J/A+A/694/A24 ALMA-IMF XVI (Motte+, 2025)
ALMA-IMF. XVI: Mass-averaged temperature of cores and protostellar luminosities
in the ALMA-IMF protoclusters.
Motte F., Pouteau Y., Nony T., Dell'Ova P., Gusdorf A., Brouillet N.,
Stutz A.M., Bontemps S., Ginsburg A., Csengeri T., Men'shchikov A.,
Valeille-Manet M., Louvet F., Bonfand M., Galvan-Madrid R.,
Alvarez-Gutierrez R.H., Armante M., Bronfman L., Chen H.-R.V.,
Cunningham N., Diaz-Gonzalez D., Didelon P., Fernandez-Lopez M.,
Herpin F., Kessler N., Koley A., Lefloch B., Le Nestour N., Liu H.-L.,
Moraux E., Nguyen Luong Q., Olguin F., Salinas J., Sandoval-Garrido N.A.,
Sanhueza P., Veyry R., Yoo T.
<Astron. Astrophys. 694, A24 (2025)>
=2025A&A...694A..24M 2025A&A...694A..24M (SIMBAD/NED BibCode)
ADC_Keywords: Star Forming Region ; Infrared sources ; Interstellar medium ;
YSOs
Keywords: circumstellar matter - stars: formation -
stars: fundamental parameters - stars: protostars - dust, extinction -
ISM: structure
Abstract:
The ALMA-IMF Large Program imaged 15 massive protoclusters down to a
resolution of 2kau scales, identifying about 1000 star-forming cores.
The mass and luminosity of these cores, which are fundamental physical
characteristics, are difficult to determine, a problem greatly
exacerbated at the distances >2kpc of ALMA-IMF protoclusters.
We combined new datasets and radiative transfer modeling to
characterize these cores. We estimated their mass-averaged temperature
and the masses these estimates imply. For one-sixth of the sample, we
measured the bolometric luminosities, implementing deblending
corrections when necessary.
We used spectral energy distribution (SED) analysis obtained with the
point process mapping (PPMAP) Bayesian procedure, which aims to
preserve the best angular resolution of the input data. We
extrapolated the luminosity and dust temperature images provided by
PPMAP at 2.5" resolution to estimate those of individual cores, which
were identified at higher angular resolution. To do this, we applied
approximate radiative transfer relationships between the luminosity of
a protostar and the temperature of its surrounding envelope and
between the external heating of prestellar cores and their
temperatures.
For the first time, we provide data-informed estimates of dust
temperatures for 882 cores identified with ALMA-IMF: 17-31K and 28-79K
(5th and 95th percentiles, up to 127K) for the 616 prestellar and
266 protostellar cores, respectively. We also measured protostellar
luminosities spanning 20-80000L☉.
Dust temperatures previously estimated from SED-based analyses at a
comparatively lower resolution validate our method. For hot cores, on
the other hand, we estimated systematically lower temperatures than
studies based on complex organic molecules. We established a
mass-luminosity evolutionary diagram, for the first time at the core
spatial resolution and for a large sample of intermediate- to
high-mass protostellar cores. The ALMA-IMF data favor a scenario in
which protostars accrete their mass from a larger mass reservoir than
their host cores.
Description:
Appendix C presents Tables C.1-C.2 and Table C.4, which focus on the
case study regions G012.80, W43-MM1, W43-MM2, and-MM3. Tables C.6-C.8
complement them, respectively, for the ten other ALMA-IMF regions: the
Young G327.29, G328.25, G337.92, and G338.93 protoclusters, the
Intermediate G008.67, G353.41, and W51-E protoclusters, and the
G010.62, G333.60, and W51-IRS2 protoclusters. Tables C.1 and C.6, for
the Young and Intermediate protoclusters, their luminosity peaks
associated with protostars, characterize them and their association
with temperature peaks (see Sects. 2.1-2.2 and 3.2, Fig. D.1).
Tables C.2 and C.7 do the same for the luminosity peaks identified
by the present study in Evolved protoclusters. As for Tables C.4 and
C.8, they give the main physical properties of the protostellar cores
found in the ALMA-IMF protoclusters. They list their mass-averaged
temperature, mass, and luminosity, as computed in Sects. 4 and 6.1
(see also Fig. 3), in Sect. 6.2, and in Sect. 4.3 (see also Fig. 4).
