J/A+A/687/A217 15 massive protoclusters point-process mapping (Dell'Ova+, 2024)
ALMA-IMF XII: Point-process mapping of 15 massive protoclusters.
Dell'Ova P., Motte F., Gusdorf A., Pouteau Y., Men'shchikov A.,
Diaz-Gonzalez D., Galvan-Madrid R., Lesaffre P., Didelon P., Stutz A.M.,
Towner A.P.M., Marsh K., Whitworth A., Armante M., Bonfand M., Nony T.,
Valeille-Manet M., Bontemps S., Csengeri T., Cunningham N., Ginsburg A.,
Louvet F., Alvarez-Gutierrez R.H., Brouillet N., Salinas J., Sanhueza P.,
Nakamura F., Nguyen Luong Q., Baug T., Fernandez-Lopez M., Liu H.-L.,
Olguin F.
<Astron. Astrophys. 687, A217 (2024)>
=2024A&A...687A.217D 2024A&A...687A.217D (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds ; H II regions ; Interstellar medium ;
Millimetric/submm sources
Keywords: stars: formation - stars: luminosity function, mass function -
stars: protostars - ISM: clouds - dust, extinction - evolutio
Abstract:
A crucial aspect in addressing the challenge of measuring the core
mass function (CMF), that is pivotal for comprehending the origin of
the initial mass function (IMF), lies in constraining the temperatures
of the cores.
We aim to measure the luminosity, mass, column density and dust
temperature of star-forming regions imaged by the ALMA-IMF large
program. These fields were chosen to encompass early evolutionary
stages of massive protoclusters. High angular resolution mapping is
required to capture the properties of protostellar and pre-stellar
cores within these regions, and to effectively separate them from
larger features, such as dusty filaments.
We employed the point process mapping (PPMAP) technique, enabling us
to perform spectral energy distribution fitting of far-infrared and
submillimeter observations across the 15 ALMA-IMF fields, at an
unmatched 2.5'' angular resolution. By combining the modified
blackbody model with near-infrared data, we derived bolometric
luminosity maps. We estimated the errors impacting values of each
pixel in the temperature, column density, and luminosity maps.
Subsequently, we employed the extraction algorithm getsf on the
luminosity maps in order to detect luminosity peaks and measure their
associated masses.
We obtained high-resolution constraints on the luminosity, dust
temperature, and mass of protoclusters, that are in agreement with
previously reported measurements made at a coarser angular resolution.
We find that the luminosity-to-mass ratio correlates with the
evolutionary stage of the studied regions, albeit with intra-region
variability. We compiled a PPMAP source catalog of 313 luminosity
peaks using getsf on the derived bolometric luminosity maps. The PPMAP
source catalog provides constraints on the mass and luminosity of
protostars and cores, although one source may encompass several
objects. Finally, we compare the estimated luminosity-to-mass ratio of
PPMAP sources with evolutionary tracks and discuss the limitations
imposed by the 2.5'' beam.
Description:
Luminosity, temperature and column density maps obtained with PPMAP
(Marsh et al., 2015MNRAS.454.4282M 2015MNRAS.454.4282M).
The maps were optimized for Herschel/PACS, Herschel/SPIRE, SABOCA,
LABOCA and ALMA observations.
The following star-forming regions were mapped : G008, G010, G012,
G327, G328, G333, G337, G338, G351, G353, W43-MM1, W43-MM2, W43-MM3,
W51-E, W51-IRS.
Objects:
-------------------------------------------------------
RA (2000) DE Designation(s)
-------------------------------------------------------
18 06 19.02 -21 37 32.3 G008 = AGAL_G008.671-00.356
18 10 29.21 -19 55 41.1 G010 = AGAL_G010.624-00.384
18 14 13.34 -17 55 45.2 G012 = AGAL_G012.804-00.199
15 53 08.61 -54 37 06.1 G327 = AGAL_G327.293-00.579
15 55 48.91 -52 43 07.8 G328 = AGAL_G328.809+00.632
16 22 09.45 -50 05 58.0 G333 = AGAL_G333.604-00.212
16 41 10.60 -47 08 02.9 G337 = AGAL_G337.916-00.477
16 40 34.39 -45 41 40.5 G338 = AGAL_G338.926+00.554
17 26 42.59 -36 09 20.5 G351 = AGAL_G351.774-00.537
17 29 18.93 -34 32 05.9 G353 = AGAL_G353.417-00.079
18 47 47.00 -01 54 28.0 W43-MM1 = [MSL2003] W43-MM1
18 47 36.60 -02 00 54.0 W43-MM2 = [MSL2003] W43-MM2
18 47 41.70 -02 00 25.9 W43-MM3 = [MSL2003] W43-MM3
19 23 41.89 +14 30 35.9 W51E = W 51e
19 23 39.93 +14 31 09.3 W51IRS = [WBN74] W 51 IRS 2
-------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 122 120 List of fits maps
fits/* . 120 Individual fits maps
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See also:
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)
J/A+A/674/A75 : W43-MM1 and W43-MM2+MM3 ALMA datacubes (Nony+, 2023)
J/ApJS/269/55 : ALMA-IMF VIII. Dust-dominated structures (Diaz-Gonzalez+, 2023)
Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 22 I3 --- Nx Number of pixels along X-axis
24- 26 I3 --- Ny Number of pixels along Y-axis
28- 30 I3 Kibyte size Size of FITS file
32- 65 A34 --- FileName Name of FITS file, in subdirectory fits
67-122 A56 --- Title Title of the FITS file
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Acknowledgements:
Pierre Dell'Ova, pierre.dellova(at)universite-paris-saclay.fr
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
Nony et al., Paper V 2023A&A...674A..75N 2023A&A...674A..75N, Cat. J/A+A/674/A75
Pouteau et al., Paper VI 2023A&A...674A..76P 2023A&A...674A..76P
Cunningham et al., Paper VII 2023A&A...678A.194C 2023A&A...678A.194C
Diaz-Gonzalez et al., Paper VIII 2023ApJS..269...55D 2023ApJS..269...55D, Cat. J/ApJS/269/55
Towner et al., Paper IX 2024ApJ...960...48T 2024ApJ...960...48T
(End) Patricia Vannier [CDS] 21-Jun-2024