J/A+A/696/A149ivo://CDS.VizieR/J/A+A/696/A149doi:10.26093/cds/vizier/bc-nr/lbejCDSMolinari S.Schilke P.Battersby C.Ho P.T.P.Sanchez-Monge A.,Traficante A.Jones B.Beltran M.T.Beuther H.Fuller G.A.Zhang Q.,Klessen R.S.Walch S.Tang Y.-W.Benedettini M.Elia D.Coletta A.,Mininni C.Schisano E.Avison A.Law C.Y.Nucara A.Soler J.D.,Stroud G.Wallace J.Wells M.R.A.Ahmadi A.Brogan C.L.Hunter T.R.,Liu S.-Y.Pezzuto S.Su Y.-N.Zimmermann B.Zhang T.Wyrowski F.,De Angelis F.Liu S.Clarke S.D.Fontani F.Klaassen P.D.Koch P.,Johnston K.G.Lebreuilly U.Liu T.Lumsden S.L.Moeller T.,Moscadelli L.Kuiper R.Lis D.Peretto N.Pfalzner S.Rigby A.J.,Sanhueza P.Rygl K.L.J.van der Tak F.Zinnecker H.Amaral F.Bally J.,Bronfman L.Cesaroni R.Goh K.Hoare M.G.Hatchfield P.Hennebelle P.,Henning T.Kim K.T.Kim W.-J.Maud L.Merello M.Nakamura F.Plume R.,Qin S.-L.Svoboda B.Testi L.Veena V.S.Walker D.2026-07-03T06:36:49Z2025-04-15T09:32:32ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frinfrared-sourcesinterferometrymillimeter-astronomysubmillimeter-astronomyA large fraction of stars form in clusters containing high-mass stars, which subsequently influences the local and galaxy-wide environment. Fundamental questions about the physics responsible for fragmenting molecular parsec-scale clumps into cores of a few thousand astronomical units (au) are still open, that only a statistically significant investigation with ALMA is able to address; for instance: the identification of the dominant agents that determine the core demographics, mass, and spatial distribution as a function of the physical properties of the hosting clumps, their evolutionary stage and the different Galactic environments in which they reside. The extent to which fragmentation is driven by clumps dynamics or mass transport in filaments also remains elusive. With the ALMAGAL project, we observed the 1.38mm continuum and lines toward more than 1000 dense clumps in our Galaxy, with M>=500M_{sun}_, {SIGMA}>=0.1g/cm^2^ and d<=7.5 kiloparsec (kpc). Two different combinations of ALMA Compact Array (ACA) and 12-m array setups were used to deliver a minimum resolution of ~1000 au over the entire sample distance range. The sample covers all evolutionary stages from infrared dark clouds (IRDCs) to HII regions from the tip of the Galactic bar to the outskirts of the Galaxy. With a continuum sensitivity of 0.1mJy, ALMAGAL enables a complete study of the clump-to-core fragmentation process down to M~0.3M_{sun}_ across the Galaxy. The spectral setup includes several molecular lines to trace the multiscale physics and dynamics of gas, notably CH_3_CN, H_2_CO, SiO, CH_3_OH, DCN, HC_3_N, and SO, among others. We present an initial overview of the observations and the early science product and results produced in the ALMAGAL Consortium, with a first characterization of the morphological properties of the continuum emission detected above 5{sigma} in our fields. We used "perimeter-versus-area" and convex hull-versus-area metrics to classify the different morphologies. We find that more extended and morphologically complex (significantly departing from circular or generally convex) shapes are found toward clumps that are relatively more evolved and have higher surface densities. ALMAGAL is poised to serve as a game-changer for a number of specific issues in star formation: clump-to-core fragmentation processes, demographics of cores, core and clump gas chemistry and dynamics, infall and outflow dynamics, and disk detections. Many of these issues will be covered in the first generation of papers that closely follow on the present publication.2025A&A...696A.149Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/696/A149CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/696/A151 : ALMAGAL III. Compact source catalog (Coletta+, 2024)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/696/A149https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/696/A149http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/696/A149https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/696/A149https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/696/A149http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/696/A149GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/696/A149/table1 (Targets physical parameters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/696/A149/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/696/A149/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/696/A149/table1?GETtext/xml+votable180.050000true272.7258306-20.54723190.0055555555555555565/7278 7377 7383 7564 9341 9482 10424 10453 10542 10556 10595 10624 6/20831 21504 21671 22038-22039 22041 22045 29091 29094 29097 29099-29101 29103 29116 29118-29119 29162 29461 29463 29504-29505 29522-29523 29526 29528-29529 30218-30219 30223 30241 30244-30245 30247 30260 30262-30263 30268-30269 30312 37333 37340-37341 37343 37372 37713 37746 37752-37753 37842 37848 37850 37895 37897 37901-37902 37922-37924 37926 37934 38016 38018-38019 38024 38026 39246 39268 39270-39271 39276 39376 39386 39404 39408 39768 39803 39889 39898-39899 39926 39934 40618 41598 41653 41655 41660-41661 41671 41673 41675-41678 41681-41684 41688 41766-41767 41770 41772 41777-41778 41780-41782 41799 41804-41805 41809 41811 41816-41817 41820-41821 41824-41825 41856 42159 42172-42174 42207 42210-42211 42213-42217 42220 42228-42230 42376 42378-42379 42387 42390-42393 42396-42398 42400 42435-42438 42440-42441 42444-42445 42500-42502 42512 43013-43015 43019-43021 43024 43026 43040https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/696/A149?format=asciiInfraredMillimeterdefaultJ/A+A/696/A149/table1Targets physical parameters_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.raindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decindexedrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNum[1/1013] Target clump running numbermeta.idintNameALMAGAL target name (AGLLL.llll+B.bbbb)meta.id;meta.maincharOrigNameOriginal target namemeta.idcharIntIDTarget name in ALMA archive (internal ID)meta.idcharGLONGalactic Longitudedegpos.galactic.lonGLATGalactic Latitudedegpos.galactic.latsubflag[n/f] subsample flag (near/far)meta.codecharVlsrLSR velocity of targetkm/sphys.veloc;pos.lsrfloatDistHeliocentric distancepcpos.distanceinte_DistUncertainty on distancepcstat.errorintMass? Target clump mass (from Hi-GAL)solMassphys.massintnullablee_Mass? Uncertainty on target clump masssolMassstat.error;phys.massintnullableLum? Target clump luminosity (from Hi-GAL)solLumphys.luminosityintnullablee_Lum? Uncertainty on target clump luminositysolLumstat.errorintnullableTdust? Clump dust temperature (from Hi-GAL)Kphys.temperaturefloatnullableTbol? Clump bolometric temperatureKphys.temperaturefloatnullableSdens? Clump surface density (from Hi-GAL)g.cm**-2phot.flux.density.sbfloatnullableEclEvolutionary Class (Urquhart et al., 2022MNRAS.510.3389U, Cat. J/MNRAS/510/3389) (1)meta.code.classcharFlagsSource data flags (2)meta.code.errorcharJ/A+A/696/A149/table2Morphological parameters of the 1.38mm emissionrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNumTarget clump running numbermeta.idintAlin-5s? Area of 5-sigma continuum RoIpc**2phys.area;spect.continuumfloatnullableAfrac-5s? Area of 5-sigma continuum RoI/FoV%stat.fit.paramfloatnullableDcirc-5s? Departure from circularity parameterstat.fit.paramfloatnullableQhull-5s? Area RoI/Area Convex Hullstat.fit.paramfloatnullable