Table C.5 is dedicated to the prestellar core candidates found in the
14 ALMA-IMF protoclusters studied in the present study (see Sects.
2.1). It focuses here on the cores more massive than 6:5 M but the
complete table of 617 ALMA-IMF prestellar cores is accessible through
the CDS services. The table provides the mass-averaged dust
temperature and mass of prestellar cores, as computed in Sect. 5 (see
also Fig. 3) and Sect. 6.2, respectively.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablec1.dat 61 45 Luminosity peaks in Young and Intermediate W43
protoclusters and their association with
temperature peaks and protostellar cores
tablec2.dat 78 26 Luminosity peaks in the Evolved G012.80
protocluster and their association with
temperature peaks and protostellar cores
tablec3.dat 100 8 Luminosity and mass-averaged temperature of the
protostellar cores driving the six brightest
hot cores of ALMA-IMF
tablec4.dat 79 111 Main characteristics of protostellar cores in
the G012.80, W43-MM1, W43-MM2, and W43-MM3
protoclusters
tablec5.dat 38 616 Main characteristics of the 616 prestellar cores
in the ALMA-IMF protoclusters
tablec6.dat 60 52 Luminosity peaks and their association with
temperature peaks and protostellar cores in the
Young G327.29, G328.25, G337.92, and G338.93
protoclusters and in the Intermediate G008.67,
G353.41, and W51-E protoclusters
tablec7.dat 81 32 Luminosity peaks and their association with
temperature peaks and protostellar cores in the
Evolved G010.62, G333.60, and W51-IRS2
protoclusters
tablec8.dat 86 155 Main characteristics of protostellar cores in
the G327.29, G328.25, G337.92, G338.93,
G008.67, G353.41, W51-E, G010.62, G333.60, and
W51-IRS2 protoclusters
--------------------------------------------------------------------------------
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/A+A/687/A217 : 15 massive protoclusters point-process mapping
(Dell'Ova+, 2024)
J/A+A/690/A33 : Core mass function in high-mass star formation (Louvet+, 2024)
Byte-by-byte Description of file: tablec1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Protocluster Protocluster name in the ALMA-IMF sample
9- 11 A3 --- LPeak Luminosity peak identifier (1)
13 A1 --- n_LPeak [+] Note on LPeak (2)
15- 19 F5.2 10+3Lsun Lbol Integrated luminosity (1)
21- 24 F4.2 10+3Lsun e_Lbol Integrated luminosity error (1)
26- 28 F3.1 arcsec thetaLbol Mean full width at half maximum of the
luminosity peak (1)
30- 33 F4.1 kau FWHMLbol Mean full width at half maximum of the
luminosity peak (1)
35- 37 A3 --- Tpeak? [yes/no ] Presence or absence of
temperature peak (3)
39- 41 I3 --- N Protostellar core identifier (4)
42 A1 --- n_N [*] *: protostellar cores are tentative
44- 47 F4.2 arcsec thetacore Mean full width at half maximum of
the core (5)
49- 52 F4.2 arcsec DLbol Distance between the centers of the
protostellar core and its host
luminosity peak (5)
54- 55 I2 K PPMAPTdust Dust temperature measured in the PPMAP
temperature image (6)
57 I1 K e_PPMAPTdust Temperature error measured in the error
image of the PPMAP temperature (6)
59- 61 I3 % ContribL Contribution level of each protostellar
core to their associated luminosity
peak (7)
--------------------------------------------------------------------------------
Note (1): Luminosity peak name, integrated luminosity and its error, and mean
FWHM sizes. Values are taken or computed from Table B.1 of
Dell'Ova et al., 2024A&A...687A.217D 2024A&A...687A.217D, Cat. J/A+A/687/A217.
Note (2): The luminosity peak with a + tag is common to the W43-MM2 and W43-MM3
regions; we characterized it only once, in W43-MM3.
Note (3): Presence or absence of a temperature peak detected in the ellipse
describing the FWHM of the luminosity peak.
Note (4): Protostellar cores associated with the luminosity peak of LPeak
have their centers inside the ellipse describing the FWHM of the luminosity
peak.
ID numbers and FWHM angular sizes of protostellar cores are taken from the
catalogs of Nony et al. 2023A&A...674A..75N 2023A&A...674A..75N, Cat. J/A+A/674/A75 and
Pouteau et al. 2022A&A...664A..26P 2022A&A...664A..26P, Cat. J/A+A/664/A26 (see Sect 2.1).
