam@10km/s,71.6uJy/beam@native, XX YY] U [115.09..115.56GHz,244.14kHz,1.4mJy/beam@10km/s,128.7uJy/beam@native, XX YY]	115.32153972727079	633.3361638077225	ALMA	Dense cloud cores revealed by CO in the low metallicity dwarf galaxy WLM Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM	Archer, Haylee N. Rubio, Monica	Archer, Haylee N.; Hunter, Deidre A.; Elmegreen, Bruce G.; Cigan, Phil; Jansen, Rolf A.; Windhorst, Rogier A.; Hunt, Leslie K.; Rubio, Monica Archer, Haylee N.; Hunter, Deidre A.; Elmegreen, Bruce G.; Hunt, Leslie K.; O'Brien, Rosalia; Brinks, Elias; Cigan, Phil; Rubio, Monica; Windhorst, Rogier A.; Jansen, Rolf A.; Mathews, Elijah P. Archer, Haylee N.; Hunter, Deidre A.; Elmegreen, Bruce G.; Rubio, Monica; Cigan, Phil; Windhorst, Rogier A.; Cortés, Juan R.; Jansen, Rolf A. Rubio, Monica; Elmegreen, Bruce G.; Hunter, Deidre A.; Brinks, Elias; Cortés, Juan R.; Cigan, Phil	The low metallicities of dwarf irregular galaxies (dIrr) greatly influence the formation and structure of molecular clouds. These clouds, which consist primarily of H<SUB>2</SUB>, are typically traced by CO, but low-metallicity galaxies are found to have little CO despite ongoing star formation. In order to probe the conditions necessary for CO core formation in dwarf galaxies, we have used the catalog of Rubio et al. for CO cores in WLM, a Local Group dwarf with an oxygen abundance that is 13% of solar. Here we aim to characterize the galactic environments in which these 57 CO cores formed. We grouped the cores together based on proximity to each other and strong FUV emission, examining properties of the star-forming region enveloping the cores and the surrounding environment where the cores formed. We find that high H I surface density does not necessarily correspond to higher total CO mass, but regions with higher CO mass have higher H I surface densities. We also find the cores in star-forming regions spa	2015	Stars form out of molecular clouds, dense concentrations of gas that are traditionally traced in external galaxies using transitions of CO. However, the structure of molecular clouds at low metallicities may be fundamentally different compared to that found in higher metallicity spirals. In particular, the CO core in a typical cloud is expected to shrink and the photo-dissociation region (PDR) grow with decreasing metallicity. This potentially has profound affects on the star formation process. We propose to map 12CO 1-0 in two regions of the low metallicity dwarf galaxy WLM where we have 12CO 3-2 detections with the single-dish APEX-2 telescope. These will be the lowest metallicity clouds ever mapped at this detail (by a factor of 1.6). With the ALMA data, coupled with our Herschel PDR fine-structure line maps, we will determine the structure of the molecular cloud to test the theoretical prediction on molecular cloud differences at low metallicity. This simple observation will demonstrate that ALMA can prob	WLM-NW-SE_115_12m_C32-2	Young, Lisa; Rubio, Monica; Brinks, Elias; Elmegreen, Bruce; Simpson, Caroline;	1.4208650241793324	0.06254455290480532	4.488383	uid://A002/X628157/X4	uid://A002/X628157/X5	uid://A002/X6a533e/X1855	The Lowest Metallicity Molecular Clouds	S	TARGET WVR	T	16.005107323701623	T	2015Natur.525..218R 2022AJ....163..141A 2024AJ....167..274A 2025AJ....169..301A	Dwarf/metal-poor galaxies;Giant Molecular Clouds (GMC) properties	Local Universe	dhunter	Hunter, Deidre	244.140625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2012.1.00208.S	ALMA	JAO	ALMA	uid://A002/X628157/X5.source.WLM-NW.spw.15	image	2		WLM-NW	0.4888333333333333	-15.447083333333333	0.014195746733542222	Circle ICRS 0.488833 -15.447083 0.007098			128	1	2	0.4819788557799018	56481.344414	56750.50545	2903.04	2903.04	0.0026225884905870874	0.002668918074534811	3658.263663628157	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A002/X628157/X5	application/x-votable+xml; content=datalink		2012.1.00208.S	Public	75.8875326896972	-73.61179583104362	3	7.296166103637901E-7	2.0E9	A001:DA64 A006:DV07 A007:DV23 A010:DV12 A011:DV22 A016:DA62 A018:DA60 A020:DV20 A021:DA59 A025:DV14 A026:DA47 A029:DA49 A031:DV11 A033:DV18 A037:DV06 A038:DA53 A038:DV24 A042:DV15 A045:DA50 A046:DA48 A054:DA55 A056:DV25 A058:DA46 A060:DV09 A062:DV05 A063:DA54 A064:DA56 A066:DA43 A067:DA46 A067:DV13 A068:DA44 A069:DV16 A070:DA45 A071:DV10 A072:DV13 A074:DA47 A074:DV15 A075:DA43 A075:DA61 A077:DV02 A077:DV19 A078:DV04 A079:DA41 A080:DV18 A081:DA42 A081:DV01 A082:DV05 A087:DA58 A096:DV07 A106:DV25 A117:DV19 A131:DV24 A137:DA55 A137:DV03 A138:DV17 T703:PM04 T704:PM01	F	2015-07-02T14:09:15.000	0.4819788557799018	[112.33..114.31GHz,31250.00kHz,1.6mJy/beam@10km/s,71.6uJy/beam@native, XX YY] U [115.09..115.56GHz,244.14kHz,1.4mJy/beam@10km/s,128.7uJy/beam@native, XX YY]	113.3195008249677	633.3361638077225	ALMA	Dense cloud cores revealed by CO in the low metallicity dwarf galaxy WLM Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM	Archer, Haylee N. Rubio, Monica	Archer, Haylee N.; Hunter, Deidre A.; Elmegreen, Bruce G.; Cigan, Phil; Jansen, Rolf A.; Windhorst, Rogier A.; Hunt, Leslie K.; Rubio, Monica Archer, Haylee N.; Hunter, Deidre A.; Elmegreen, Bruce G.; Hunt, Leslie K.; O'Brien, Rosalia; Brinks, Elias; Cigan, Phil; Rubio, Monica; Windhorst, Rogier A.; Jansen, Rolf A.; Mathews, Elijah P. Archer, Haylee N.; Hunter, Deidre A.; Elmegreen, Bruce G.; Rubio, Monica; Cigan, Phil; Windhorst, Rogier A.; Cortés, Juan R.; Jansen, Rolf A. Rubio, Monica; Elmegreen, Bruce G.; Hunter, Deidre A.; Brinks, Elias; Cortés, Juan R.; Cigan, Phil	The low metallicities of dwarf irregular galaxies (dIrr) greatly influence the formation and structure of molecular clouds. These clouds, which consist primarily of H<SUB>2</SUB>, are typically traced by CO, but low-metallicity galaxies are found to have little CO despite ongoing star formation. In order to probe the conditions necessary for CO core formation in dwarf galaxies, we have used the catalog of Rubio et al. for CO cores in WLM, a Local Group dwarf with an oxygen abundance that is 13% of solar. Here we aim to characterize the galactic environments in which these 57 CO cores formed. We grouped the cores together based on proximity to each other and strong FUV emission, examining properties of the star-forming region enveloping the cores and the surrounding environment where the cores formed. We find that high H I surface density does not necessarily correspond to higher total CO mass, but regions with higher CO mass have higher H I surface densities. We also find the cores in star-forming regions spa	2015	Stars form out of molecular clouds, dense concentrations of gas that are traditionally traced in external galaxies using transitions of CO. However, the structure of molecular clouds at low metallicities may be fundamentally different compared to that found in higher metallicity spirals. In particular, the CO core in a typical cloud is expected to shrink and the photo-dissociation region (PDR) grow with decreasing metallicity. This potentially has profound affects on the star formation process. We propose to map 12CO 1-0 in two regions of the low metallicity dwarf galaxy WLM where we have 12CO 3-2 detections with the single-dish APEX-2 telescope. These will be the lowest metallicity clouds ever mapped at this detail (by a factor of 1.6). With the ALMA data, coupled with our Herschel PDR fine-structure line maps, we will determine the structure of the molecular cloud to test the theoretical prediction on molecular cloud differences at low metallicity. This simple observation will demonstrate that ALMA can prob	WLM-NW-SE_115_12m_C32-2	Young, Lisa; Rubio, Monica; Brinks, Elias; Elmegreen, Bruce; Simpson, Caroline;	1.6460716178475887	0.06254455290480532	4.488383	uid://A002/X628157/X4	uid://A002/X628157/X5	uid://A002/X6a533e/X1855	The Lowest Metallicity Molecular Clouds	S	TARGET WVR	T	16.005107323701623	T	2015Natur.525..218R 2022AJ....163..141A 2024AJ....167..274A 2025AJ....169..301A	Dwarf/metal-poor galaxies;Giant Molecular Clouds (GMC) properties	Local Universe	dhunter	Hunter, Deidre	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00222.S	ALMA	JAO	ALMA	uid://A001/X2fb/X390.source.LupusIII_89.spw.27	cube	2		LupusIII_89	242.3464583333365	-39.06872222222723	0.007175461252508504	Polygon ICRS 242.347886 -39.065310 242.349404 -39.065958 242.350508 -39.066994 242.351043 -39.068272 242.351070 -39.068947 242.350853 -39.069831 242.350019 -39.071009 242.349404 -39.071487 242.348426 -39.071968 242.346749 -39.072303 242.345030 -39.072134 242.343513 -39.071487 242.342409 -39.070451 242.341874 -39.069172 242.341874 -39.068272 242.342064 -39.067613 242.342557 -39.066800 242.343090 -39.066266 242.344491 -39.065476 242.346168 -39.065142			960	1	2	0.17212287051357575	57593.0288	57639.841145	90.72	90.72	0.0013598887217112067	0.0013606114549667113	1562157.0531599543	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X390	application/x-votable+xml; content=datalink		2015.1.00222.S	Public	339.6664406724036	9.293307195365811	6	8.7093287162229E-10	1.171875E8	A001:DA59 A002:DA49 A004:DA41 A006:DA61 A007:DV12 A008:DV06 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A077:DA58 A079:DA64 A080:DV23 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A106:DV08 A108:DA54 A109:DA55 A112:DA50 A113:DV15 A114:DA52 A115:DA44 A130:DA64 A134:DA44 A135:DV19 A136:DV04 T701:PM03 T703:PM04 T704:PM01	F	2017-12-18T21:28:28.000	0.17212287051357575	[215.55..217.42GHz,1128.91kHz,3.8mJy/beam@10km/s,234.3uJy/beam@native, XX YY] U [219.50..219.62GHz,141.11kHz,3.8mJy/beam@10km/s,938.6uJy/beam@native, XX YY] U [220.34..220.45GHz,141.11kHz,3.7mJy/beam@10km/s,939uJy/beam@native, XX YY] U [230.48..230.59GHz,121.15kHz,3.7mJy/beam@10km/s,943.3uJy/beam@native, XX YY] U [233.30..235.29GHz,31250.00kHz,3.7mJy/beam@10km/s,233.3uJy/beam@native, XX YY]	220.395118315569	157.60175986830563	ALMA	ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii Constraining the gas mass of Herbig disks using CO isotopologues Constraining the radial drift of millimeter-sized grains in the protoplanetary disks in Lupus Dynamical Stellar Masses of Pre-main-sequence Stars in Lupus and Taurus Obtained with ALMA Surveys in Comparison with Stellar Evolutionary Models Gas Disk Sizes from CO Line Observations: A Test of Angular Momentum Evolution High-resolution ALMA observations of compact discs in the wide-binary system Sz 65 and Sz 66 Intermediate mass T Tauri disk masses and a comparison to their Herbig disk descendants Measuring the ratio of the gas and dust emission radii of protoplanetary disks in the Lupus star-forming region Multiwavelength continuum sizes of protoplanetary discs: scaling relations and implications for grain growth and radial drift Protoplanetary Disk Rings and Gaps across Ages and Luminosities Spatial segregation of dust grains in transition disks. SPHERE observations of 2MASS J16083070-	Ansdell, M. Braun, Teresa A. M. Long, Feng Miley, J. M. Sanchis, E. Stapper, L. M. Tazzari, M. Trapman, L. Villenave, M. Zagaria, Francesco Zurlo, Alice van Terwisga, S. E. van der Marel, Nienke	Ansdell, M.; Williams, J. P.; Trapman, L.; van Terwisga, S. E.; Facchini, S.; Manara, C. F.; van der Marel, N.; Miotello, A.; Tazzari, M.; Hogerheijde, M.; Guidi, G.; Testi, L.; van Dishoeck, E. F. Braun, Teresa A. M.; Yen, Hsi-Wei; Koch, Patrick M.; Manara, Carlo F.; Miotello, Anna; Testi, Leonardo Long, Feng; Andrews, Sean M.; Rosotti, Giovanni; Harsono, Daniel; Pinilla, Paola; Wilner, David J.; Öberg, Karin I.; Teague, Richard; Trapman, Leon; Tabone, Benoît Miley, J. M.; Carpenter, J.; Booth, R.; Jennings, J.; Haworth, T. J.; Vioque, M.; Andrews, S.; Wilner, D.; Benisty, M.; Huang, J.; Perez, L.; Guzman, V.; Ricci, L.; Isella, A. Sanchis, E.; Testi, L.; Natta, A.; Facchini, S.; Manara, C. F.; Miotello, A.; Ercolano, B.; Henning, Th.; Preibisch, T.; Carpenter, J. M.; de Gregorio-Monsalvo, I.; Jayawardhana, R.; Lopez, C.; Mužić, K.; Pascucci, I.; Santamaría-Miranda, A.; van Terwisga, S.; Williams, J. P. Stapper, L. M.; Hogerheijde, M. R.; van Dishoeck, E. F.; Lin, L.; Ahmadi, A.; Booth, A. S.; Grant, S. L.;	Context. Herbig disks are prime sites for the formation of massive exoplanets and looking into the precursors of these disks can offer clues for determining planet formation timescales. The precursors of Herbig stars, called intermediate-mass T Tauri (IMTT) stars, have spectral types later than F, but stellar masses between 1.5 and 5 M<SUB>⊙</SUB>. These stars will eventually become Herbig stars of spectral types A and B. Aims. The aim of this work is to obtain the dust and gas masses and radii of all IMTT disks with ALMA archival data. The obtained disk masses are then compared to Herbig disks and T Tauri disks and the obtained disks sizes to those of Herbig disks. Methods. ALMA Band 6 and 7 archival data were obtained for 34 IMTT disks with continuum observations, 32 of which have at least <SUP>12</SUP>CO, <SUP>13</SUP>CO, or C<SUP>18</SUP>O observations, but with most of them at quite shallow integrations. The disk integrated flux together with a stellar luminosity-scaled disk temperature were used to obta	2018	We propose to survey the gas and dust in 98 protoplanetary disks in the nearby Lupus star-forming region. This is a complete sample of all known optically visible stars with large infrared excesses and stellar masses > 0.1 solar. We will observe the CO, 13CO and C18O 2-1 lines and have developed models to derive gas masses. We will image with a resolution that corresponds to 20AU in radius while maintaining sensitivity over the entire disk. We expect to detect almost all disks in the continuum and measure sub-Jupiter masses of gas. From the resolved images, we will determine radial profiles of the gas, dust, and gas-to-dust ratio, as well as characterize the prevalence of dust holes and asymmetries. This efficient, large, and complete survey will provide an unbiased view of the gas and dust properties in young planet-forming disks, and is complemented by our VLT optical-infrared spectroscopic survey of the host stars.	