J/A+A/674/A75 W43-MM1 and W43-MM2+MM3 ALMA datacubes (Nony+, 2023)
ALMA-IMF. V.
Prestellar and protostellar core populations in the W43 cloud complex.
Nony T., Galvan-Madrid R., Motte F., Pouteau Y., Cunningham N., Louvet F.,
Stutz A.M., Lefloch B., Bontemps S., Brouillet N., Ginsburg A., Joncour I.,
Herpin F., Sanhueza P., Csengeri T., Towner A.P.M., Bonfand M.,
Fernandez-Lopez M., Baug T., Bronfman L., Busquet G., Di Francesco J.,
Gusdorf A., Lu X., Olguin F., Valeille-Manet M., Whitworth A.P.
<Astron. Astrophys. 674, A75 (2023)>
=2023A&A...674A..75N 2023A&A...674A..75N (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds ; Millimetric/submm sources
Keywords: stars: formation - stars: protostars - stars: massive - ISM: clouds -
ISM: jets and outflows
Abstract:
The origin of the stellar initial mass function (IMF) and its relation
with the core mass function (CMF) are actively debated issues with
important implications in astrophysics. Recent observations in the W43
molecular complex of top-heavy CMFs, with an excess of high-mass cores
compared to the canonical mass distribution, raise questions about our
understanding of the star formation processes and their evolution in
space and time. We aim to compare populations of protostellar and
prestellar cores in three regions imaged in the ALMA-IMF Large
Program. We created an homogeneous core catalogue in W43, combining a
new core extraction in W43-MM1 with the catalogue of W43-MM2&MM3
presented in a previous work. Our detailed search for protostellar
outflows enabled us to identify between 23 and 30 protostellar cores
out of 127 cores in W43-MM1 and between 42 and 51 protostellar cores
out of 205 cores in W43-MM2&MM3. Cores with neither outflows nor hot
core emission are classified as prestellar candidates. We found a
similar fraction of cores which are protostellar in the two regions,
about 35%. This fraction strongly varies in mass, from 15-20% at low
mass, between 0.8 and 3M☉ up to about 80% above 16M☉.
Protostellar cores are found to be, on average, more massive and
smaller in size than prestellar cores. Our analysis also revealed that
the high-mass slope of the prestellar CMF in W43,
alpha=-1.46-0.19+0.12, is consistent with the Salpeter slope, and
thus the top-heavy form measured for the global CMF, alpha=-0.96, is
due to the protostellar core population. Our results could be
explained by clump-fed models in which cores grow in mass, especially
during the protostellar phase, through inflow from their environment.
The difference between the slopes of the prestellar and protostellar
CMFs moreover implies that high-mass cores grow more in mass than
low-mass cores.
Description:
Catalogs of protostellar and prestellar cores identified in ALMA 1.3mm
continuum maps in W43-MM2&MM3 (Tables F1) and W43-MM1 (Table F2). The
protostellar cores have been characterized through outflow surveys
using CO(2-1) data, which are also provided. The full properties of
cores in W43-MM2&MM3 are presented in the catalogue of Pouteau et al.
(2022A&A...664A..26P 2022A&A...664A..26P, Cat. J/A+A/664/A26).
The PPV CO(2-1) cube of region MM1 is available at Cat. J/A+A/636/A38.