Note (5): Distance between the centers of the protostellar core and its host
luminosity peak.
Note (6): Temperature measured in the PPMAP dust temperature image at core
location, and its error, corresponding to the background-diluted core
temperature, mass-averaged up to a 1.25" radius (see Sect 3.1).
Note (7): Contribution level of each protostellar core to their associated
luminosity peak, estimated in Sect 4.3.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Protocluster Protocluster name in the ALMA-IMF sample
9- 11 A3 --- LPeak Luminosity peak identifier (1)
13- 21 F9.5 deg RAdeg Right ascension (ICRS) (1)
23- 31 F9.5 deg DEdeg Declination (ICRS) (1)
33- 36 F4.2 10+3Lsun Lbol Integrated luminosity (1)
38- 41 F4.2 10+3Lsun e_Lbol Integrated luminosity error (1)
43- 45 F3.1 arcsec thetaLbol Mean full width at half maximum of
the luminosity peak (1)
47- 50 F4.1 kau FWHMLbol Mean full width at half maximum of
the luminosity peak (1)
52- 54 A3 --- Tpeak? [yes/ no] Presence or absence of
temperature peak (2)
56- 58 I3 --- N Protostellar core identifier (2)
59 A1 --- n_N [*] *: protostellar cores are tentative
61- 64 F4.2 arcsec thetacore Mean full width at half maximum of the
core, in arcsec (2)
66- 69 F4.2 arcsec DLbol Distance between the centers of the
protostellar core and its host
luminosity peak
71- 72 I2 K PPMAPTdust Dust temperature measured in the PPMAP
temperature image
74 I1 K e_PPMAPTdust Temperature error measured in the error
image of the PPMAP temperature
76- 78 I3 % ContribL Contribution level of each protostellar
core to their associated luminosity peak
--------------------------------------------------------------------------------
Note (1): Luminosity peak name, RA and Dec peak coordinates, integrated
luminosity and its error, and mean FWHM angular and spatial sizes.
Values are taken and computed from the catalog obtained in Sect 2.2.
Note (2): Protostellar cores associated with the luminosity peak of LPeak
have their centers inside the ellipse describing the FWHM of the luminosity
peak.
ID numbers and FWHM angular sizes of protostellar cores are taken from the
catalog of Armante et al. 2024A&A...686A.122A 2024A&A...686A.122A (see Sect. 2.1).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Protocluster Protocluster name in the ALMA-IMF sample
10- 15 A6 --- LProfile Luminosity profile named after methyl
formate sources (1)
17- 18 I2 h RAh Right ascension of the profile center
(ICRS) (1)
20- 21 I2 min RAm Right ascension of the profile center
(ICRS) (1)
23- 27 F5.2 s RAs Right ascension of the profile center
(ICRS) (1)
29 A1 --- DE- Declination sign of the profile center
(ICRS) (1)
30- 31 I2 deg DEd Declination of the profile center
(ICRS) (1)
33- 34 I2 arcmin DEm Declination of the profile center
(ICRS) (1)
36- 40 F5.2 arcsec DEs Declination of the profile center
(ICRS) (1)
42- 45 F4.1 10+3Lsun LMFpeak Luminosity estimated using luminosity
peaks (lower limit) (2)
47- 50 F4.1 10+3Lsun e_LMFpeak Error of the luminosity estimated using
luminosity peaks (2)
52- 54 I3 10+3Lsun LMFpow Luminosity estimated by integrating the
power-law component of the profile (2)
56- 57 I2 10+3Lsun e_LMFpow Error of the luminosity estimated by
integrating the power-law component of
the profile (2)
59- 61 I3 10+3Lsun LMFtot Luminosity estimated by integrating the
total profile (upper limit) (2)
63- 64 I2 10+3Lsun e_LMFtot Error of the luminosity estimated by
integrating the total profile (2)
66- 67 I2 --- N Protostellar core identifier (3)
68 A1 --- n_N [*] *: protostellar cores are tentative
70- 72 I3 % ContribLMF Contribution level to the hot core
luminosity (3)
74- 77 F4.1 10+3Lsun Lprotopow Luminosity computed from
LMFpow and ContribLMF (3)
79- 82 F4.1 10+3Lsun e_Lprotopow Luminosity error computed from
e_LMFpeak and ContribLMF (3)
84- 86 I3 K TLproto Temperature estimated from LMFpeak
(lower limit) (4)
88 I1 K e_TLproto Temperature error estimated from
e_LMFpeak (4)
90- 92 I3 K TLprotopow Temperature estimated from LMFpow (4)
94 I1 K e_TLprotopow Temperature error estimated from
e_LMFpow (4)
96- 98 I3 K TLprototot Temperature estimated from
LMFtot (upper limit) (4)
100 I1 K e_TLprototot Temperature error estimated from
e_LMFtot (4)
--------------------------------------------------------------------------------
Note (1): Name, RA and Dec coordinates of the four locations around which the
luminosity profiles, presented in Fig. D.2, are built to characterize the six
brightest methyl formate (MF) sources of the ALMA-IMF survey Bonfand et al.