LupusIII_a_06_TE	van der Marel, Nienke; Oliveira, Isa; Mathews, Geoffrey; van Dishoeck, Ewine; Manara, Carlo Felice; Ansdell, Megan; Natta, Antonella; Miotello, Anna; Carpenter, John; Alcala', Juan Manuel; Testi, Leonardo; Tazzari, Marco; Guidi, Greta; Hogerheijde, Michiel;	3.748909803852401	0.15814175477574752	0.71056074	uid://A001/X2fb/X38f	uid://A001/X2fb/X390	uid://A002/Xb5bd46/X64b2	Disk demographics in Lupus	S	TARGET	T	3.7042307812178303	T	2018ApJ...859...21A 2019A&A...623A.150V 2019A&A...624A...7V 2019ApJ...872..112V 2020A&A...638A..38T 2021A&A...649A..19S 2021ApJ...908...46B 2021MNRAS.501.2305Z 2021MNRAS.506.2804T 2022ApJ...931....6L 2023A&A...672L..15Z 2024A&A...682A..55M 2024A&A...682A.149S 2025A&A...693A.286S	Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00222.S	ALMA	JAO	ALMA	uid://A001/X2fb/X390.source.LupusIII_89.spw.25	cube	2		LupusIII_89	242.3464583333365	-39.06872222222723	0.007175461252508504	Polygon ICRS 242.347886 -39.065310 242.349404 -39.065958 242.350508 -39.066994 242.351043 -39.068272 242.351070 -39.068947 242.350853 -39.069831 242.350019 -39.071009 242.349404 -39.071487 242.348426 -39.071968 242.346749 -39.072303 242.345030 -39.072134 242.343513 -39.071487 242.342409 -39.070451 242.341874 -39.069172 242.341874 -39.068272 242.342064 -39.067613 242.342557 -39.066800 242.343090 -39.066266 242.344491 -39.065476 242.346168 -39.065142			960	1	2	0.17212287051357575	57593.0288	57639.841145	90.72	90.72	0.0013650800876078514	0.0013658082642300118	1556216.3092153175	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X390	application/x-votable+xml; content=datalink		2015.1.00222.S	Public	339.6664406724036	9.293307195365811	6	8.775968493273981E-10	1.171875E8	A001:DA59 A002:DA49 A004:DA41 A006:DA61 A007:DV12 A008:DV06 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A077:DA58 A079:DA64 A080:DV23 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A106:DV08 A108:DA54 A109:DA55 A112:DA50 A113:DV15 A114:DA52 A115:DA44 A130:DA64 A134:DA44 A135:DV19 A136:DV04 T701:PM03 T703:PM04 T704:PM01	F	2017-12-18T21:28:28.000	0.17212287051357575	[215.55..217.42GHz,1128.91kHz,3.8mJy/beam@10km/s,234.3uJy/beam@native, XX YY] U [219.50..219.62GHz,141.11kHz,3.8mJy/beam@10km/s,938.6uJy/beam@native, XX YY] U [220.34..220.45GHz,141.11kHz,3.7mJy/beam@10km/s,939uJy/beam@native, XX YY] U [230.48..230.59GHz,121.15kHz,3.7mJy/beam@10km/s,943.3uJy/beam@native, XX YY] U [233.30..235.29GHz,31250.00kHz,3.7mJy/beam@10km/s,233.3uJy/beam@native, XX YY]	219.55674541823726	157.60175986830563	ALMA	ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii Constraining the gas mass of Herbig disks using CO isotopologues Constraining the radial drift of millimeter-sized grains in the protoplanetary disks in Lupus Dynamical Stellar Masses of Pre-main-sequence Stars in Lupus and Taurus Obtained with ALMA Surveys in Comparison with Stellar Evolutionary Models Gas Disk Sizes from CO Line Observations: A Test of Angular Momentum Evolution High-resolution ALMA observations of compact discs in the wide-binary system Sz 65 and Sz 66 Intermediate mass T Tauri disk masses and a comparison to their Herbig disk descendants Measuring the ratio of the gas and dust emission radii of protoplanetary disks in the Lupus star-forming region Multiwavelength continuum sizes of protoplanetary discs: scaling relations and implications for grain growth and radial drift Protoplanetary Disk Rings and Gaps across Ages and Luminosities Spatial segregation of dust grains in transition disks. SPHERE observations of 2MASS J16083070-	Ansdell, M. Braun, Teresa A. M. Long, Feng Miley, J. M. Sanchis, E. Stapper, L. M. Tazzari, M. Trapman, L. Villenave, M. Zagaria, Francesco Zurlo, Alice van Terwisga, S. E. van der Marel, Nienke	Ansdell, M.; Williams, J. P.; Trapman, L.; van Terwisga, S. E.; Facchini, S.; Manara, C. F.; van der Marel, N.; Miotello, A.; Tazzari, M.; Hogerheijde, M.; Guidi, G.; Testi, L.; van Dishoeck, E. F. Braun, Teresa A. M.; Yen, Hsi-Wei; Koch, Patrick M.; Manara, Carlo F.; Miotello, Anna; Testi, Leonardo Long, Feng; Andrews, Sean M.; Rosotti, Giovanni; Harsono, Daniel; Pinilla, Paola; Wilner, David J.; Öberg, Karin I.; Teague, Richard; Trapman, Leon; Tabone, Benoît Miley, J. M.; Carpenter, J.; Booth, R.; Jennings, J.; Haworth, T. J.; Vioque, M.; Andrews, S.; Wilner, D.; Benisty, M.; Huang, J.; Perez, L.; Guzman, V.; Ricci, L.; Isella, A. Sanchis, E.; Testi, L.; Natta, A.; Facchini, S.; Manara, C. F.; Miotello, A.; Ercolano, B.; Henning, Th.; Preibisch, T.; Carpenter, J. M.; de Gregorio-Monsalvo, I.; Jayawardhana, R.; Lopez, C.; Mužić, K.; Pascucci, I.; Santamaría-Miranda, A.; van Terwisga, S.; Williams, J. P. Stapper, L. M.; Hogerheijde, M. R.; van Dishoeck, E. F.; Lin, L.; Ahmadi, A.; Booth, A. S.; Grant, S. L.;	Context. Herbig disks are prime sites for the formation of massive exoplanets and looking into the precursors of these disks can offer clues for determining planet formation timescales. The precursors of Herbig stars, called intermediate-mass T Tauri (IMTT) stars, have spectral types later than F, but stellar masses between 1.5 and 5 M<SUB>⊙</SUB>. These stars will eventually become Herbig stars of spectral types A and B. Aims. The aim of this work is to obtain the dust and gas masses and radii of all IMTT disks with ALMA archival data. The obtained disk masses are then compared to Herbig disks and T Tauri disks and the obtained disks sizes to those of Herbig disks. Methods. ALMA Band 6 and 7 archival data were obtained for 34 IMTT disks with continuum observations, 32 of which have at least <SUP>12</SUP>CO, <SUP>13</SUP>CO, or C<SUP>18</SUP>O observations, but with most of them at quite shallow integrations. The disk integrated flux together with a stellar luminosity-scaled disk temperature were used to obta	2018	We propose to survey the gas and dust in 98 protoplanetary disks in the nearby Lupus star-forming region. This is a complete sample of all known optically visible stars with large infrared excesses and stellar masses > 0.1 solar. We will observe the CO, 13CO and C18O 2-1 lines and have developed models to derive gas masses. We will image with a resolution that corresponds to 20AU in radius while maintaining sensitivity over the entire disk. We expect to detect almost all disks in the continuum and measure sub-Jupiter masses of gas. From the resolved images, we will determine radial profiles of the gas, dust, and gas-to-dust ratio, as well as characterize the prevalence of dust holes and asymmetries. This efficient, large, and complete survey will provide an unbiased view of the gas and dust properties in young planet-forming disks, and is complemented by our VLT optical-infrared spectroscopic survey of the host stars.	LupusIII_a_06_TE	van der Marel, Nienke; Oliveira, Isa; Mathews, Geoffrey; van Dishoeck, Ewine; Manara, Carlo Felice; Ansdell, Megan; Natta, Antonella; Miotello, Anna; Carpenter, John; Alcala', Juan Manuel; Testi, Leonardo; Tazzari, Marco; Guidi, Greta; Hogerheijde, Michiel;	3.754539494869223	0.15814175477574752	0.71056074	uid://A001/X2fb/X38f	uid://A001/X2fb/X390	uid://A002/Xb5bd46/X64b2	Disk demographics in Lupus	S	TARGET	T	3.7042307812178303	T	2018ApJ...859...21A 2019A&A...623A.150V 2019A&A...624A...7V 2019ApJ...872..112V 2020A&A...638A..38T 2021A&A...649A..19S 2021ApJ...908...46B 2021MNRAS.501.2305Z 2021MNRAS.506.2804T 2022ApJ...931....6L 2023A&A...672L..15Z 2024A&A...682A..55M 2024A&A...682A.149S 2025A&A...693A.286S	Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	141.11328125	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00222.S	ALMA	JAO	ALMA	uid://A001/X2fb/X390.source.LupusIII_89.spw.23	image	2		LupusIII_89	242.3464583333365	-39.06872222222723	0.007175461252508504	Polygon ICRS 242.347886 -39.065310 242.349404 -39.065958 242.350508 -39.066994 242.351043 -39.068272 242.351070 -39.068947 242.350853 -39.069831 242.350019 -39.071009 242.349404 -39.071487 242.348426 -39.071968 242.346749 -39.072303 242.345030 -39.072134 242.343513 -39.071487 242.342409 -39.070451 242.341874 -39.069172 242.341874 -39.068272 242.342064 -39.067613 242.342557 -39.066800 242.343090 -39.066266 242.344491 -39.065476 242.346168 -39.065142			128	1	2	0.17212287051357575	57593.0288	57639.841145	90.72	90.72	0.001274148873861075	0.0012849870213688223	7465.299691408143	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X390	application/x-votable+xml; content=datalink		2015.1.00222.S	Public	339.6664406724036	9.293307195365811	6	1.7066648135574328E-7	2.0E9	A001:DA59 A002:DA49 A004:DA41 A006:DA61 A007:DV12 A008:DV06 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A077:DA58 A079:DA64 A080:DV23 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A106:DV08 A108:DA54 A109:DA55 A112:DA50 A113:DV15 A114:DA52 A115:DA44 A130:DA64 A134:DA44 A135:DV19 A136:DV04 T701:PM03 T703:PM04 T704:PM01	F	2017-12-18T21:28:28.000	0.17212287051357575	[215.55..217.42GHz,1128.91kHz,3.8mJy/beam@10km/s,234.3uJy/beam@native, XX YY] U [219.50..219.62GHz,141.11kHz,3.8mJy/beam@10km/s,938.6uJy/beam@native, XX YY] U [220.34..220.45GHz,141.11kHz,3.7mJy/beam@10km/s,939uJy/beam@native, XX YY] U [230.48..230.59GHz,121.15kHz,3.7mJy/beam@10km/s,943.3uJy/beam@native, XX YY] U [233.30..235.29GHz,31250.00kHz,3.7mJy/beam@10km/s,233.3uJy/beam@native, XX YY]	234.2961432457137	157.60175986830563	ALMA	ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii Constraining the gas mass of Herbig disks using CO isotopologues Constraining the radial drift of millimeter-sized grains in the protoplanetary disks in Lupus Dynamical Stellar Masses of Pre-main-sequence Stars in Lupus and Taurus Obtained with ALMA Surveys in Comparison with Stellar Evolutionary Models Gas Disk Sizes from CO Line Observations: A Test of Angular Momentum Evolution High-resolution ALMA observations of compact discs in the wide-binary system Sz 65 and Sz 66 Intermediate mass T Tauri disk masses and a comparison to their Herbig disk descendants Measuring the ratio of the gas and dust emission radii of protoplanetary disks in the Lupus star-forming region Multiwavelength continuum sizes of protoplanetary discs: scaling relations and implications for grain growth and radial drift Protoplanetary Disk Rings and Gaps across Ages and Luminosities Spatial segregation of dust grains in transition disks. SPHERE observations of 2MASS J16083070-	Ansdell, M. Braun, Teresa A. M. Long, Feng Miley, J. M. Sanchis, E. Stapper, L. M. Tazzari, M. Trapman, L. Villenave, M. Zagaria, Francesco Zurlo, Alice van Terwisga, S. E. van der Marel, Nienke	Ansdell, M.; Williams, J. P.; Trapman, L.; van Terwisga, S. E.; Facchini, S.; Manara, C. F.; van der Marel, N.; Miotello, A.; Tazzari, M.; Hogerheijde, M.; Guidi, G.; Testi, L.; van Dishoeck, E. F. Braun, Teresa A. M.; Yen, Hsi-Wei; Koch, Patrick M.; Manara, Carlo F.; Miotello, Anna; Testi, Leonardo Long, Feng; Andrews, Sean M.; Rosotti, Giovanni; Harsono, Daniel; Pinilla, Paola; Wilner, David J.; Öberg, Karin I.; Teague, Richard; Trapman, Leon; Tabone, Benoît Miley, J. M.; Carpenter, J.; Booth, R.; Jennings, J.; Haworth, T. J.; Vioque, M.; Andrews, S.; Wilner, D.; Benisty, M.; Huang, J.; Perez, L.; Guzman, V.; Ricci, L.; Isella, A. Sanchis, E.; Testi, L.; Natta, A.; Facchini, S.; Manara, C. F.; Miotello, A.; Ercolano, B.; Henning, Th.; Preibisch, T.; Carpenter, J. M.; de Gregorio-Monsalvo, I.; Jayawardhana, R.; Lopez, C.; Mužić, K.; Pascucci, I.; Santamaría-Miranda, A.; van Terwisga, S.; Williams, J. P. Stapper, L. M.; Hogerheijde, M. R.; van Dishoeck, E. F.; Lin, L.; Ahmadi, A.; Booth, A. S.; Grant, S. L.;	Context. Herbig disks are prime sites for the formation of massive exoplanets and looking into the precursors of these disks can offer clues for determining planet formation timescales. The precursors of Herbig stars, called intermediate-mass T Tauri (IMTT) stars, have spectral types later than F, but stellar masses between 1.5 and 5 M<SUB>⊙</SUB>. These stars will eventually become Herbig stars of spectral types A and B. Aims. The aim of this work is to obtain the dust and gas masses and radii of all IMTT disks with ALMA archival data. The obtained disk masses are then compared to Herbig disks and T Tauri disks and the obtained disks sizes to those of Herbig disks. Methods. ALMA Band 6 and 7 archival data were obtained for 34 IMTT disks with continuum observations, 32 of which have at least <SUP>12</SUP>CO, <SUP>13</SUP>CO, or C<SUP>18</SUP>O observations, but with most of them at quite shallow integrations. The disk integrated flux together with a stellar luminosity-scaled disk temperature were used to obta	2018	We propose to survey the gas and dust in 98 protoplanetary disks in the nearby Lupus star-forming region. This is a complete sample of all known optically visible stars with large infrared excesses and stellar masses > 0.1 solar. We will observe the CO, 13CO and C18O 2-1 lines and have developed models to derive gas masses. We will image with a resolution that corresponds to 20AU in radius while maintaining sensitivity over the entire disk. We expect to detect almost all disks in the continuum and measure sub-Jupiter masses of gas. From the resolved images, we will determine radial profiles of the gas, dust, and gas-to-dust ratio, as well as characterize the prevalence of dust holes and asymmetries. This efficient, large, and complete survey will provide an unbiased view of the gas and dust properties in young planet-forming disks, and is complemented by our VLT optical-infrared spectroscopic survey of the host stars.	