Objects:
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RA (2000) DE Designation(s)
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18 47 36.6 -02 00 54 [MSL2003] W43-MM2 = AGAL G030.703-00.067
18 47 41.7 -02 00 26 [MSL2003] W43-MM3 = [MSL2003] W43-MM3
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablef2.dat 108 71 Catalog of cores in W43-MM1
tablef1.dat 102 130 Catalog of cores in W43-MM2&MM3
list.dat 151 2 List of fits datacubes
fits/* . 2 Individual fits files
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See also:
J/A+A/636/A38 : W43-MM1 ALMA 12CO(2-1) datacube (Nony+, 2020)
J/A+A/662/A9 : 15 dense molecular cloud regions ALMA images (Ginsburg+, 2022)
J/A+A/664/A26 : W43-MM2+MM3 ministarburst ALMA data (Pouteau+, 2022)
Byte-by-byte Description of file: tablef2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/177] Core number
5- 15 A11 --- Name Core full name, W43-MM1_ALMA-IMF1847s-154s
17- 18 I2 h RAh Right Ascension ICRS, Epoch=J2000
20- 21 I2 min RAm Right Ascension ICRS, Epoch=J2000
23- 27 F5.2 s RAs Right Ascension ICRS, Epoch=J2000
29 A1 --- DE- Declination sign ICRS, Epoch=J2000
30- 31 I2 deg DEd Declination ICRS, Epoch=J2000
33- 34 I2 arcmin DEm Declination ICRS, Epoch=J2000
36- 40 F5.2 arcsec DEs Declination ICRS, Epoch=J2000
42- 45 F4.2 arcsec aFWHM FWHM major axis
47- 50 F4.2 arcsec bFWHM FWHM minor axis
52- 54 I3 deg PA Position angle (North to East)
56- 60 F5.1 mJy/beam Speak Peak flux at 1.3mm
62- 64 F3.1 mJy/beam e_Speak Peak flux uncertainty
66- 70 F5.1 mJy Sint Integrated flux at 1.3mm
72- 74 F3.1 mJy e_Sint Integrated flux uncertainty
76- 77 I2 K Tdust Dust temperature
79- 80 I2 K e_Tdust Dust temperature uncertainty
82- 86 F5.1 Msun Mass Mass
88- 91 F4.1 Msun e_Mass Mass uncertainty
93- 94 A2 --- Blue [N/Y/Y?] Outflow Blue lobe [No/Yes/Possibly]
96- 97 A2 --- Red [N/Y/Y?] Outflow Red lobe [No/Yes/Possibly]
99-108 A10 --- Com Comment on protostellar core nature (1)
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Note (1): Commnets as follows:
tent. = Tentative outflows
HC = associated to hot cores
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Byte-by-byte Description of file: tablef1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/287] Core number
5- 22 A18 --- Name Core full name, W43-MM1_ALMA-IMF RAhmsDEdms
24- 25 I2 h RAh Right Ascension ICRS, Epoch=J2000
27- 28 I2 min RAm Right Ascension ICRS, Epoch=J2000
30- 34 F5.2 s RAs Right Ascension ICRS, Epoch=J2000
36 A1 --- DE- Declination sign ICRS, Epoch=J2000
37- 38 I2 deg DEd Declination ICRS, Epoch=J2000
40- 41 I2 arcmin DEm Declination ICRS, Epoch=J2000
43- 47 F5.2 arcsec DEs Declination ICRS, Epoch=J2000
49- 52 F4.2 arcsec aFWHM FWHM major axis
54- 57 F4.2 arcsec bFWHM FWHM minor axis
59- 61 I3 deg PA Position angle (North to East)
63- 66 F4.1 Msun Mass Mass
68- 71 F4.1 Msun e_Mass Mass uncertainty
73- 75 A3 --- Blue [N/Y/Y?] Outflow Blue lobe [No/Yes/Possibly]
77- 79 A3 --- Red [N/Y/Y?] Outflow Red lobe [No/Yes/Possibly]
81-102 A22 --- Com Comment on protostellar core nature,
tentative or low velocity outflows, hot core
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 23 I4 --- Nx Number of pixels along X-axis
25- 28 I4 --- Ny Number of pixels along Y-axis
30- 32 I3 --- Nz Number of slices
34- 59 A26 "datime" Obs.date Observation date
61- 67 F7.3 GHz bFreq Lower value of frequency interval
69- 75 F7.3 GHz BFreq Upper value of frequency interval
77- 82 I6 Hz dFreq Frequency resolution
84- 90 I7 Kibyte size Size of FITS file
92-126 A35 --- FileName Name of FITS file, in subdirectory fits
128-151 A24 --- Title Title of the FITS file
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Acknowledgements:
Thomas Nony, t.nony(at)irya.unam.mx
References:
Motte et al., Paper I 2022A&A...662A...8M 2022A&A...662A...8M
Ginsburg et al., Paper II 2022A&A...662A...9G 2022A&A...662A...9G, Cat. J/A+A/662/A9
Pouteau et al., Paper III 2022A&A...664A..26P 2022A&A...664A..26P, Cat. J/A+A/664/A26
Brouillet et al., Paper IV 2022A&A...665A.140B 2022A&A...665A.140B
(End) Patricia Vannier [CDS] 08-Mar-2023