2024A&A...687A.163B 2024A&A...687A.163B, encompassing eight protostellar cores.
Note (2): Three luminosity estimates, and their errors, for these extreme hot
cores, derived from the luminosity peak (lower limit), integration of the
power-law component of the profile, and total integration of the profile
(upper limit).
Note (3): The eight protostellar cores, located within the extent of the six
brightest MF sources of ALMA-IMF, their contribution to the hot core
luminosity, their luminosity and their error computed from LMF(pow)-e_LMF(pow)
and ContribLMF in Sect. 4.3.
Note (4): Dust temperature and its error of the protostellar cores, which is
estimated from LMFpeak, e_LMFpeak, LMFpow, e_LMFpow, LMFtot, e_LMFtot,
ContribLMF and the core size of tablec8.dat.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Protocluster Protocluster name in the ALMA-IMF
sample (1)
9- 11 I3 --- N Protostellar core identifier
12 A1 --- n_N [*] *: protostellar cores are tentative
14- 17 I4 au Rout Outer radius of the protostellar core (3)
19- 22 F4.2 10+3Lsun Lproto ?=- Protostellar luminosity (4)
24- 27 F4.2 10+3Lsun e_Lproto ?=- Protostellar luminosity error (4)
29- 30 I2 K TcorePPMAP Mass-averaged dust temperature of
protostellar cores estimated from the
PPMAP temperature (5)
32- 33 I2 K e_TcorePPMAP Error on the mass-averaged temperature of
protostellar cores estimated from the
PPMAP temperature (5)
35- 36 I2 K TcoreLproto ?=- Mass-averaged dust temperature of
protostellar cores estimated from
Rout and Lproto (6)
38 I1 K e_TcoreLproto ?=- Error on the mass-averaged dust
temperature of protostellar cores
estimated from Rout, Lproto and
e_Lproto (6)
40- 41 I2 K MeanTcore Average dust temperature of protostellar
cores from TcorePPMAP and TcoreLproto
(7)
43- 44 I2 K e_MeanTcore Error on the average dust temperature of
protostellar cores, using TcorePPMAP,
e_TcorePPMAP, TcoreLproto and
e_TcoreLproto (7)
46- 50 F5.1 Msun Mass Protostellar core mass (8)
52- 55 F4.1 Msun e_Mass Error on the protostellar core mass (8)
57- 79 A23 --- Comments Comments on the core nature (9)
--------------------------------------------------------------------------------
Note (1): Protostellar core ID numbers.
Note (3): Outer radius of protostellar cores, assumed to be equal to their FWHM
(theta_core of tablec1.dat or tablec2.dat), deconvolved by the beam and
set at their distance to the Sun (Motte et al., 2022A&A...662A...8M 2022A&A...662A...8M).
Note (4): Protostellar luminosity, and its error, estimated from their
luminosity contribution to their host PPMAP luminosity peak (Lbol, e_Lbol and
ContribL of tablec1.dat or tablec2.dat) in Sect. 4.3.
Note (5): Mass-averaged temperature of protostellar cores, and its error,
estimated from the PPMAP temperature (PPMAPTdust and ePPMAPTdust of
tablec1.dat.cds or tablec2.dat) and outer radius (Rout) in Sect. 4.2.
Note (6): Mass-averaged dust temperature of protostellar cores, and its error,
estimated from their outer radius and protostellar luminosity (Rout, Lproto
and e_Lproto) in Sect. 4.1.