LupusIII_a_06_TE	van der Marel, Nienke; Oliveira, Isa; Mathews, Geoffrey; van Dishoeck, Ewine; Manara, Carlo Felice; Ansdell, Megan; Natta, Antonella; Miotello, Anna; Carpenter, John; Alcala', Juan Manuel; Testi, Leonardo; Tazzari, Marco; Guidi, Greta; Hogerheijde, Michiel;	3.73165998204699	0.15814175477574752	0.71056074	uid://A001/X2fb/X38f	uid://A001/X2fb/X390	uid://A002/Xb5bd46/X64b2	Disk demographics in Lupus	S	TARGET	T	3.7042307812178303	T	2018ApJ...859...21A 2019A&A...623A.150V 2019A&A...624A...7V 2019ApJ...872..112V 2020A&A...638A..38T 2021A&A...649A..19S 2021ApJ...908...46B 2021MNRAS.501.2305Z 2021MNRAS.506.2804T 2022ApJ...931....6L 2023A&A...672L..15Z 2024A&A...682A..55M 2024A&A...682A.149S 2025A&A...693A.286S	Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00222.S	ALMA	JAO	ALMA	uid://A001/X2fb/X390.source.LupusIII_89.spw.29	cube	2		LupusIII_89	242.3464583333365	-39.06872222222723	0.007175461252508504	Polygon ICRS 242.347886 -39.065310 242.349404 -39.065958 242.350508 -39.066994 242.351043 -39.068272 242.351070 -39.068947 242.350853 -39.069831 242.350019 -39.071009 242.349404 -39.071487 242.348426 -39.071968 242.346749 -39.072303 242.345030 -39.072134 242.343513 -39.071487 242.342409 -39.070451 242.341874 -39.069172 242.341874 -39.068272 242.342064 -39.067613 242.342557 -39.066800 242.343090 -39.066266 242.344491 -39.065476 242.346168 -39.065142			1920	1	2	0.17212287051357575	57593.0288	57639.841145	90.72	90.72	0.0013788374298970962	0.0013908269219966229	192586.1526225029	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X390	application/x-votable+xml; content=datalink		2015.1.00222.S	Public	339.6664406724036	9.293307195365811	6	7.221432021835393E-9	1.875E9	A001:DA59 A002:DA49 A004:DA41 A006:DA61 A007:DV12 A008:DV06 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A077:DA58 A079:DA64 A080:DV23 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A106:DV08 A108:DA54 A109:DA55 A112:DA50 A113:DV15 A114:DA52 A115:DA44 A130:DA64 A134:DA44 A135:DV19 A136:DV04 T701:PM03 T703:PM04 T704:PM01	F	2017-12-18T21:28:28.000	0.17212287051357575	[215.55..217.42GHz,1128.91kHz,3.8mJy/beam@10km/s,234.3uJy/beam@native, XX YY] U [219.50..219.62GHz,141.11kHz,3.8mJy/beam@10km/s,938.6uJy/beam@native, XX YY] U [220.34..220.45GHz,141.11kHz,3.7mJy/beam@10km/s,939uJy/beam@native, XX YY] U [230.48..230.59GHz,121.15kHz,3.7mJy/beam@10km/s,943.3uJy/beam@native, XX YY] U [233.30..235.29GHz,31250.00kHz,3.7mJy/beam@10km/s,233.3uJy/beam@native, XX YY]	216.4869369261432	157.60175986830563	ALMA	ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii Constraining the gas mass of Herbig disks using CO isotopologues Constraining the radial drift of millimeter-sized grains in the protoplanetary disks in Lupus Dynamical Stellar Masses of Pre-main-sequence Stars in Lupus and Taurus Obtained with ALMA Surveys in Comparison with Stellar Evolutionary Models Gas Disk Sizes from CO Line Observations: A Test of Angular Momentum Evolution High-resolution ALMA observations of compact discs in the wide-binary system Sz 65 and Sz 66 Intermediate mass T Tauri disk masses and a comparison to their Herbig disk descendants Measuring the ratio of the gas and dust emission radii of protoplanetary disks in the Lupus star-forming region Multiwavelength continuum sizes of protoplanetary discs: scaling relations and implications for grain growth and radial drift Protoplanetary Disk Rings and Gaps across Ages and Luminosities Spatial segregation of dust grains in transition disks. SPHERE observations of 2MASS J16083070-	Ansdell, M. Braun, Teresa A. M. Long, Feng Miley, J. M. Sanchis, E. Stapper, L. M. Tazzari, M. Trapman, L. Villenave, M. Zagaria, Francesco Zurlo, Alice van Terwisga, S. E. van der Marel, Nienke	Ansdell, M.; Williams, J. P.; Trapman, L.; van Terwisga, S. E.; Facchini, S.; Manara, C. F.; van der Marel, N.; Miotello, A.; Tazzari, M.; Hogerheijde, M.; Guidi, G.; Testi, L.; van Dishoeck, E. F. Braun, Teresa A. M.; Yen, Hsi-Wei; Koch, Patrick M.; Manara, Carlo F.; Miotello, Anna; Testi, Leonardo Long, Feng; Andrews, Sean M.; Rosotti, Giovanni; Harsono, Daniel; Pinilla, Paola; Wilner, David J.; Öberg, Karin I.; Teague, Richard; Trapman, Leon; Tabone, Benoît Miley, J. M.; Carpenter, J.; Booth, R.; Jennings, J.; Haworth, T. J.; Vioque, M.; Andrews, S.; Wilner, D.; Benisty, M.; Huang, J.; Perez, L.; Guzman, V.; Ricci, L.; Isella, A. Sanchis, E.; Testi, L.; Natta, A.; Facchini, S.; Manara, C. F.; Miotello, A.; Ercolano, B.; Henning, Th.; Preibisch, T.; Carpenter, J. M.; de Gregorio-Monsalvo, I.; Jayawardhana, R.; Lopez, C.; Mužić, K.; Pascucci, I.; Santamaría-Miranda, A.; van Terwisga, S.; Williams, J. P. Stapper, L. M.; Hogerheijde, M. R.; van Dishoeck, E. F.; Lin, L.; Ahmadi, A.; Booth, A. S.; Grant, S. L.;	Context. Herbig disks are prime sites for the formation of massive exoplanets and looking into the precursors of these disks can offer clues for determining planet formation timescales. The precursors of Herbig stars, called intermediate-mass T Tauri (IMTT) stars, have spectral types later than F, but stellar masses between 1.5 and 5 M<SUB>⊙</SUB>. These stars will eventually become Herbig stars of spectral types A and B. Aims. The aim of this work is to obtain the dust and gas masses and radii of all IMTT disks with ALMA archival data. The obtained disk masses are then compared to Herbig disks and T Tauri disks and the obtained disks sizes to those of Herbig disks. Methods. ALMA Band 6 and 7 archival data were obtained for 34 IMTT disks with continuum observations, 32 of which have at least <SUP>12</SUP>CO, <SUP>13</SUP>CO, or C<SUP>18</SUP>O observations, but with most of them at quite shallow integrations. The disk integrated flux together with a stellar luminosity-scaled disk temperature were used to obta	2018	We propose to survey the gas and dust in 98 protoplanetary disks in the nearby Lupus star-forming region. This is a complete sample of all known optically visible stars with large infrared excesses and stellar masses > 0.1 solar. We will observe the CO, 13CO and C18O 2-1 lines and have developed models to derive gas masses. We will image with a resolution that corresponds to 20AU in radius while maintaining sensitivity over the entire disk. We expect to detect almost all disks in the continuum and measure sub-Jupiter masses of gas. From the resolved images, we will determine radial profiles of the gas, dust, and gas-to-dust ratio, as well as characterize the prevalence of dust holes and asymmetries. This efficient, large, and complete survey will provide an unbiased view of the gas and dust properties in young planet-forming disks, and is complemented by our VLT optical-infrared spectroscopic survey of the host stars.	LupusIII_a_06_TE	van der Marel, Nienke; Oliveira, Isa; Mathews, Geoffrey; van Dishoeck, Ewine; Manara, Carlo Felice; Ansdell, Megan; Natta, Antonella; Miotello, Anna; Carpenter, John; Alcala', Juan Manuel; Testi, Leonardo; Tazzari, Marco; Guidi, Greta; Hogerheijde, Michiel;	3.7755118236581047	0.15814175477574752	0.71056074	uid://A001/X2fb/X38f	uid://A001/X2fb/X390	uid://A002/Xb5bd46/X64b2	Disk demographics in Lupus	S	TARGET	T	3.7042307812178303	T	2018ApJ...859...21A 2019A&A...623A.150V 2019A&A...624A...7V 2019ApJ...872..112V 2020A&A...638A..38T 2021A&A...649A..19S 2021ApJ...908...46B 2021MNRAS.501.2305Z 2021MNRAS.506.2804T 2022ApJ...931....6L 2023A&A...672L..15Z 2024A&A...682A..55M 2024A&A...682A.149S 2025A&A...693A.286S	Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2015.1.00222.S	ALMA	JAO	ALMA	uid://A001/X2fb/X390.source.LupusIII_89.spw.31	cube	2		LupusIII_89	242.3464583333365	-39.06872222222723	0.007175461252508504	Polygon ICRS 242.347886 -39.065310 242.349404 -39.065958 242.350508 -39.066994 242.351043 -39.068272 242.351070 -39.068947 242.350853 -39.069831 242.350019 -39.071009 242.349404 -39.071487 242.348426 -39.071968 242.346749 -39.072303 242.345030 -39.072134 242.343513 -39.071487 242.342409 -39.070451 242.341874 -39.069172 242.341874 -39.068272 242.342064 -39.067613 242.342557 -39.066800 242.343090 -39.066266 242.344491 -39.065476 242.346168 -39.065142			960	1	2	0.17212287051357575	57593.0288	57639.841145	90.72	90.72	0.0013000953880156348	0.0013007558645299726	1902215.167206959	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X2fb/X390	application/x-votable+xml; content=datalink		2015.1.00222.S	Public	339.6664406724036	9.293307195365811	6	6.834250278718917E-10	1.171875E8	A001:DA59 A002:DA49 A004:DA41 A006:DA61 A007:DV12 A008:DV06 A009:DV18 A014:DV09 A015:DV04 A017:DV22 A023:DA51 A034:DA46 A064:DV13 A065:DV01 A071:DA43 A072:DV05 A073:DA54 A074:DA48 A075:DV24 A076:DA52 A077:DA58 A079:DA64 A080:DV23 A081:DA53 A084:DV07 A085:DA47 A086:DV11 A087:DV10 A088:DA57 A089:DA50 A091:DA63 A092:DV17 A093:DV02 A094:DA45 A095:DV25 A096:DA65 A097:DV03 A098:DV21 A099:DA55 A100:DA56 A101:DA60 A102:DV16 A103:DA62 A104:DV14 A106:DV08 A108:DA54 A109:DA55 A112:DA50 A113:DV15 A114:DA52 A115:DA44 A130:DA64 A134:DA44 A135:DV19 A136:DV04 T701:PM03 T703:PM04 T704:PM01	F	2017-12-18T21:28:28.000	0.17212287051357575	[215.55..217.42GHz,1128.91kHz,3.8mJy/beam@10km/s,234.3uJy/beam@native, XX YY] U [219.50..219.62GHz,141.11kHz,3.8mJy/beam@10km/s,938.6uJy/beam@native, XX YY] U [220.34..220.45GHz,141.11kHz,3.7mJy/beam@10km/s,939uJy/beam@native, XX YY] U [230.48..230.59GHz,121.15kHz,3.7mJy/beam@10km/s,943.3uJy/beam@native, XX YY] U [233.30..235.29GHz,31250.00kHz,3.7mJy/beam@10km/s,233.3uJy/beam@native, XX YY]	230.53411996538225	157.60175986830563	ALMA	ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii Constraining the gas mass of Herbig disks using CO isotopologues Constraining the radial drift of millimeter-sized grains in the protoplanetary disks in Lupus Dynamical Stellar Masses of Pre-main-sequence Stars in Lupus and Taurus Obtained with ALMA Surveys in Comparison with Stellar Evolutionary Models Gas Disk Sizes from CO Line Observations: A Test of Angular Momentum Evolution High-resolution ALMA observations of compact discs in the wide-binary system Sz 65 and Sz 66 Intermediate mass T Tauri disk masses and a comparison to their Herbig disk descendants Measuring the ratio of the gas and dust emission radii of protoplanetary disks in the Lupus star-forming region Multiwavelength continuum sizes of protoplanetary discs: scaling relations and implications for grain growth and radial drift Protoplanetary Disk Rings and Gaps across Ages and Luminosities Spatial segregation of dust grains in transition disks. SPHERE observations of 2MASS J16083070-	Ansdell, M. Braun, Teresa A. M. Long, Feng Miley, J. M. Sanchis, E. Stapper, L. M. Tazzari, M. Trapman, L. Villenave, M. Zagaria, Francesco Zurlo, Alice van Terwisga, S. E. van der Marel, Nienke	Ansdell, M.; Williams, J. P.; Trapman, L.; van Terwisga, S. E.; Facchini, S.; Manara, C. F.; van der Marel, N.; Miotello, A.; Tazzari, M.; Hogerheijde, M.; Guidi, G.; Testi, L.; van Dishoeck, E. F. Braun, Teresa A. M.; Yen, Hsi-Wei; Koch, Patrick M.; Manara, Carlo F.; Miotello, Anna; Testi, Leonardo Long, Feng; Andrews, Sean M.; Rosotti, Giovanni; Harsono, Daniel; Pinilla, Paola; Wilner, David J.; Öberg, Karin I.; Teague, Richard; Trapman, Leon; Tabone, Benoît Miley, J. M.; Carpenter, J.; Booth, R.; Jennings, J.; Haworth, T. J.; Vioque, M.; Andrews, S.; Wilner, D.; Benisty, M.; Huang, J.; Perez, L.; Guzman, V.; Ricci, L.; Isella, A. Sanchis, E.; Testi, L.; Natta, A.; Facchini, S.; Manara, C. F.; Miotello, A.; Ercolano, B.; Henning, Th.; Preibisch, T.; Carpenter, J. M.; de Gregorio-Monsalvo, I.; Jayawardhana, R.; Lopez, C.; Mužić, K.; Pascucci, I.; Santamaría-Miranda, A.; van Terwisga, S.; Williams, J. P. Stapper, L. M.; Hogerheijde, M. R.; van Dishoeck, E. F.; Lin, L.; Ahmadi, A.; Booth, A. S.; Grant, S. L.;	Context. Herbig disks are prime sites for the formation of massive exoplanets and looking into the precursors of these disks can offer clues for determining planet formation timescales. The precursors of Herbig stars, called intermediate-mass T Tauri (IMTT) stars, have spectral types later than F, but stellar masses between 1.5 and 5 M<SUB>⊙</SUB>. These stars will eventually become Herbig stars of spectral types A and B. Aims. The aim of this work is to obtain the dust and gas masses and radii of all IMTT disks with ALMA archival data. The obtained disk masses are then compared to Herbig disks and T Tauri disks and the obtained disks sizes to those of Herbig disks. Methods. ALMA Band 6 and 7 archival data were obtained for 34 IMTT disks with continuum observations, 32 of which have at least <SUP>12</SUP>CO, <SUP>13</SUP>CO, or C<SUP>18</SUP>O observations, but with most of them at quite shallow integrations. The disk integrated flux together with a stellar luminosity-scaled disk temperature were used to obta	2018	We propose to survey the gas and dust in 98 protoplanetary disks in the nearby Lupus star-forming region. This is a complete sample of all known optically visible stars with large infrared excesses and stellar masses > 0.1 solar. We will observe the CO, 13CO and C18O 2-1 lines and have developed models to derive gas masses. We will image with a resolution that corresponds to 20AU in radius while maintaining sensitivity over the entire disk. We expect to detect almost all disks in the continuum and measure sub-Jupiter masses of gas. From the resolved images, we will determine radial profiles of the gas, dust, and gas-to-dust ratio, as well as characterize the prevalence of dust holes and asymmetries. This efficient, large, and complete survey will provide an unbiased view of the gas and dust properties in young planet-forming disks, and is complemented by our VLT optical-infrared spectroscopic survey of the host stars.	