J/A+A/696/A151 ALMAGAL III. Compact source catalog (Coletta+, 2025)
ALMAGAL. III. Compact source catalog:
Fragmentation statistics and physical evolution of the core population.
Coletta A., Molinari S., Schisano E., Traficante A., Elia D.,
Benedettini M., Mininni C., Soler J.D., Sanchez-Monge A., Schilke P.,
Battersby C., Fuller G.A., Beuther H., Zhang Q., Beltran M.T., Jones B.,
Klessen R.S., Walch S., Fontani F., Avison A., Brogan C.L., Clarke S.D.,
Hatchfield P., Hennebelle P., Ho P.T.P., Hunter T.R., Johnston K.G.,
Klaassen P.D., Koch P.M., Kuiper R., Lis D.C., Liu T., Lumsden S.L.,
Maruccia Y., Moeller T., Moscadelli L., Nucara A., Rigby A.J., Rygl K.L.J.,
Sanhueza P., van der Tak F., Wells M.R.A., Wyrowski F., De Angelis F.,
Liu S., Ahmadi A., Bronfman L., Liu S.-Y., Su Y.-N., Tang Y., Testi L.,
Zinnecker H.
<Astron. Astrophys. 696, A151 (2025)>
=2025A&A...696A.151C 2025A&A...696A.151C (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Interferometry ;
Photometry, millimetric/submm ; Stars, diameters ; Stars, masses
Keywords: methods: observational - techniques: interferometric - surveys -
stars: formation - ISM: structure - submillimeter: ISM
Abstract:
The physical mechanisms behind the fragmentation of high-mass dense
clumps into compact star-forming cores and the properties of these
cores are fundamental topics that are heavily investigated in current
astrophysical research. The ALMAGAL survey provides the opportunity to
study this process at an unprecedented level of detail and statistical
significance, featuring high-angular resolution 1.38mm ALMA
observations of 1013 massive dense clumps at various Galactic
locations. These clumps cover a wide range of distances (∼2-8kpc),
masses (∼102-104M☉), surface densities (0.1-10g/cm-2), and
evolutionary stages (luminosity over mass ratio indicator of
∼0.05<L/M<450L☉/M☉). Here, we present the catalog of
compact sources obtained with the CuTEx algorithm from continuum
images of the full ALMAGAL clump sample combining ACA-7m and 12m ALMA
arrays, reaching a uniform high median spatial resolution of ∼1400au
(down to ∼800au). We characterize and discuss the revealed
fragmentation properties and the photometric and estimated physical
parameters of the core population. The ALMAGAL compact source catalog
includes 6348 cores detected in 844 clumps (83% of the total), with a
number of cores per clump between 1 and 49 (median of 5). The
estimated core diameters are mostly within ∼800-3000au (median of
1700au). We assigned core temperatures based on the L/M of the hosting
clump, and obtained core masses from 0.002 to 345M☉ (complete
above 0.23M☉), exhibiting a good correlation with the core radii
(M∼R^2.6). We evaluated the variation in the core mass function (CMF)
with evolution as traced by the clump L/M, finding a clear, robust
shift and change in slope among CMFs within subsamples at different
stages. This finding suggests that the CMF shape is not constant
throughout the star formation process, but rather it builds (and
flattens) with evolution, with higher core masses reached at later
stages. We found that all cores within a clump grow in mass on average
with evolution, while a population of possibly newly formed lower-mass
cores is present throughout. The number of cores increases with the
core masses, at least until the most massive core reaches ∼10M☉.
More generally, our results favor a clump-fed scenario for high-mass
star formation, in which cores form as low-mass seeds, and then gain
mass while further fragmentation occurs in the clump.
Description:
We present the catalog of the compact cores (6348 sources) detected
and measured with the source extraction and photometry algorithm CuTEx
in the high-resolution (∼1400au) and high-sensitivity (∼0.05mJy)
continuum images of the 1013 massive clumps observed at 1.38mm with
the ALMA interferometer in the context of the ALMAGAL large survey. In
detail, Table 3 reports the coordinates and the main measured
photometric parameters of the sources, while Table 7 reports the main
estimated physical properties. The tables have the same name, and
number and order of columns as in the paper.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 115 6348 Core coordinates and photometric parameters
table7.dat 53 6348 Core estimated physical properties
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See also:
J/A+A/690/A185 : Dynamical accretion flows. ALMAGAL (Wells+, 2024)
J/A+A/696/A149 : ALMAGAL. I. Target clumps properties (Molinari+, 2025)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name ALMAGAL clump name, AGLLL.llll+B.bbbb
19- 20 I2 --- Seq Ordinal core id within the clump
22- 30 F9.5 deg RAdeg Right ascension (FK5, J2000)
32- 40 F9.5 deg DEdeg Declination (FK5, J2000)
42- 50 F9.5 deg GLON Galactic longitude
52- 59 F8.5 deg GLAT Galactic latitude
61- 67 F7.2 mJy/beam Fpeak Background-subtracted peak flux at 1.38mm
69- 74 F6.2 mJy/beam Fbkg Background flux value at 1.38mm at
flux peak position
76- 79 F4.2 arcsec Diam1 FWHM of the fitted source ellipse (axis 1)
81- 84 F4.2 arcsec Diam2 FWHM of the fitted source ellipse (axis 2)
86- 89 I4 deg PAs Orientation (position angle) of the source
91- 97 F7.2 mJy Fint Integrated flux at 1.38mm
99-102 F4.2 arcsec MajDiam Major axis of the map beam
104-107 F4.2 arcsec MinDiam Minor axis of the map beam
109-111 I3 deg PAb Beam position angle
113 A1 --- Flag1 [Y/N] Flag for radio emission within the core
115 A1 --- Flag2 [Y/N] Flag for radio emission within the clump
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name ALMAGAL clump name, AGLLL.llll+B.bbbb
19- 20 I2 --- Seq Ordinal core id within the clump
22- 25 I4 AU Diam Core physical diameter
27- 31 F5.1 Msun/Lsun L/M Clump evolutionary indicator
33- 34 I2 K Tcore Core temperature (used for Mcore)
36- 41 F6.2 Msun Mcore Core mass
43- 47 F5.1 g/cm2 surfdcore Core average mass surface density
49- 53 F5.1 10+7cm-3 nH2 Core average volume density
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Acknowledgements:
Alessandro Coletta, alessandro.coletta(at)inaf.it
References:
Molinari et al., Paper I 2025A&A...696A.149N 2025A&A...696A.149N, Cat. J/A+A/696/A149
Sanchez-Monge et al., Paper II 2025A&A...696A.150S 2025A&A...696A.150S
(End) A. Coletta [INAF-IAPS Rome, Italy], P. Vannier [CDS] 14-Feb-2025