Note (7): Average value of the dust temperatures, and its error, taken from
TcorePPMAP, e_TcorePPMAP, TcoreLproto and e_TcoreLproto).
Note (8): Mass of protostellar cores and its error computed from its 1.3mm
(peak and integrated) fluxes measured in the catalogs of Pouteau et al.
2022A&A...664A..26P 2022A&A...664A..26P, Cat. J/A+A/664/A26, Nony et al. 2023A&A...674A..75N 2023A&A...674A..75N,
Cat. J/A+A/674/A75, and Armante et al. 2024A&A...686A.122A 2024A&A...686A.122A, and the
temperature and error of MeanTcore and e_MeanTcore in Eq. 11. When necessary,
fluxes have been corrected for contamination by free-free and line emission.
Note (9): Protostellar cores driving an outflow (tag "O", Nony et al.
2020A&A...636A..38N 2020A&A...636A..38N, Cat. J/A+A/636/A38, Nony et al. 2023A&A...674A..75N 2023A&A...674A..75N,
Cat. J/A+A/674/A75,, Nony in prep., Valeille et al. 2024), coincident with a
hot core candidate (tag "hot-core", Bonfand et al. 2024A&A...687A.163B 2024A&A...687A.163B),
and/or whose flux is corrected for contamination by free-free emission
(tag "FF corrected", Armante et al. 2024A&A...686A.122A 2024A&A...686A.122A).
Masses are uncertain when the core flux is corrected for free-free
contamination.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Protocluster Protocluster name in the ALMA-IMF sample
10- 12 I3 --- N Prestellar core identifier (1)
14- 17 I4 au Rout Outer radius of the prestellar core (1)
19- 20 I2 K PPMAPTdust Dust temperature measured in the PPMAP
temperature image (2)
22- 23 I2 K e_PPMAPTdust Temperature error measured in the error
image of the PPMAP temperature (2)
25- 26 I2 K Tcore Mass-averaged temperature of prestellar
cores estimated from PPMAPTdust (3)
28- 29 I2 K e_Tcore Mass-averaged temperature error of
prestellar cores estimated from
e_PPMAPTdust (3)
31- 34 F4.1 Msun Mass Prestellar core mass (4)
36- 38 F3.1 Msun e_Mass Error on the prestellar core mass (4)
--------------------------------------------------------------------------------
Note (1): ID numbers and outer radius of prestellar cores, assumed to be equal
to their FWHM deconvolved by the beam and set at their distance to the Sun
(Motte et al. 2022A&A...662A...8M 2022A&A...662A...8M), are taken from the catalogs of
Pouteau et al. 2022A&A...664A..26P 2022A&A...664A..26P, Cat. J/A+A/664/A26, Nony et al.
2023A&A...674A..75N 2023A&A...674A..75N, Cat. J/A+A/674/A75, Armante et al. 2024A&A...686A.122A 2024A&A...686A.122A,
and Louvet et al. 2024A&A...690A..33L 2024A&A...690A..33L, Cat. J/A+A/690/A33 (see Sect. 2.1).
Note (2): Temperature measured in the PPMAP dust temperature image at core
location, and its error, corresponding to the background-diluted core
temperature, mass-averaged up to a 1.25" radius (see Sect 3.1).
Note (3): Mass-averaged temperature of prestellar cores, and its error,
estimated from Sect. 5.2 using Rout, PPMAPTdust and e_PPMAPTdust.
Note (4): Mass of prestellar cores and its error computed from the fluxes
measured in the catalogs listed in Sect. 2.1 and the temperature and its error
taken from Tcore and e_Tcore in Eq. 11.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Protocluster Protocluster name in the ALMA-IMF sample
9- 11 A3 --- LPeak Luminosity peak identifier (1)
13- 17 F5.2 10+3Lsun Lbol Integrated luminosity (1)
19- 23 F5.2 10+3Lsun e_Lbol Integrated luminosity error (1)
25- 27 F3.1 arcsec thetaLbol Mean full width at half maximum of the
luminosity peak, in arcsec (1)
29- 32 F4.1 kau FWHMLbol Mean full width at half maximum of the
luminosity peak, in kau (1)
34- 36 A3 --- Tpeak? [yes/no ] Presence or absence of
temperature peak (2)
38- 39 I2 --- N Protostellar core identifier (3)
40 A1 --- n_N [*] *: protostellar cores are tentative
42- 45 F4.2 arcsec thetacore Mean full width at half maximum of the
core, in arcsec (3)
47- 50 F4.2 arcsec DLbol Distance between the centers of the
protostellar core and its host
luminosity peak (4)
52- 53 I2 K PPMAPTdust Dust temperature measured in the PPMAP
temperature image (5)
55- 56 I2 K e_PPMAPTdust Temperature error measured in the error
image of the PPMAP temperature (5)
58- 60 I3 % ContribL Contribution level of each protostellar
core to their associated luminosity
peak (6)
--------------------------------------------------------------------------------
Note (1): Luminosity peak name, integrated luminosity and its error, and mean
FWHM sizes. Values are taken or computed from Table B.1 of Dell'Ova et al.,
2024A&A...687A.217D 2024A&A...687A.217D, Cat. J/A+A/687/A217.