LupusIII_a_06_TE	van der Marel, Nienke; Oliveira, Isa; Mathews, Geoffrey; van Dishoeck, Ewine; Manara, Carlo Felice; Ansdell, Megan; Natta, Antonella; Miotello, Anna; Carpenter, John; Alcala', Juan Manuel; Testi, Leonardo; Tazzari, Marco; Guidi, Greta; Hogerheijde, Michiel;	3.682309215844993	0.15814175477574752	0.71056074	uid://A001/X2fb/X38f	uid://A001/X2fb/X390	uid://A002/Xb5bd46/X64b2	Disk demographics in Lupus	S	TARGET	T	3.7042307812178303	T	2018ApJ...859...21A 2019A&A...623A.150V 2019A&A...624A...7V 2019ApJ...872..112V 2020A&A...638A..38T 2021A&A...649A..19S 2021ApJ...908...46B 2021MNRAS.501.2305Z 2021MNRAS.506.2804T 2022ApJ...931....6L 2023A&A...672L..15Z 2024A&A...682A..55M 2024A&A...682A.149S 2025A&A...693A.286S	Disks around low-mass stars;null	Disks and planet formation	jpw	Williams, Jonathan	121.15478515625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.A.00061.S	ALMA	JAO	ALMA	uid://A001/X142c/X98.source.J0538-4405.spw.18	image	2		J0538-4405	84.70983982496699	-44.08581636391016	0.012310946924556069	Polygon ICRS 84.714432 -44.091014 84.711446 -44.091863 84.708234 -44.091863 84.706191 -44.091386 84.704802 -44.090796 84.702604 -44.089114 84.701422 -44.086969 84.701422 -44.084663 84.702605 -44.082518 84.703974 -44.081329 84.705248 -44.080619 84.708234 -44.079770 84.711445 -44.079770 84.714431 -44.080619 84.716086 -44.081602 84.717075 -44.082518 84.718257 -44.084663 84.718409 -44.085816 84.718140 -44.087347 84.716773 -44.089434			128	1	2	4.9980301022903015	58755.39152	58756.312391	1209.6	1209.6	0.0012833368300963076	0.0012943321609787631	7411.618239057106	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X142c/X98	application/x-votable+xml; content=datalink		2018.A.00061.S	Public	250.0827775726156	-31.08967696513065	6	1.7314729826381564E-7	2.0E9	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-07-14T00:00:00.000	4.9980301022903015	[216.86..216.99GHz,70.56kHz,10.3mJy/beam@10km/s,2.5mJy/beam@native, XX YY] U [219.35..219.41GHz,70.56kHz,12.2mJy/beam@10km/s,4.2mJy/beam@native, XX YY] U [220.18..220.25GHz,70.56kHz,14.1mJy/beam@10km/s,4.8mJy/beam@native, XX YY] U [230.28..230.41GHz,70.56kHz,12.4mJy/beam@10km/s,3.1mJy/beam@native, XX YY] U [231.62..233.60GHz,31250.00kHz,9.7mJy/beam@10km/s,605.4uJy/beam@native, XX YY]	232.61164563007728	91.85575281185695	ALMA	LMC<SUP>+</SUP>: Large-scale mapping of [C II] and [O III] in the LMC molecular ridge: I. Dataset and line ratio analyses	Fischer, C.	Fischer, C.; Madden, S. C.; Krabbe, A.; Polles, F. L.; Fadda, D.; Tarantino, E.; Galliano, F.; Chen, C.-H. R.; Abel, N.; Beck, Á.; Belloir, L.; Bigiel, F.; Bolatto, A.; Chevance, M.; Colditz, S.; Fischer, N.; Green, A.; Hughes, A.; Indebetouw, R.; Iserlohe, C.; Kaźmierczak-Barthel, M.; Klein, R.; Lambert-Huyghe, A.; Lebouteiller, V.; Mikheeva, E.; Poglitsch, A.; Ramambason, L.; Reach, W.; Rubio, M.; Vacca, W.; Wong, T.; Zinnecker, H.	Context. The fundamental process of star formation in galaxies involves the intricate interplay between the fueling of star formation via molecular gas and the feedback from recently formed massive stars that can, in turn, hinder the conversion of gas into stars. This process, by which galaxies evolve, is also closely connected to the intrinsic properties of the interstellar medium (ISM), such as structure, density, pressure, and metallicity. Aims. To study the role that different molecular and atomic phases of the ISM play in star formation, and to characterize their physical conditions, we zoom into our nearest neighboring galaxy, the Large Magellanic Cloud (LMC; 50 kpc), the most convenient laboratory in which to study the effects of the lower metal abundance on the properties of the ISM. The LMC offers a view of the ISM and star formation conditions in a low-metallicity (Z ~ 0.5 Z<SUB>⊙</SUB>) environment similar, in that regard, to the epoch of the peak of star formation in the earlier Universe (z ~ 1.5)	2025	The Molecular Ridge is the most salient molecular feature in the Large Magellanic Cloud. It is mostly quiescent except for its norther region, which experiences progressively younger and more embedded star formation activity away from the 30 Doradus nebula. We propose to map a 10'x26' area encompassing all massive star formation in the area using only the ACA. This will allow us to study the broader environment of the star forming clouds, characterize the progression of star formation activity using YSOs and statistical techniques, and create a large catalog of molecular clouds with which to study the effects of feedback in the area.	North_Mo_i_06_7M	Jameson, Katherine; McClure-Griffiths, Naomi; Rubio, Monica; Leroy, Adam; Sandstrom, Karin; Tarantino, Elizabeth; Johnson, Lent; Indebetouw, Remy;	9.7201446993249	0.5683433247054367	1.8	uid://A001/X142c/X97	uid://A001/X142c/X98	uid://A002/Xe191fa/X2850	ACA Mapping of the Star-Forming Northern Tip of the Large Magellanic Cloud Molecular Ridge	S	BANDPASS FLUX WVR	F	30.210103579245587	T	2025A&A...702A.273F	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	bolatto	Bolatto, Alberto	31250.0	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.A.00061.S	ALMA	JAO	ALMA	uid://A001/X142c/X98.source.J0538-4405.spw.16	cube	2		J0538-4405	84.70983982496699	-44.08581636391016	0.012310946924556069	Polygon ICRS 84.714432 -44.091014 84.711446 -44.091863 84.708234 -44.091863 84.706191 -44.091386 84.704802 -44.090796 84.702604 -44.089114 84.701422 -44.086969 84.701422 -44.084663 84.702605 -44.082518 84.703974 -44.081329 84.705248 -44.080619 84.708234 -44.079770 84.711445 -44.079770 84.714431 -44.080619 84.716086 -44.081602 84.717075 -44.082518 84.718257 -44.084663 84.718409 -44.085816 84.718140 -44.087347 84.716773 -44.089434			2048	1	2	4.9980301022903015	58755.39152	58756.312391	1209.6	1209.6	0.0013011307623021855	0.0013018368741070478	3263730.8913470916	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X142c/X98	application/x-votable+xml; content=datalink		2018.A.00061.S	Public	250.0827775726156	-31.08967696513065	6	3.986526959244303E-10	1.25E8	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-07-14T00:00:00.000	4.9980301022903015	[216.86..216.99GHz,70.56kHz,10.3mJy/beam@10km/s,2.5mJy/beam@native, XX YY] U [219.35..219.41GHz,70.56kHz,12.2mJy/beam@10km/s,4.2mJy/beam@native, XX YY] U [220.18..220.25GHz,70.56kHz,14.1mJy/beam@10km/s,4.8mJy/beam@native, XX YY] U [230.28..230.41GHz,70.56kHz,12.4mJy/beam@10km/s,3.1mJy/beam@native, XX YY] U [231.62..233.60GHz,31250.00kHz,9.7mJy/beam@10km/s,605.4uJy/beam@native, XX YY]	230.34668266164994	91.85575281185695	ALMA	LMC<SUP>+</SUP>: Large-scale mapping of [C II] and [O III] in the LMC molecular ridge: I. Dataset and line ratio analyses	Fischer, C.	Fischer, C.; Madden, S. C.; Krabbe, A.; Polles, F. L.; Fadda, D.; Tarantino, E.; Galliano, F.; Chen, C.-H. R.; Abel, N.; Beck, Á.; Belloir, L.; Bigiel, F.; Bolatto, A.; Chevance, M.; Colditz, S.; Fischer, N.; Green, A.; Hughes, A.; Indebetouw, R.; Iserlohe, C.; Kaźmierczak-Barthel, M.; Klein, R.; Lambert-Huyghe, A.; Lebouteiller, V.; Mikheeva, E.; Poglitsch, A.; Ramambason, L.; Reach, W.; Rubio, M.; Vacca, W.; Wong, T.; Zinnecker, H.	Context. The fundamental process of star formation in galaxies involves the intricate interplay between the fueling of star formation via molecular gas and the feedback from recently formed massive stars that can, in turn, hinder the conversion of gas into stars. This process, by which galaxies evolve, is also closely connected to the intrinsic properties of the interstellar medium (ISM), such as structure, density, pressure, and metallicity. Aims. To study the role that different molecular and atomic phases of the ISM play in star formation, and to characterize their physical conditions, we zoom into our nearest neighboring galaxy, the Large Magellanic Cloud (LMC; 50 kpc), the most convenient laboratory in which to study the effects of the lower metal abundance on the properties of the ISM. The LMC offers a view of the ISM and star formation conditions in a low-metallicity (Z ~ 0.5 Z<SUB>⊙</SUB>) environment similar, in that regard, to the epoch of the peak of star formation in the earlier Universe (z ~ 1.5)	2025	The Molecular Ridge is the most salient molecular feature in the Large Magellanic Cloud. It is mostly quiescent except for its norther region, which experiences progressively younger and more embedded star formation activity away from the 30 Doradus nebula. We propose to map a 10'x26' area encompassing all massive star formation in the area using only the ACA. This will allow us to study the broader environment of the star forming clouds, characterize the progression of star formation activity using YSOs and statistical techniques, and create a large catalog of molecular clouds with which to study the effects of feedback in the area.	North_Mo_i_06_7M	Jameson, Katherine; McClure-Griffiths, Naomi; Rubio, Monica; Leroy, Adam; Sandstrom, Karin; Tarantino, Elizabeth; Johnson, Lent; Indebetouw, Remy;	12.389634890656792	0.5683433247054367	1.8	uid://A001/X142c/X97	uid://A001/X142c/X98	uid://A002/Xe191fa/X2850	ACA Mapping of the Star-Forming Northern Tip of the Large Magellanic Cloud Molecular Ridge	S	BANDPASS FLUX WVR	F	30.210103579245587	T	2025A&A...702A.273F	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	bolatto	Bolatto, Alberto	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.A.00061.S	ALMA	JAO	ALMA	uid://A001/X142c/X98.source.J0538-4405.spw.22	cube	2		J0538-4405	84.70983982496699	-44.08581636391016	0.012310946924556069	Polygon ICRS 84.714432 -44.091014 84.711446 -44.091863 84.708234 -44.091863 84.706191 -44.091386 84.704802 -44.090796 84.702604 -44.089114 84.701422 -44.086969 84.701422 -44.084663 84.702605 -44.082518 84.703974 -44.081329 84.705248 -44.080619 84.708234 -44.079770 84.711445 -44.079770 84.714431 -44.080619 84.716086 -44.081602 84.717075 -44.082518 84.718257 -44.084663 84.718409 -44.085816 84.718140 -44.087347 84.716773 -44.089434			1024	1	2	4.9980301022903015	58755.39152	58756.312391	1209.6	1209.6	0.0013663613211546688	0.0013667504469977753	3109605.512886884	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X142c/X98	application/x-votable+xml; content=datalink		2018.A.00061.S	Public	250.0827775726156	-31.08967696513065	6	4.3951325377493656E-10	6.25E7	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-07-14T00:00:00.000	4.9980301022903015	[216.86..216.99GHz,70.56kHz,10.3mJy/beam@10km/s,2.5mJy/beam@native, XX YY] U [219.35..219.41GHz,70.56kHz,12.2mJy/beam@10km/s,4.2mJy/beam@native, XX YY] U [220.18..220.25GHz,70.56kHz,14.1mJy/beam@10km/s,4.8mJy/beam@native, XX YY] U [230.28..230.41GHz,70.56kHz,12.4mJy/beam@10km/s,3.1mJy/beam@native, XX YY] U [231.62..233.60GHz,31250.00kHz,9.7mJy/beam@10km/s,605.4uJy/beam@native, XX YY]	219.37812245388886	91.85575281185695	ALMA	LMC<SUP>+</SUP>: Large-scale mapping of [C II] and [O III] in the LMC molecular ridge: I. Dataset and line ratio analyses	Fischer, C.	Fischer, C.; Madden, S. C.; Krabbe, A.; Polles, F. L.; Fadda, D.; Tarantino, E.; Galliano, F.; Chen, C.-H. R.; Abel, N.; Beck, Á.; Belloir, L.; Bigiel, F.; Bolatto, A.; Chevance, M.; Colditz, S.; Fischer, N.; Green, A.; Hughes, A.; Indebetouw, R.; Iserlohe, C.; Kaźmierczak-Barthel, M.; Klein, R.; Lambert-Huyghe, A.; Lebouteiller, V.; Mikheeva, E.; Poglitsch, A.; Ramambason, L.; Reach, W.; Rubio, M.; Vacca, W.; Wong, T.; Zinnecker, H.	Context. The fundamental process of star formation in galaxies involves the intricate interplay between the fueling of star formation via molecular gas and the feedback from recently formed massive stars that can, in turn, hinder the conversion of gas into stars. This process, by which galaxies evolve, is also closely connected to the intrinsic properties of the interstellar medium (ISM), such as structure, density, pressure, and metallicity. Aims. To study the role that different molecular and atomic phases of the ISM play in star formation, and to characterize their physical conditions, we zoom into our nearest neighboring galaxy, the Large Magellanic Cloud (LMC; 50 kpc), the most convenient laboratory in which to study the effects of the lower metal abundance on the properties of the ISM. The LMC offers a view of the ISM and star formation conditions in a low-metallicity (Z ~ 0.5 Z<SUB>⊙</SUB>) environment similar, in that regard, to the epoch of the peak of star formation in the earlier Universe (z ~ 1.5)	2025	The Molecular Ridge is the most salient molecular feature in the Large Magellanic Cloud. It is mostly quiescent except for its norther region, which experiences progressively younger and more embedded star formation activity away from the 30 Doradus nebula. We propose to map a 10'x26' area encompassing all massive star formation in the area using only the ACA. This will allow us to study the broader environment of the star forming clouds, characterize the progression of star formation activity using YSOs and statistical techniques, and create a large catalog of molecular clouds with which to study the effects of feedback in the area.	North_Mo_i_06_7M	Jameson, Katherine; McClure-Griffiths, Naomi; Rubio, Monica; Leroy, Adam; Sandstrom, Karin; Tarantino, Elizabeth; Johnson, Lent; Indebetouw, Remy;	12.243197250259296	0.5683433247054367	1.8	uid://A001/X142c/X97	uid://A001/X142c/X98	uid://A002/Xe191fa/X2850	ACA Mapping of the Star-Forming Northern Tip of the Large Magellanic Cloud Molecular Ridge	S	BANDPASS FLUX WVR	F	30.210103579245587	T	2025A&A...702A.273F	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	bolatto	Bolatto, Alberto	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.A.00061.S	ALMA	JAO	ALMA	uid://A001/X142c/X98.source.J0538-4405.spw.24	cube	2		J0538-4405	84.70983982496699	-44.08581636391016	0.012310946924556069	Polygon ICRS 84.714432 -44.091014 84.711446 -44.091863 84.708234 -44.091863 84.706191 -44.091386 84.704802 -44.090796 84.702604 -44.089114 84.701422 -44.086969 84.701422 -44.084663 84.702605 -44.082518 84.703974 -44.081329 84.705248 -44.080619 84.708234 -44.079770 84.711445 -44.079770 84.714431 -44.080619 84.716086 -44.081602 84.717075 -44.082518 84.718257 -44.084663 84.718409 -44.085816 84.718140 -44.087347 84.716773 -44.089434			1024	1	2	4.9980301022903015	58755.39152	58756.312391	1209.6	1209.6	0.0013611646131117467	0.001361550785946265	3121477.4852052233	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X142c/X98	application/x-votable+xml; content=datalink		2018.A.00061.S	Public	250.0827775726156	-31.08967696513065	6	4.3617592128415257E-10	6.25E7	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-07-14T00:00:00.000	4.9980301022903015	[216.86..216.99GHz,70.56kHz,10.3mJy/beam@10km/s,2.5mJy/beam@native, XX YY] U [219.35..219.41GHz,70.56kHz,12.2mJy/beam@10km/s,4.2mJy/beam@native, XX YY] U [220.18..220.25GHz,70.56kHz,14.1mJy/beam@10km/s,4.8mJy/beam@native, XX YY] U [230.28..230.41GHz,70.56kHz,12.4mJy/beam@10km/s,3.1mJy/beam@native, XX YY] U [231.62..233.60GHz,31250.00kHz,9.7mJy/beam@10km/s,605.4uJy/beam@native, XX YY]	220.21579202481905	91.85575281185695	ALMA	LMC<SUP>+</SUP>: Large-scale mapping of [C II] and [O III] in the LMC molecular ridge: I. Dataset and line ratio analyses	Fischer, C.	Fischer, C.; Madden, S. C.; Krabbe, A.; Polles, F. L.; Fadda, D.; Tarantino, E.; Galliano, F.; Chen, C.-H. R.; Abel, N.; Beck, Á.; Belloir, L.; Bigiel, F.; Bolatto, A.; Chevance, M.; Colditz, S.; Fischer, N.; Green, A.; Hughes, A.; Indebetouw, R.; Iserlohe, C.; Kaźmierczak-Barthel, M.; Klein, R.; Lambert-Huyghe, A.; Lebouteiller, V.; Mikheeva, E.; Poglitsch, A.; Ramambason, L.; Reach, W.; Rubio, M.; Vacca, W.; Wong, T.; Zinnecker, H.	Context. The fundamental process of star formation in galaxies involves the intricate interplay between the fueling of star formation via molecular gas and the feedback from recently formed massive stars that can, in turn, hinder the conversion of gas into stars. This process, by which galaxies evolve, is also closely connected to the intrinsic properties of the interstellar medium (ISM), such as structure, density, pressure, and metallicity. Aims. To study the role that different molecular and atomic phases of the ISM play in star formation, and to characterize their physical conditions, we zoom into our nearest neighboring galaxy, the Large Magellanic Cloud (LMC; 50 kpc), the most convenient laboratory in which to study the effects of the lower metal abundance on the properties of the ISM. The LMC offers a view of the ISM and star formation conditions in a low-metallicity (Z ~ 0.5 Z<SUB>⊙</SUB>) environment similar, in that regard, to the epoch of the peak of star formation in the earlier Universe (z ~ 1.5)	2025	The Molecular Ridge is the most salient molecular feature in the Large Magellanic Cloud. It is mostly quiescent except for its norther region, which experiences progressively younger and more embedded star formation activity away from the 30 Doradus nebula. We propose to map a 10'x26' area encompassing all massive star formation in the area using only the ACA. This will allow us to study the broader environment of the star forming clouds, characterize the progression of star formation activity using YSOs and statistical techniques, and create a large catalog of molecular clouds with which to study the effects of feedback in the area.	North_Mo_i_06_7M	Jameson, Katherine; McClure-Griffiths, Naomi; Rubio, Monica; Leroy, Adam; Sandstrom, Karin; Tarantino, Elizabeth; Johnson, Lent; Indebetouw, Remy;	14.097584169414114	0.5683433247054367	1.8	uid://A001/X142c/X97	uid://A001/X142c/X98	uid://A002/Xe191fa/X2850	ACA Mapping of the Star-Forming Northern Tip of the Large Magellanic Cloud Molecular Ridge	S	BANDPASS FLUX WVR	F	30.210103579245587	T	2025A&A...702A.273F	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	bolatto	Bolatto, Alberto	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2018.A.00061.S	ALMA	JAO	ALMA	uid://A001/X142c/X98.source.J0538-4405.spw.20	cube	2		J0538-4405	84.70983982496699	-44.08581636391016	0.012310946924556069	Polygon ICRS 84.714432 -44.091014 84.711446 -44.091863 84.708234 -44.091863 84.706191 -44.091386 84.704802 -44.090796 84.702604 -44.089114 84.701422 -44.086969 84.701422 -44.084663 84.702605 -44.082518 84.703974 -44.081329 84.705248 -44.080619 84.708234 -44.079770 84.711445 -44.079770 84.714431 -44.080619 84.716086 -44.081602 84.717075 -44.082518 84.718257 -44.084663 84.718409 -44.085816 84.718140 -44.087347 84.716773 -44.089434			2048	1	2	4.9980301022903015	58755.39152	58756.312391	1209.6	1209.6	0.001381612318656111	0.0013824084939773084	3075279.959162719	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X142c/X98	application/x-votable+xml; content=datalink		2018.A.00061.S	Public	250.0827775726156	-31.08967696513065	6	4.4951043945264826E-10	1.25E8	J501:CM10 J502:CM02 J503:CM03 J504:CM12 J505:CM08 J506:CM05 N601:CM07 N602:CM01 N604:CM11 N605:CM04 N606:CM06	F	2021-07-14T00:00:00.000	4.9980301022903015	[216.86..216.99GHz,70.56kHz,10.3mJy/beam@10km/s,2.5mJy/beam@native, XX YY] U [219.35..219.41GHz,70.56kHz,12.2mJy/beam@10km/s,4.2mJy/beam@native, XX YY] U [220.18..220.25GHz,70.56kHz,14.1mJy/beam@10km/s,4.8mJy/beam@native, XX YY] U [230.28..230.41GHz,70.56kHz,12.4mJy/beam@10km/s,3.1mJy/beam@native, XX YY] U [231.62..233.60GHz,31250.00kHz,9.7mJy/beam@10km/s,605.4uJy/beam@native, XX YY]	216.92490990249868	91.85575281185695	ALMA	LMC<SUP>+</SUP>: Large-scale mapping of [C II] and [O III] in the LMC molecular ridge: I. Dataset and line ratio analyses	Fischer, C.	Fischer, C.; Madden, S. C.; Krabbe, A.; Polles, F. L.; Fadda, D.; Tarantino, E.; Galliano, F.; Chen, C.-H. R.; Abel, N.; Beck, Á.; Belloir, L.; Bigiel, F.; Bolatto, A.; Chevance, M.; Colditz, S.; Fischer, N.; Green, A.; Hughes, A.; Indebetouw, R.; Iserlohe, C.; Kaźmierczak-Barthel, M.; Klein, R.; Lambert-Huyghe, A.; Lebouteiller, V.; Mikheeva, E.; Poglitsch, A.; Ramambason, L.; Reach, W.; Rubio, M.; Vacca, W.; Wong, T.; Zinnecker, H.	Context. The fundamental process of star formation in galaxies involves the intricate interplay between the fueling of star formation via molecular gas and the feedback from recently formed massive stars that can, in turn, hinder the conversion of gas into stars. This process, by which galaxies evolve, is also closely connected to the intrinsic properties of the interstellar medium (ISM), such as structure, density, pressure, and metallicity. Aims. To study the role that different molecular and atomic phases of the ISM play in star formation, and to characterize their physical conditions, we zoom into our nearest neighboring galaxy, the Large Magellanic Cloud (LMC; 50 kpc), the most convenient laboratory in which to study the effects of the lower metal abundance on the properties of the ISM. The LMC offers a view of the ISM and star formation conditions in a low-metallicity (Z ~ 0.5 Z<SUB>⊙</SUB>) environment similar, in that regard, to the epoch of the peak of star formation in the earlier Universe (z ~ 1.5)	2025	The Molecular Ridge is the most salient molecular feature in the Large Magellanic Cloud. It is mostly quiescent except for its norther region, which experiences progressively younger and more embedded star formation activity away from the 30 Doradus nebula. We propose to map a 10'x26' area encompassing all massive star formation in the area using only the ACA. This will allow us to study the broader environment of the star forming clouds, characterize the progression of star formation activity using YSOs and statistical techniques, and create a large catalog of molecular clouds with which to study the effects of feedback in the area.	North_Mo_i_06_7M	Jameson, Katherine; McClure-Griffiths, Naomi; Rubio, Monica; Leroy, Adam; Sandstrom, Karin; Tarantino, Elizabeth; Johnson, Lent; Indebetouw, Remy;	10.330264863554197	0.5683433247054367	1.8	uid://A001/X142c/X97	uid://A001/X142c/X98	uid://A002/Xe191fa/X2850	ACA Mapping of the Star-Forming Northern Tip of the Large Magellanic Cloud Molecular Ridge	S	BANDPASS FLUX WVR	F	30.210103579245587	T	2025A&A...702A.273F	Inter-Stellar Medium (ISM)/Molecular clouds;Magellanic Clouds	ISM and star formation	bolatto	Bolatto, Alberto	70.556640625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00869.L	ALMA	JAO	ALMA	uid://A001/X1590/X18a4.source.J1617-5848.spw.25	cube	2		J1617-5848	244.32454692494915	-58.80218339173886	0.01880167238741964	Circle ICRS 244.324547 -58.802183 0.009401			3840	1	2	1.332131670700783	59588.433887	59593.390062	302.4	302.4	0.0035255402593546248	0.00356483006742603	288582.3508368187	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X18a4	application/x-votable+xml; content=datalink		2021.1.00869.L	Public	326.9703934312925	-5.902580661738899	3	1.2353531581029761E-8	9.375E8	A001:DA57 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A015:DV21 A023:DA47 A024:DV06 A025:DV19 A027:DV03 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A040:DA50 A042:DA60 A043:DA55 A045:DA58 A047:DA42 A048:DV10 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A070:DA51 A072:DA53 A073:DA41 A075:DA59 A076:DA48 A082:DV22 A083:DV18 A085:DA56 A086:DV17 A088:DV11 A089:DA52 A090:DV16 A091:DA61 A092:DV13 A094:DV14 T701:PM02 T703:PM01	F	2023-01-27T05:13:05.000	1.332131670700783	[84.10..85.03GHz,294.68kHz,1.7mJy/beam@10km/s,92.8uJy/beam@native, XX YY] U [84.93..85.87GHz,294.68kHz,1.7mJy/beam@10km/s,92.8uJy/beam@native, XX YY] U [86.08..87.01GHz,294.68kHz,1.7mJy/beam@10km/s,94.7uJy/beam@native, XX YY] U [87.02..87.96GHz,294.68kHz,1.7mJy/beam@10km/s,94.7uJy/beam@native, XX YY]	84.56586888011527	1004.2890311338177	ALMA						A radio survey of red giant SiO sources in the inner Galaxy and Bulge is not hindered by extinction. Extremely accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<<1 min) per source. Our aim to collect 20000 SiO maser velocities yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy and Plane. Large samples reveal dynamical structures and minority populations, and their velocity structure may be compared with kinematics of molecular gas, complex orbits in the bar, or stellar streams resulting from recently captured systems. From existing data we collected ~12000 stellar velocities, almost exclusively in the northern Bulge. ALMA is the only instrument that can efficiently add measurements to the undersampled southern Bulge region (-11070% detection rate). We propose to use ALMA to survey 6000 sources in ~120h to obtain 4200+ data points in the undersampled Southern Bulge as part of this larger NSF-	ad3a-191_a_03_TM1	Habing, Harm; Quiroga Nunez, Luis Henry; Stroh, Michael; Lewis, Megan; van Langevelde, Huib; Claussen, Mark; Pihlstrom, Ylva;	1.6917850222976716	0.04686313988524399	4.132136	uid://A001/X1590/X18a3	uid://A001/X1590/X18a4	uid://A002/Xf4f299/X1bbb	Bulge symmetry or not? The hidden dynamics of the Far Side	L	BANDPASS FLUX WVR	F	20.091170703585135	T		Spiral galaxies;Galactic centres/nuclei	Local Universe	lsjouwerman	Sjouwerman, Lorant	294.677734375	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00869.L	ALMA	JAO	ALMA	uid://A001/X1590/X18a4.source.J1617-5848.spw.29	cube	2		J1617-5848	244.32454692494915	-58.80218339173886	0.01880167238741964	Circle ICRS 244.324547 -58.802183 0.009401			3840	1	2	1.332131670700783	59588.433887	59593.390062	302.4	302.4	0.003445377480472902	0.0034828913736259215	295296.72779853386	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X18a4	application/x-votable+xml; content=datalink		2021.1.00869.L	Public	326.9703934312925	-5.902580661738899	3	1.1795147050628479E-8	9.375E8	A001:DA57 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A015:DV21 A023:DA47 A024:DV06 A025:DV19 A027:DV03 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A040:DA50 A042:DA60 A043:DA55 A045:DA58 A047:DA42 A048:DV10 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A070:DA51 A072:DA53 A073:DA41 A075:DA59 A076:DA48 A082:DV22 A083:DV18 A085:DA56 A086:DV17 A088:DV11 A089:DA52 A090:DV16 A091:DA61 A092:DV13 A094:DV14 T701:PM02 T703:PM01	F	2023-01-27T05:13:05.000	1.332131670700783	[84.10..85.03GHz,294.68kHz,1.7mJy/beam@10km/s,92.8uJy/beam@native, XX YY] U [84.93..85.87GHz,294.68kHz,1.7mJy/beam@10km/s,92.8uJy/beam@native, XX YY] U [86.08..87.01GHz,294.68kHz,1.7mJy/beam@10km/s,94.7uJy/beam@native, XX YY] U [87.02..87.96GHz,294.68kHz,1.7mJy/beam@10km/s,94.7uJy/beam@native, XX YY]	86.54434575098986	1004.2890311338177	ALMA						A radio survey of red giant SiO sources in the inner Galaxy and Bulge is not hindered by extinction. Extremely accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<<1 min) per source. Our aim to collect 20000 SiO maser velocities yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy and Plane. Large samples reveal dynamical structures and minority populations, and their velocity structure may be compared with kinematics of molecular gas, complex orbits in the bar, or stellar streams resulting from recently captured systems. From existing data we collected ~12000 stellar velocities, almost exclusively in the northern Bulge. ALMA is the only instrument that can efficiently add measurements to the undersampled southern Bulge region (-11070% detection rate). We propose to use ALMA to survey 6000 sources in ~120h to obtain 4200+ data points in the undersampled Southern Bulge as part of this larger NSF-	ad3a-191_a_03_TM1	Habing, Harm; Quiroga Nunez, Luis Henry; Stroh, Michael; Lewis, Megan; van Langevelde, Huib; Claussen, Mark; Pihlstrom, Ylva;	1.705947757301183	0.04686313988524399	4.132136	uid://A001/X1590/X18a3	uid://A001/X1590/X18a4	uid://A002/Xf4f299/X1bbb	Bulge symmetry or not? The hidden dynamics of the Far Side	L	BANDPASS FLUX WVR	F	20.091170703585135	T		Spiral galaxies;Galactic centres/nuclei	Local Universe	lsjouwerman	Sjouwerman, Lorant	294.677734375	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00869.L	ALMA	JAO	ALMA	uid://A001/X1590/X18a4.source.J1617-5848.spw.31	cube	2		J1617-5848	244.32454692494915	-58.80218339173886	0.01880167238741964	Circle ICRS 244.324547 -58.802183 0.009401			3840	1	2	1.332131670700783	59588.433887	59593.390062	302.4	302.4	0.0034082658396544043	0.003444971623891998	298512.1301798364	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X18a4	application/x-votable+xml; content=datalink		2021.1.00869.L	Public	326.9703934312925	-5.902580661738899	3	1.154106082578669E-8	9.375E8	A001:DA57 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A015:DV21 A023:DA47 A024:DV06 A025:DV19 A027:DV03 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A040:DA50 A042:DA60 A043:DA55 A045:DA58 A047:DA42 A048:DV10 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A070:DA51 A072:DA53 A073:DA41 A075:DA59 A076:DA48 A082:DV22 A083:DV18 A085:DA56 A086:DV17 A088:DV11 A089:DA52 A090:DV16 A091:DA61 A092:DV13 A094:DV14 T701:PM02 T703:PM01	F	2023-01-27T05:13:05.000	1.332131670700783	[84.10..85.03GHz,294.68kHz,1.7mJy/beam@10km/s,92.8uJy/beam@native, XX YY] U [84.93..85.87GHz,294.68kHz,1.7mJy/beam@10km/s,92.8uJy/beam@native, XX YY] U [86.08..87.01GHz,294.68kHz,1.7mJy/beam@10km/s,94.7uJy/beam@native, XX YY] U [87.02..87.96GHz,294.68kHz,1.7mJy/beam@10km/s,94.7uJy/beam@native, XX YY]	87.4918051025031	1004.2890311338177	ALMA						A radio survey of red giant SiO sources in the inner Galaxy and Bulge is not hindered by extinction. Extremely accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<<1 min) per source. Our aim to collect 20000 SiO maser velocities yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy and Plane. Large samples reveal dynamical structures and minority populations, and their velocity structure may be compared with kinematics of molecular gas, complex orbits in the bar, or stellar streams resulting from recently captured systems. From existing data we collected ~12000 stellar velocities, almost exclusively in the northern Bulge. ALMA is the only instrument that can efficiently add measurements to the undersampled southern Bulge region (-11070% detection rate). We propose to use ALMA to survey 6000 sources in ~120h to obtain 4200+ data points in the undersampled Southern Bulge as part of this larger NSF-	ad3a-191_a_03_TM1	Habing, Harm; Quiroga Nunez, Luis Henry; Stroh, Michael; Lewis, Megan; van Langevelde, Huib; Claussen, Mark; Pihlstrom, Ylva;	1.6969929116307723	0.04686313988524399	4.132136	uid://A001/X1590/X18a3	uid://A001/X1590/X18a4	uid://A002/Xf4f299/X1bbb	Bulge symmetry or not? The hidden dynamics of the Far Side	L	BANDPASS FLUX WVR	F	20.091170703585135	T		Spiral galaxies;Galactic centres/nuclei	Local Universe	lsjouwerman	Sjouwerman, Lorant	294.677734375	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2021.1.00869.L	ALMA	JAO	ALMA	uid://A001/X1590/X18a4.source.J1617-5848.spw.27	cube	2		J1617-5848	244.32454692494915	-58.80218339173886	0.01880167238741964	Circle ICRS 244.324547 -58.802183 0.009401			3840	1	2	1.332131670700783	59588.433887	59593.390062	302.4	302.4	0.0034913903304615037	0.0035299185092865664	291405.0277156838	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X1590/X18a4	application/x-votable+xml; content=datalink		2021.1.00869.L	Public	326.9703934312925	-5.902580661738899	3	1.211405952938137E-8	9.375E8	A001:DA57 A007:DV04 A008:DV24 A010:DV15 A011:DV25 A015:DV21 A023:DA47 A024:DV06 A025:DV19 A027:DV03 A033:DV01 A034:DA49 A035:DA63 A036:DV08 A040:DA50 A042:DA60 A043:DA55 A045:DA58 A047:DA42 A048:DV10 A050:DA45 A058:DA64 A060:DV20 A062:DA65 A066:DA62 A068:DA54 A070:DA51 A072:DA53 A073:DA41 A075:DA59 A076:DA48 A082:DV22 A083:DV18 A085:DA56 A086:DV17 A088:DV11 A089:DA52 A090:DV16 A091:DA61 A092:DV13 A094:DV14 T701:PM02 T703:PM01	F	2023-01-27T05:13:05.000	1.332131670700783	[84.10..85.03GHz,294.68kHz,1.7mJy/beam@10km/s,92.8uJy/beam@native, XX YY] U [84.93..85.87GHz,294.68kHz,1.7mJy/beam@10km/s,92.8uJy/beam@native, XX YY] U [86.08..87.01GHz,294.68kHz,1.7mJy/beam@10km/s,94.7uJy/beam@native, XX YY] U [87.02..87.96GHz,294.68kHz,1.7mJy/beam@10km/s,94.7uJy/beam@native, XX YY]	85.39760664977433	1004.2890311338177	ALMA						A radio survey of red giant SiO sources in the inner Galaxy and Bulge is not hindered by extinction. Extremely accurate stellar velocities (<1 km/s) are obtained with minimal observing time (<<1 min) per source. Our aim to collect 20000 SiO maser velocities yields data comparable to optical surveys with the additional strength of a much more thorough coverage of the highly obscured inner Galaxy and Plane. Large samples reveal dynamical structures and minority populations, and their velocity structure may be compared with kinematics of molecular gas, complex orbits in the bar, or stellar streams resulting from recently captured systems. From existing data we collected ~12000 stellar velocities, almost exclusively in the northern Bulge. ALMA is the only instrument that can efficiently add measurements to the undersampled southern Bulge region (-11070% detection rate). We propose to use ALMA to survey 6000 sources in ~120h to obtain 4200+ data points in the undersampled Southern Bulge as part of this larger NSF-	ad3a-191_a_03_TM1	Habing, Harm; Quiroga Nunez, Luis Henry; Stroh, Michael; Lewis, Megan; van Langevelde, Huib; Claussen, Mark; Pihlstrom, Ylva;	1.6837875855031603	0.04686313988524399	4.132136	uid://A001/X1590/X18a3	uid://A001/X1590/X18a4	uid://A002/Xf4f299/X1bbb	Bulge symmetry or not? The hidden dynamics of the Far Side	L	BANDPASS FLUX WVR	F	20.091170703585135	T		Spiral galaxies;Galactic centres/nuclei	Local Universe	lsjouwerman	Sjouwerman, Lorant	294.677734375	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01411.S	ALMA	JAO	ALMA	uid://A001/X3841/X233.source.G19.01-0.03.spw.25	cube	2		G19.01-0.03	276.43657916670657	-12.379430000003413	0.004761764396179007	Polygon ICRS 276.437036 -12.377091 276.437885 -12.377420 276.438551 -12.378031 276.438785 -12.378416 276.438974 -12.378984 276.438974 -12.379876 276.438637 -12.380706 276.438248 -12.381166 276.437885 -12.381440 276.437036 -12.381769 276.436122 -12.381769 276.435273 -12.381440 276.434607 -12.380829 276.434218 -12.380022 276.434146 -12.379579 276.434185 -12.378984 276.434521 -12.378154 276.434911 -12.377694 276.435273 -12.377420 276.436122 -12.377091			1920	1	2	0.46796127769716916	61153.426128	61155.441036	423.36	423.36	8.985346582442685E-4	9.036095329179697E-4	295588.1810818936	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3841/X233	application/x-votable+xml; content=datalink		2025.1.01411.S	Proprietary	19.00862803657853	-0.029303941799007395	7	3.057403876429973E-9	1.875E9	A001:DA63 A002:DA45 A003:DV04 A005:DA54 A006:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A017:DV05 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV14 A027:DV08 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A039:DA58 A043:DV13 A044:DA57 A045:DA65 A047:DA42 A048:DA55 A049:DV11 A050:DV10 A058:DV12 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DV09 A073:DA41 A074:DA61 A075:DA50 A076:DA48 A082:DV22 A083:DA56 A085:DA64 A088:DA46	F	2027-04-28T13:00:35.000	0.46796127769716916	[331.77..333.65GHz,1128.91kHz,2.8mJy/beam@10km/s,217.4uJy/beam@native, XX YY] U [333.72..335.59GHz,1128.91kHz,3.1mJy/beam@10km/s,239.3uJy/beam@native, XX YY] U [343.82..345.70GHz,1128.91kHz,3mJy/beam@10km/s,235.1uJy/beam@native, XX YY] U [345.72..347.59GHz,1128.91kHz,3mJy/beam@10km/s,235.4uJy/beam@native, XX YY]	332.70904385386694	978.8071258099275	ALMA						We propose ALMA observations of 15 high-mass hot cores that will be observed in a newly approved JWST Cycle 4 program using MIRI-MRS. These sources were specifically selected for their rich chemical environments, making them ideal targets to diagnose the physical conditions and investigate the chemical evolution in star-forming regions. The two primary goals of this follow-up proposal are: 1) compare the gas and ice abundances of three simple molecules (H2CO, HCOOH, and HNCO) to trace their evolution from ice to gas (the ice reservoir will be observed with JWST/MIRI); 2) investigate IR pumping effects by jointly analyzing ALMA and JWST spectra of SO2, SiO, CS, and HCN, which are observable at both mm and IR wavelengths from their pure rotational and ro-vibrational transitions, respectively. Our spectral setup is optimized to cover multiple transitions across a wide range of upper energy levels of the aforementioned species and their minor isotopologs, enabling robust constraints on their column densities and	G11.92-0_a_07_TM1	Xu, Fengwei; Beuther, Henrik; Gieser, Caroline; van Dishoeck, Ewine; Francis, Logan; Liu, Tie;	2.8262482192378258	0.11565256325853233	0.9931427	uid://A001/X3841/X232	uid://A001/X3841/X233	uid://A002/X13967c1/X18781	Comparative chemical studies on high-mass protostars with ALMA and JWST	S	TARGET	T	5.250297159256434	T		High-mass star formation;Astrochemistry	ISM and star formation	ssaaercy	Chen, Yuan	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01411.S	ALMA	JAO	ALMA	uid://A001/X3841/X233.source.G19.01-0.03.spw.29	cube	2		G19.01-0.03	276.43657916670657	-12.379430000003413	0.004761764396179007	Polygon ICRS 276.437036 -12.377091 276.437885 -12.377420 276.438551 -12.378031 276.438785 -12.378416 276.438974 -12.378984 276.438974 -12.379876 276.438637 -12.380706 276.438248 -12.381166 276.437885 -12.381440 276.437036 -12.381769 276.436122 -12.381769 276.435273 -12.381440 276.434607 -12.380829 276.434218 -12.380022 276.434146 -12.379579 276.434185 -12.378984 276.434521 -12.378154 276.434911 -12.377694 276.435273 -12.377420 276.436122 -12.377091			1920	1	2	0.46796127769716916	61153.426128	61155.441036	423.36	423.36	8.672120306473332E-4	8.719383346527872E-4	304604.426548456	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3841/X233	application/x-votable+xml; content=datalink		2025.1.01411.S	Proprietary	19.00862803657853	-0.029303941799007395	7	2.8473984245554825E-9	1.875E9	A001:DA63 A002:DA45 A003:DV04 A005:DA54 A006:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A017:DV05 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV14 A027:DV08 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A039:DA58 A043:DV13 A044:DA57 A045:DA65 A047:DA42 A048:DA55 A049:DV11 A050:DV10 A058:DV12 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DV09 A073:DA41 A074:DA61 A075:DA50 A076:DA48 A082:DV22 A083:DA56 A085:DA64 A088:DA46	F	2027-04-28T13:00:35.000	0.46796127769716916	[331.77..333.65GHz,1128.91kHz,2.8mJy/beam@10km/s,217.4uJy/beam@native, XX YY] U [333.72..335.59GHz,1128.91kHz,3.1mJy/beam@10km/s,239.3uJy/beam@native, XX YY] U [343.82..345.70GHz,1128.91kHz,3mJy/beam@10km/s,235.1uJy/beam@native, XX YY] U [345.72..347.59GHz,1128.91kHz,3mJy/beam@10km/s,235.4uJy/beam@native, XX YY]	344.75992192479924	978.8071258099275	ALMA						We propose ALMA observations of 15 high-mass hot cores that will be observed in a newly approved JWST Cycle 4 program using MIRI-MRS. These sources were specifically selected for their rich chemical environments, making them ideal targets to diagnose the physical conditions and investigate the chemical evolution in star-forming regions. The two primary goals of this follow-up proposal are: 1) compare the gas and ice abundances of three simple molecules (H2CO, HCOOH, and HNCO) to trace their evolution from ice to gas (the ice reservoir will be observed with JWST/MIRI); 2) investigate IR pumping effects by jointly analyzing ALMA and JWST spectra of SO2, SiO, CS, and HCN, which are observable at both mm and IR wavelengths from their pure rotational and ro-vibrational transitions, respectively. Our spectral setup is optimized to cover multiple transitions across a wide range of upper energy levels of the aforementioned species and their minor isotopologs, enabling robust constraints on their column densities and	G11.92-0_a_07_TM1	Xu, Fengwei; Beuther, Henrik; Gieser, Caroline; van Dishoeck, Ewine; Francis, Logan; Liu, Tie;	3.001378555762502	0.11565256325853233	0.9931427	uid://A001/X3841/X232	uid://A001/X3841/X233	uid://A002/X13967c1/X18781	Comparative chemical studies on high-mass protostars with ALMA and JWST	S	TARGET	T	5.250297159256434	T		High-mass star formation;Astrochemistry	ISM and star formation	ssaaercy	Chen, Yuan	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01411.S	ALMA	JAO	ALMA	uid://A001/X3841/X233.source.G19.01-0.03.spw.31	cube	2		G19.01-0.03	276.43657916670657	-12.379430000003413	0.004761764396179007	Polygon ICRS 276.437036 -12.377091 276.437885 -12.377420 276.438551 -12.378031 276.438785 -12.378416 276.438974 -12.378984 276.438974 -12.379876 276.438637 -12.380706 276.438248 -12.381166 276.437885 -12.381440 276.437036 -12.381769 276.436122 -12.381769 276.435273 -12.381440 276.434607 -12.380829 276.434218 -12.380022 276.434146 -12.379579 276.434185 -12.378984 276.434521 -12.378154 276.434911 -12.377694 276.435273 -12.377420 276.436122 -12.377091			1920	1	2	0.46796127769716916	61153.426128	61155.441036	423.36	423.36	8.624835661157467E-4	8.671583238480573E-4	306283.4853719854	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3841/X233	application/x-votable+xml; content=datalink		2025.1.01411.S	Proprietary	19.00862803657853	-0.029303941799007395	7	2.8163485408693306E-9	1.875E9	A001:DA63 A002:DA45 A003:DV04 A005:DA54 A006:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A017:DV05 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV14 A027:DV08 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A039:DA58 A043:DV13 A044:DA57 A045:DA65 A047:DA42 A048:DA55 A049:DV11 A050:DV10 A058:DV12 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DV09 A073:DA41 A074:DA61 A075:DA50 A076:DA48 A082:DV22 A083:DA56 A085:DA64 A088:DA46	F	2027-04-28T13:00:35.000	0.46796127769716916	[331.77..333.65GHz,1128.91kHz,2.8mJy/beam@10km/s,217.4uJy/beam@native, XX YY] U [333.72..335.59GHz,1128.91kHz,3.1mJy/beam@10km/s,239.3uJy/beam@native, XX YY] U [343.82..345.70GHz,1128.91kHz,3mJy/beam@10km/s,235.1uJy/beam@native, XX YY] U [345.72..347.59GHz,1128.91kHz,3mJy/beam@10km/s,235.4uJy/beam@native, XX YY]	346.65516563500955	978.8071258099275	ALMA						We propose ALMA observations of 15 high-mass hot cores that will be observed in a newly approved JWST Cycle 4 program using MIRI-MRS. These sources were specifically selected for their rich chemical environments, making them ideal targets to diagnose the physical conditions and investigate the chemical evolution in star-forming regions. The two primary goals of this follow-up proposal are: 1) compare the gas and ice abundances of three simple molecules (H2CO, HCOOH, and HNCO) to trace their evolution from ice to gas (the ice reservoir will be observed with JWST/MIRI); 2) investigate IR pumping effects by jointly analyzing ALMA and JWST spectra of SO2, SiO, CS, and HCN, which are observable at both mm and IR wavelengths from their pure rotational and ro-vibrational transitions, respectively. Our spectral setup is optimized to cover multiple transitions across a wide range of upper energy levels of the aforementioned species and their minor isotopologs, enabling robust constraints on their column densities and	G11.92-0_a_07_TM1	Xu, Fengwei; Beuther, Henrik; Gieser, Caroline; van Dishoeck, Ewine; Francis, Logan; Liu, Tie;	2.9974729727420275	0.11565256325853233	0.9931427	uid://A001/X3841/X232	uid://A001/X3841/X233	uid://A002/X13967c1/X18781	Comparative chemical studies on high-mass protostars with ALMA and JWST	S	TARGET	T	5.250297159256434	T		High-mass star formation;Astrochemistry	ISM and star formation	ssaaercy	Chen, Yuan	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2025.1.01411.S	ALMA	JAO	ALMA	uid://A001/X3841/X233.source.G19.01-0.03.spw.27	cube	2		G19.01-0.03	276.43657916670657	-12.379430000003413	0.004761764396179007	Polygon ICRS 276.437036 -12.377091 276.437885 -12.377420 276.438551 -12.378031 276.438785 -12.378416 276.438974 -12.378984 276.438974 -12.379876 276.438637 -12.380706 276.438248 -12.381166 276.437885 -12.381440 276.437036 -12.381769 276.436122 -12.381769 276.435273 -12.381440 276.434607 -12.380829 276.434218 -12.380022 276.434146 -12.379579 276.434185 -12.378984 276.434521 -12.378154 276.434911 -12.377694 276.435273 -12.377420 276.436122 -12.377091			1920	1	2	0.46796127769716916	61153.426128	61155.441036	423.36	423.36	8.93319647615199E-4	8.98335674716242E-4	297313.7621885944	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X3841/X233	application/x-votable+xml; content=datalink		2025.1.01411.S	Proprietary	19.00862803657853	-0.029303941799007395	7	3.0219182201649487E-9	1.875E9	A001:DA63 A002:DA45 A003:DV04 A005:DA54 A006:DA43 A007:DV20 A008:DV17 A010:DV06 A011:DV01 A015:DA52 A016:DA44 A017:DV05 A022:DA47 A023:DA60 A024:DV02 A025:DV19 A026:DV14 A027:DV08 A033:DV25 A034:DV15 A035:DA51 A036:DV16 A039:DA58 A043:DV13 A044:DA57 A045:DA65 A047:DA42 A048:DA55 A049:DV11 A050:DV10 A058:DV12 A060:DV23 A062:DA53 A066:DA49 A068:DV21 A069:DA62 A070:DV18 A072:DV09 A073:DA41 A074:DA61 A075:DA50 A076:DA48 A082:DV22 A083:DA56 A085:DA64 A088:DA46	F	2027-04-28T13:00:35.000	0.46796127769716916	[331.77..333.65GHz,1128.91kHz,2.8mJy/beam@10km/s,217.4uJy/beam@native, XX YY] U [333.72..335.59GHz,1128.91kHz,3.1mJy/beam@10km/s,239.3uJy/beam@native, XX YY] U [343.82..345.70GHz,1128.91kHz,3mJy/beam@10km/s,235.1uJy/beam@native, XX YY] U [345.72..347.59GHz,1128.91kHz,3mJy/beam@10km/s,235.4uJy/beam@native, XX YY]	334.65678815016474	978.8071258099275	ALMA						We propose ALMA observations of 15 high-mass hot cores that will be observed in a newly approved JWST Cycle 4 program using MIRI-MRS. These sources were specifically selected for their rich chemical environments, making them ideal targets to diagnose the physical conditions and investigate the chemical evolution in star-forming regions. The two primary goals of this follow-up proposal are: 1) compare the gas and ice abundances of three simple molecules (H2CO, HCOOH, and HNCO) to trace their evolution from ice to gas (the ice reservoir will be observed with JWST/MIRI); 2) investigate IR pumping effects by jointly analyzing ALMA and JWST spectra of SO2, SiO, CS, and HCN, which are observable at both mm and IR wavelengths from their pure rotational and ro-vibrational transitions, respectively. Our spectral setup is optimized to cover multiple transitions across a wide range of upper energy levels of the aforementioned species and their minor isotopologs, enabling robust constraints on their column densities and	G11.92-0_a_07_TM1	Xu, Fengwei; Beuther, Henrik; Gieser, Caroline; van Dishoeck, Ewine; Francis, Logan; Liu, Tie;	3.101139495695215	0.11565256325853233	0.9931427	uid://A001/X3841/X232	uid://A001/X3841/X233	uid://A002/X13967c1/X18781	Comparative chemical studies on high-mass protostars with ALMA and JWST	S	TARGET	T	5.250297159256434	T		High-mass star formation;Astrochemistry	ISM and star formation	ssaaercy	Chen, Yuan	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.1.01036.S	ALMA	JAO	ALMA	uid://A001/X88e/Xfe.source.G11.1-0.12.spw.25	cube	2		G11.1-0.12	272.617784583385	-19.37525555556819	0.007152277190130827	Polygon ICRS 272.621390 -19.374150 272.621568 -19.375480 272.621215 -19.376778 272.620380 -19.377862 272.619611 -19.378389 272.618956 -19.378657 272.618260 -19.378803 272.617309 -19.378803 272.615958 -19.378389 272.614864 -19.377535 272.614179 -19.376361 272.614001 -19.375031 272.614355 -19.373733 272.614718 -19.373154 272.615368 -19.372500 272.616613 -19.371854 272.617547 -19.371686 272.618260 -19.371708 272.619611 -19.372122 272.620705 -19.372976			1920	1	2	0.04128075130196105	58007.094777	58692.220904	689.472	689.472	0.001273342260554134	0.0012835622459238197	206891.59978434377	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X88e/Xfe	application/x-votable+xml; content=datalink		2016.1.01036.S	Public	11.10894801097218	-0.1143484859888878	6	6.154591914882967E-9	1.875E9	A001:DA59 A007:DV09 A015:DA61 A042:DV05 A058:DA41 A065:DA64 A069:DA55 A071:DA52 A074:DA47 A074:DV09 A075:DA56 A078:DV08 A082:DA60 A083:DA51 A084:DV04 A086:DV22 A087:DV25 A088:DV11 A089:DV16 A090:DV13 A090:DV24 A091:DA45 A091:DA61 A092:DV04 A092:DV14 A093:DV03 A093:DV20 A094:DV14 A094:DV19 A096:DA50 A101:DA62 A102:DV03 A104:DA58 A105:DA64 A105:DV02 A108:DA50 A110:DA41 A110:DA55 A111:DV12 A111:PM02 A115:DA43 A116:DV07 A116:DV08 A118:DV01 A118:DV07 A120:DA44 A120:DV19 A121:PM03 A122:DV11 A123:DA42 A124:DA42 A124:DA51 A125:DA49 A125:DA53 A126:DV10 A126:PM01 A127:DA49 A127:DV24 A128:DV15 A129:DA46 A129:DV01 A130:DA58 A130:DV15 A131:DV21 A131:PM03 A132:DA57 A132:DV23 A133:DV10 A133:PM04 A134:DA63 A135:DA57 A135:PM02 P401:DA59 P401:DA65 P403:DA45 P404:DV16 P410:DV06 S301:DA54 S301:DA60 S306:DV20 S307:DA47 W207:DV17 W207:DV25 W209:DA48 W210:DA53 W210:DV22	F	2019-03-01T20:36:27.000	0.04128075130196105	[216.86..218.74GHz,1052.73kHz,1.2mJy/beam@10km/s,76.8uJy/beam@native, XX YY] U [219.06..220.94GHz,976.56kHz,1.2mJy/beam@10km/s,76.6uJy/beam@native, XX YY] U [231.06..232.94GHz,1128.91kHz,1.2mJy/beam@10km/s,76.4uJy/beam@native, XX YY] U [233.56..235.44GHz,1128.91kHz,1.2mJy/beam@10km/s,76.5uJy/beam@native, XX YY]	234.50015191389144	1325.1195201894923	ALMA	Digging Into the Interior of Hot Cores with ALMA (DIHCA). V. Deuterium Fractionation of Methanol Digging into the Interior of Hot Cores with ALMA (DIHCA). I. Dissecting the High-mass Star-forming Core G335.579-0.292 MM1 Digging into the Interior of Hot Cores with ALMA (DIHCA). II. Exploring the Inner Binary (Multiple) System Embedded in G335 MM1 ALMA1 Digging into the Interior of Hot Cores with ALMA (DIHCA). IV. Fragmentation in High-mass Star-forming Clumps Digging into the Interior of Hot Cores with ALMA (DIHCA). VI. The Formation of Low-mass Multiple Systems in High-mass Cluster-forming Regions Digging into the Interior of Hot Cores with ALMA (DIHCA). VII. Disk Candidates around High-mass Stars and Evidence of Anisotropic Infall Digging into the Interior of Hot Cores with the ALMA (DIHCA). III. The Chemical Link between NH<SUB>2</SUB>CHO, HNCO, and H<SUB>2</SUB>CO Hierarchical accretion flow from the G351 infrared dark filament to its central cores Magnetic Fields in Massive Star-forming Regions (MagMaR).	Beuther, H. Ginsburg, Adam Ishihara, Kousuke Li, Shanghuo Luo, Qiu-yi Olguin, Fernando A. Sakai, Takeshi Sanhueza, Patricio Taniguchi, Kotomi	Beuther, H.; Olguin, F. A.; Sanhueza, P.; Cunningham, N.; Ginsburg, A. Ginsburg, Adam; McGuire, Brett A.; Sanhueza, Patricio; Olguin, Fernando; Maud, Luke T.; Tanaka, Kei E. I.; Zhang, Yichen; Beuther, Henrik; Indriolo, Nick Ishihara, Kousuke; Sanhueza, Patricio; Nakamura, Fumitaka; Saito, Masao; Chen, Huei-Ru Vivien; Li, Shanghuo; Olguin, Fernando; Taniguchi, Kotomi; Morii, Kaho; Lu, Xing; Luo, Qiu-yi; Sakai, Takeshi; Zhang, Qizhou Li, Shanghuo; Sanhueza, Patricio; Beuther, Henrik; Chen, Huei-Ru Vivien; Kuiper, Rolf; Olguin, Fernando A.; Pudritz, Ralph E.; Stephens, Ian W.; Zhang, Qizhou; Nakamura, Fumitaka; Lu, Xing; Kuruwita, Rajika L.; Sakai, Takeshi; Henning, Thomas; Taniguchi, Kotomi; Li, Fei Luo, Qiu-yi; Sanhueza, Patricio; Offner, Stella S. R.; Olguin, Fernando; Ginsburg, Adam; Nakamura, Fumitaka; Morii, Kaho; Cheng, Yu; Tanaka, Kei E. I.; Liu, Junhao; Liu, Tie; Lu, Xing; Zhang, Qizhou; Taniguchi, Kotomi; Saha, Piyali; Li, Shanghuo; Mai, Xiaofeng Olguin, Fernando A.; Sanhueza, Patricio; Ginsburg, Adam	A complete understanding of the initial conditions of high-mass star formation and what processes determine multiplicity requires the study of the magnetic field in young massive cores. Using Atacama Large Millimeter/submillimeter Array (ALMA) 250 GHz polarization observations (0<inline-formula> </inline-formula>3 = 1000 au) and ALMA 220 GHz high-angular-resolution observations (0<inline-formula> </inline-formula>05 = 160 au), we have performed a full energy analysis including the magnetic field at core scales and have assessed what influences the multiplicity inside a massive core previously believed to be in the prestellar phase. With a mass of 31 M<SUB>⊙</SUB>, the G11.92 MM2 core has a young CS molecular outflow with a dynamical timescale of a few thousand years. At high resolution, the MM2 core fragments into a binary system, with a projected separation of 505 au and a binary mass ratio of 1.14. Using the Davis–Chandrasekhar–Fermi method with an angle dispersion function analysis, we estimate in this cor	2021	Different mechanisms have been suggested to explain the binarity of high-mass stars: core fragmentation, disk fragmentation, and multiple-body interactions. However, so far there is no observational constraints to assess their importance. With the unique capabilities of ALMA, we can for the first time statistically test these scenarios. We will observe continuum emission at 230 GHz to derive the multiplicity fraction and the distribution of companions separation. With a resolution of 0.06" (~100 pc at 2 kpc; ~200 pc at 3.8 kpc), we can resolved star-forming cores and the predicted disks (~1,000 AU) around high-mass stars. We have selected a large, uniform sample of 32 cores containing massive young stellar objects (MYSOs) embedded in 20 high-mass star-forming regions. With these observations, we will address: What is the binarity rate of high-mass cores at ~100s AU scales? How does the binarity rate of high-mass cores change as they evolve? Are high-mass binary systems formed at core scales (~1,000 AU) or dis	IRAS_181_b_06_TM1	Zhang, Qizhou; Hoq, Sadia; Jackson, James; Sakai, Takeshi; Nakamura, Fumitaka; Silva, Andrea; Ohashi, Satoshi; Contreras, Yanett; Chen, Vivien; Tatematsu, Ken'ichi; Miura, Rie;	1.1836438528558468	0.038286019057210165	0.502383	uid://A001/X88e/Xfd	uid://A001/X88e/Xfe	uid://A002/Xc46ab2/Xbbc	The formation of high-mass binary systems by core/disk fragmentation	S	TARGET	T	1.0389026303750921	F	2021ApJ...909..199O 2022ApJ...929...68O 2023ApJ...942...66G 2023ApJ...950...57T 2024ApJ...974...95I 2024NatAs...8..472L 2025A&A...695A..51B 2025ApJ...980...87S 2025ApJ...983...37S 2026ApJ...999..106O 2026ApJ...999..192L	High-mass star formation;null	ISM and star formation	psanhueza	Sanhueza, Patricio	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.1.01036.S	ALMA	JAO	ALMA	uid://A001/X88e/Xfe.source.G11.1-0.12.spw.27	cube	2		G11.1-0.12	272.617784583385	-19.37525555556819	0.007152277190130827	Polygon ICRS 272.621390 -19.374150 272.621568 -19.375480 272.621215 -19.376778 272.620380 -19.377862 272.619611 -19.378389 272.618956 -19.378657 272.618260 -19.378803 272.617309 -19.378803 272.615958 -19.378389 272.614864 -19.377535 272.614179 -19.376361 272.614001 -19.375031 272.614355 -19.373733 272.614718 -19.373154 272.615368 -19.372500 272.616613 -19.371854 272.617547 -19.371686 272.618260 -19.371708 272.619611 -19.372122 272.620705 -19.372976			1920	1	2	0.04128075130196105	58007.094777	58692.220904	689.472	689.472	0.001287008425202769	0.001297449828427523	204677.0836106694	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X88e/Xfe	application/x-votable+xml; content=datalink		2016.1.01036.S	Public	11.10894801097218	-0.1143484859888878	6	6.287950836335951E-9	1.875E9	A001:DA59 A007:DV09 A015:DA61 A042:DV05 A058:DA41 A065:DA64 A069:DA55 A071:DA52 A074:DA47 A074:DV09 A075:DA56 A078:DV08 A082:DA60 A083:DA51 A084:DV04 A086:DV22 A087:DV25 A088:DV11 A089:DV16 A090:DV13 A090:DV24 A091:DA45 A091:DA61 A092:DV04 A092:DV14 A093:DV03 A093:DV20 A094:DV14 A094:DV19 A096:DA50 A101:DA62 A102:DV03 A104:DA58 A105:DA64 A105:DV02 A108:DA50 A110:DA41 A110:DA55 A111:DV12 A111:PM02 A115:DA43 A116:DV07 A116:DV08 A118:DV01 A118:DV07 A120:DA44 A120:DV19 A121:PM03 A122:DV11 A123:DA42 A124:DA42 A124:DA51 A125:DA49 A125:DA53 A126:DV10 A126:PM01 A127:DA49 A127:DV24 A128:DV15 A129:DA46 A129:DV01 A130:DA58 A130:DV15 A131:DV21 A131:PM03 A132:DA57 A132:DV23 A133:DV10 A133:PM04 A134:DA63 A135:DA57 A135:PM02 P401:DA59 P401:DA65 P403:DA45 P404:DV16 P410:DV06 S301:DA54 S301:DA60 S306:DV20 S307:DA47 W207:DV17 W207:DV25 W209:DA48 W210:DA53 W210:DV22	F	2019-03-01T20:36:27.000	0.04128075130196105	[216.86..218.74GHz,1052.73kHz,1.2mJy/beam@10km/s,76.8uJy/beam@native, XX YY] U [219.06..220.94GHz,976.56kHz,1.2mJy/beam@10km/s,76.6uJy/beam@native, XX YY] U [231.06..232.94GHz,1128.91kHz,1.2mJy/beam@10km/s,76.4uJy/beam@native, XX YY] U [233.56..235.44GHz,1128.91kHz,1.2mJy/beam@10km/s,76.5uJy/beam@native, XX YY]	232.0001500749202	1325.1195201894923	ALMA	Digging Into the Interior of Hot Cores with ALMA (DIHCA). V. Deuterium Fractionation of Methanol Digging into the Interior of Hot Cores with ALMA (DIHCA). I. Dissecting the High-mass Star-forming Core G335.579-0.292 MM1 Digging into the Interior of Hot Cores with ALMA (DIHCA). II. Exploring the Inner Binary (Multiple) System Embedded in G335 MM1 ALMA1 Digging into the Interior of Hot Cores with ALMA (DIHCA). IV. Fragmentation in High-mass Star-forming Clumps Digging into the Interior of Hot Cores with ALMA (DIHCA). VI. The Formation of Low-mass Multiple Systems in High-mass Cluster-forming Regions Digging into the Interior of Hot Cores with ALMA (DIHCA). VII. Disk Candidates around High-mass Stars and Evidence of Anisotropic Infall Digging into the Interior of Hot Cores with the ALMA (DIHCA). III. The Chemical Link between NH<SUB>2</SUB>CHO, HNCO, and H<SUB>2</SUB>CO Hierarchical accretion flow from the G351 infrared dark filament to its central cores Magnetic Fields in Massive Star-forming Regions (MagMaR).	Beuther, H. Ginsburg, Adam Ishihara, Kousuke Li, Shanghuo Luo, Qiu-yi Olguin, Fernando A. Sakai, Takeshi Sanhueza, Patricio Taniguchi, Kotomi	Beuther, H.; Olguin, F. A.; Sanhueza, P.; Cunningham, N.; Ginsburg, A. Ginsburg, Adam; McGuire, Brett A.; Sanhueza, Patricio; Olguin, Fernando; Maud, Luke T.; Tanaka, Kei E. I.; Zhang, Yichen; Beuther, Henrik; Indriolo, Nick Ishihara, Kousuke; Sanhueza, Patricio; Nakamura, Fumitaka; Saito, Masao; Chen, Huei-Ru Vivien; Li, Shanghuo; Olguin, Fernando; Taniguchi, Kotomi; Morii, Kaho; Lu, Xing; Luo, Qiu-yi; Sakai, Takeshi; Zhang, Qizhou Li, Shanghuo; Sanhueza, Patricio; Beuther, Henrik; Chen, Huei-Ru Vivien; Kuiper, Rolf; Olguin, Fernando A.; Pudritz, Ralph E.; Stephens, Ian W.; Zhang, Qizhou; Nakamura, Fumitaka; Lu, Xing; Kuruwita, Rajika L.; Sakai, Takeshi; Henning, Thomas; Taniguchi, Kotomi; Li, Fei Luo, Qiu-yi; Sanhueza, Patricio; Offner, Stella S. R.; Olguin, Fernando; Ginsburg, Adam; Nakamura, Fumitaka; Morii, Kaho; Cheng, Yu; Tanaka, Kei E. I.; Liu, Junhao; Liu, Tie; Lu, Xing; Zhang, Qizhou; Taniguchi, Kotomi; Saha, Piyali; Li, Shanghuo; Mai, Xiaofeng Olguin, Fernando A.; Sanhueza, Patricio; Ginsburg, Adam	A complete understanding of the initial conditions of high-mass star formation and what processes determine multiplicity requires the study of the magnetic field in young massive cores. Using Atacama Large Millimeter/submillimeter Array (ALMA) 250 GHz polarization observations (0<inline-formula> </inline-formula>3 = 1000 au) and ALMA 220 GHz high-angular-resolution observations (0<inline-formula> </inline-formula>05 = 160 au), we have performed a full energy analysis including the magnetic field at core scales and have assessed what influences the multiplicity inside a massive core previously believed to be in the prestellar phase. With a mass of 31 M<SUB>⊙</SUB>, the G11.92 MM2 core has a young CS molecular outflow with a dynamical timescale of a few thousand years. At high resolution, the MM2 core fragments into a binary system, with a projected separation of 505 au and a binary mass ratio of 1.14. Using the Davis–Chandrasekhar–Fermi method with an angle dispersion function analysis, we estimate in this cor	2021	Different mechanisms have been suggested to explain the binarity of high-mass stars: core fragmentation, disk fragmentation, and multiple-body interactions. However, so far there is no observational constraints to assess their importance. With the unique capabilities of ALMA, we can for the first time statistically test these scenarios. We will observe continuum emission at 230 GHz to derive the multiplicity fraction and the distribution of companions separation. With a resolution of 0.06" (~100 pc at 2 kpc; ~200 pc at 3.8 kpc), we can resolved star-forming cores and the predicted disks (~1,000 AU) around high-mass stars. We have selected a large, uniform sample of 32 cores containing massive young stellar objects (MYSOs) embedded in 20 high-mass star-forming regions. With these observations, we will address: What is the binarity rate of high-mass cores at ~100s AU scales? How does the binarity rate of high-mass cores change as they evolve? Are high-mass binary systems formed at core scales (~1,000 AU) or dis	IRAS_181_b_06_TM1	Zhang, Qizhou; Hoq, Sadia; Jackson, James; Sakai, Takeshi; Nakamura, Fumitaka; Silva, Andrea; Ohashi, Satoshi; Contreras, Yanett; Chen, Vivien; Tatematsu, Ken'ichi; Miura, Rie;	1.1884810823504524	0.038286019057210165	0.502383	uid://A001/X88e/Xfd	uid://A001/X88e/Xfe	uid://A002/Xc46ab2/Xbbc	The formation of high-mass binary systems by core/disk fragmentation	S	TARGET	T	1.0389026303750921	F	2021ApJ...909..199O 2022ApJ...929...68O 2023ApJ...942...66G 2023ApJ...950...57T 2024ApJ...974...95I 2024NatAs...8..472L 2025A&A...695A..51B 2025ApJ...980...87S 2025ApJ...983...37S 2026ApJ...999..106O 2026ApJ...999..192L	High-mass star formation;null	ISM and star formation	psanhueza	Sanhueza, Patricio	1128.90625	2026-06-08T20:09:44.273
ADS/JAO.ALMA#2016.1.01036.S	ALMA	JAO	ALMA	uid://A001/X88e/Xfe.source.G11.1-0.12.spw.31	cube	2		G11.1-0.12	272.617784583385	-19.37525555556819	0.007152277190130827	Polygon ICRS 272.621390 -19.374150 272.621568 -19.375480 272.621215 -19.376778 272.620380 -19.377862 272.619611 -19.378389 272.618956 -19.378657 272.618260 -19.378803 272.617309 -19.378803 272.615958 -19.378389 272.614864 -19.377535 272.614179 -19.376361 272.614001 -19.375031 272.614355 -19.373733 272.614718 -19.373154 272.615368 -19.372500 272.616613 -19.371854 272.617547 -19.371686 272.618260 -19.371708 272.619611 -19.372122 272.620705 -19.372976			3840	1	2	0.04128075130196105	58007.094777	58692.220904	689.472	689.472	0.0013569096572749251	0.0013685240695310483	226238.05130961293	/XX/YY/	phot.flux.density;phys.polarization	https://almascience.org/datalink/sync?ID=uid://A001/X88e/Xfe	application/x-votable+xml; content=datalink		2016.1.01036.S	Public	11.10894801097218	-0.1143484859888878	6	6.048987875190272E-9	1.875E9	A001:DA59 A007:DV09 A015:DA61 A042:DV05 A058:DA41 A065:DA64 A069:DA55 A071:DA52 A074:DA47 A074:DV09 A075:DA56 A078:DV08 A082:DA60 A083:DA51 A084:DV04 A086:DV22 A087:DV25 A088:DV11 A089:DV16 A090:DV13 A090:DV24 A091:DA45 A091:DA61 A092:DV04 A092:DV14 A093:DV03 A093:DV20 A094:DV14 A094:DV19 A096:DA50 A101:DA62 A102:DV03 A104:DA58 A105:DA64 A105:DV02 A108:DA50 A110:DA41 A110:DA55 A111:DV12 A111:PM02 A115:DA43 A116:DV07 A116:DV08 A118:DV01 A118:DV07 A120:DA44 A120:DV19 A121:PM03 A122:DV11 A123:DA42 A124:DA42 A124:DA51 A125:DA49 A125:DA53 A126:DV10 A126:PM01 A127:DA49 A127:DV24 A128:DV15 A129:DA46 A129:DV01 A130:DA58 A130:DV15 A131:DV21 A131:PM03 A132:DA57 A132:DV23 A133:DV10 A133:PM04 A134:DA63 A135:DA57 A135:PM02 P401:DA59 P401:DA65 P403:DA45 P404:DV16 P410:DV06 S301:DA54 S301:DA60 S306:DV20 S307:DA47 W207:DV17 W207:DV25 W209:DA48 W210:DA53 W210:DV22	F	2019-03-01T20:36:27.000	0.04128075130196105	[216.86..218.74GHz,1052.73kHz,1.2mJy/beam@10km/s,76.8uJy/beam@native, XX YY] U [219.06..220.94GHz,976.56kHz,1.2mJy/beam@10km/s,76.6uJy/beam@native, XX YY] U [231.06..232.94GHz,1128.91kHz,1.2mJy/beam@10km/s,76.4uJy/beam@native, XX YY] U [233.56..235.44GHz,1128.91kHz,1.2mJy/beam@10km/s,76.5uJy/beam@native, XX YY]	220.00014124265695	1325.1195201894923	ALMA	Digging Into the Interior of Hot Cores with ALMA (DIHCA). V. Deuterium Fractionation of Methanol Digging into the Interior of Hot Cores with ALMA (DIHCA). I. Dissecting the High-mass Star-forming Core G335.579-0.292 MM1 Digging into the Interior of Hot Cores with ALMA (DIHCA). II. Exploring the Inner Binary (Multiple) System Embedded in G335 MM1 ALMA1 Digging into the Interior of Hot Cores with ALMA (DIHCA). IV. Fragmentation in High-mass Star-forming Clumps Digging into the Interior of Hot Cores with ALMA (DIHCA). VI. The Formation of Low-mass Multiple Systems in High-mass Cluster-forming Regions Digging into the Interior of Hot Cores with ALMA (DIHCA). VII. Disk Candidates around High-mass Stars and Evidence of Anisotropic Infall Digging into the Interior of Hot Cores with the ALMA (DIHCA). III. The Chemical Link between NH<SUB>2</SUB>CHO, HNCO, and H<SUB>2</SUB>CO Hierarchical accretion flow from the G351 infrared dark filament to its central cores Magnetic Fields in Massive Star-forming Regions (MagMaR).	Beuther, H. Ginsburg, Adam Ishihara, Kousuke Li, Shanghuo Luo, Qiu-yi Olguin, Fernando A. Sakai, Takeshi Sanhueza, Patricio Taniguchi, Kotomi	Beuther, H.; Olguin, F. A.; Sanhueza, P.; Cunningham, N.; Ginsburg, A. Ginsburg, Adam; McGuire, Brett A.; Sanhueza, Patricio; Olguin, Fernando; Maud, Luke T.; Tanaka, Kei E. I.; Zhang, Yichen; Beuther, Henrik; Indriolo, Nick Ishihara, Kousuke; Sanhueza, Patricio; Nakamura, Fumitaka; Saito, Masao; Chen, Huei-Ru Vivien; Li, Shanghuo; Olguin, Fernando; Taniguchi, Kotomi; Morii, Kaho; Lu, Xing; Luo, Qiu-yi; Sakai, Takeshi; Zhang, Qizhou Li, Shanghuo; Sanhueza, Patricio; Beuther, Henrik; Chen, Huei-Ru Vivien; Kuiper, Rolf; Olguin, Fernando A.; Pudritz, Ralph E.; Stephens, Ian W.; Zhang, Qizhou; Nakamura, Fumitaka; Lu, Xing; Kuruwita, Rajika L.; Sakai, Takeshi; Henning, Thomas; Taniguchi, Kotomi; Li, Fei Luo, Qiu-yi; Sanhueza, Patricio; Offner, Stella S. R.; Olguin, Fernando; Ginsburg, Adam; Nakamura, Fumitaka; Morii, Kaho; Cheng, Yu; Tanaka, Kei E. I.; Liu, Junhao; Liu, Tie; Lu, Xing; Zhang, Qizhou; Taniguchi, Kotomi; Saha, Piyali; Li, Shanghuo; Mai, Xiaofeng Olguin, Fernando A.; Sanhueza, Patricio; Ginsburg, Adam	A complete understanding of the initial conditions of high-mass star formation and what processes determine multiplicity requires the study of the magnetic field in young massive cores. Using Atacama Large Millimeter/submillimeter Array (ALMA) 250 GHz polarization observations (0<inline-formula> </inline-formula>3 = 1000 au) and ALMA 220 GHz high-angular-resolution observations (0<inline-formula> </inline-formula>05 = 160 au), we have performed a full energy analysis including the magnetic field at core scales and have assessed what influences the multiplicity inside a massive core previously believed to be in the prestellar phase. With a mass of 31 M<SUB>⊙</SUB>, the G11.92 MM2 core has a young CS molecular outflow with a dynamical timescale of a few thousand years. At high resolution, the MM2 core fragments into a binary system, with a projected separation of 505 au and a binary mass ratio of 1.14. Using the Davis–Chandrasekhar–Fermi method with an angle dispersion function analysis, we estimate in this cor	2021	Different mechanisms have been suggested to explain the binarity of high-mass stars: core fragmentation, disk fragmentation, and multiple-body interactions. However, so far there is no observational constraints to assess their importance. With the unique capabilities of ALMA, we can for the first time statistically test these scenarios. We will observe continuum emission at 230 GHz to derive the multiplicity fraction and the distribution of companions separation. With a resolution of 0.06" (~100 pc at 2 kpc; ~200 pc at 3.8 kpc), we can resolved star-forming cores and the predicted disks (~1,000 AU) around high-mass stars. We have selected a large, uniform sample of 32 cores containing massive young stellar objects (MYSOs) embedded in 20 high-mass star-forming regions. With these observations, we will address: What is the binarity rate of high-mass cores at ~100s AU scales? How does the binarity rate of high-mass cores change as they evolve? Are high-mass binary systems formed at core scales (~1,000 AU) or dis	IRAS_181_b_06_TM1	Zhang, Qizhou; Hoq, Sadia; Jackson, James; Sakai, Takeshi; Nakamura, Fumitaka; Silva, Andrea; Ohashi, Satoshi; Contreras, Yanett; Chen, Vivien; Tatematsu, Ken'ichi; Miura, Rie;	1.2251466730687346	0.038286019057210165	0.502383	uid://A001/X88e/Xfd	uid://A001/X88e/Xfe	uid://A002/Xc46ab2/Xbbc	The formation of high-mass binary systems by core/disk fragmentation	S	TARGET	T	1.0389026303750921	F	2021ApJ...909..199O 2022ApJ...929...68O 2023ApJ...942...66G 2023ApJ...950...57T 2024ApJ...974...95I 2024NatAs...8..472L 2025A&A...695A..51B 2025ApJ...980...87S 2025ApJ...983...37S 2026ApJ...999..106O 2026ApJ...999..192L	High-mass star formation;null	ISM and star formation	psanhueza	Sanhueza, Patricio	976.5625	2026-06-08T20:09:44.273
(1000 rows in the table, 200 printed)
INFO QUERY_STATUS = OVERFLOW