Note (2): Presence or absence of a temperature peak detected in the ellipse
describing the FWHM of the luminosity peak.
Note (3): Protostellar cores associated with the luminosity peak of LPeak have
their centers inside the ellipse describing the FWHM of the luminosity peak.
ID numbers and FWHM angular sizes of protostellar cores are taken from the
catalog of Louvet et al. 2024A&A...690A..33L 2024A&A...690A..33L, Cat. J/A+A/690/A33
(see Sect. 2.1).
Note (4): Distance between the centers of the protostellar core and its host
luminosity peak.
Note (5): Temperature measured in the PPMAP dust temperature image at core
location, and its error, corresponding to the background-diluted core
temperature, mass-averaged up to a 1.25" radius (see Sect 3.1).
Note (6): Contribution level of each protostellar core to their associated
luminosity peak, estimated in Sect. 4.3.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Protocluster Protocluster name in the ALMA-IMF sample
10- 12 A3 --- LPeak Luminosity peak identifier (1)
14- 22 F9.5 deg RAdeg Right ascension (ICRS) (1)
24- 32 F9.5 deg DEdeg Declination (ICRS) (1)
34- 38 F5.2 10+3Lsun Lbol Integrated luminosity (1)
40- 43 F4.2 10+3Lsun e_Lbol Integrated luminosity error (1)
45- 47 F3.1 arcsec thetaLbol Mean full width at half maximum of the
luminosity peak (1)
49- 52 F4.1 kau FWHMLbol Mean full width at half maximum of the
luminosity peak (1)
54- 56 A3 --- Tpeak? [yes/no ] Presence or absence of
temperature peak
58- 60 I3 --- N Protostellar core identifier
61 A1 --- n_N [*]
63- 66 F4.2 arcsec thetacore Mean full width at half maximum of the
core, in arcsec
68- 71 F4.2 arcsec DLbol Distance between the centers of the
protostellar core and its host
luminosity peak
73- 74 I2 K PPMAPTdust Dust temperature measured in the PPMAP
temperature image
76- 77 I2 K e_PPMAPTdust Temperature error measured in the error
image of the PPMAP temperature
79- 81 I3 % ContribL Contribution level of each protostellar
core to their associated luminosity peak
--------------------------------------------------------------------------------
Note (1): Luminosity peak name, RA and Dec peak coordinates, integrated
luminosity and its error, and mean FWHM angular sizes. Values are taken and
computed from the catalog obtained in Sect. 2.2. For other columns see
tablec6.dat.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Protocluster Protocluster name in the ALMA-IMF sample
10- 12 I3 --- N Protostellar core identifier (1)
13 A1 --- n_N [*] *: tentative protostellar cores
15- 18 I4 au Rout Outer radius of the protostellar core (2)
20- 24 F5.2 10+3Lsun Lproto ?=- Protostellar luminosity estimate (3)
26- 30 F5.2 10+3Lsun e_Lproto ?=- Protostellar luminosity error
estimate (3)
32- 34 I3 K TcorePPMAP Mass-averaged temperature of protostellar
cores estimated from the PPMAP
temperature (4)
36- 37 I2 K e_TcorePPMAP Error on the mass-averaged temperature of
protostellar cores estimated from the
PPMAP temperature (4)
39- 41 I3 K TcoreLproto ?=- Mass-averaged dust temperature of
protostellar cores estimated from
Rout and Lproto (5)
43 I1 K e_TcoreLproto ?=- Error on the mass-averaged dust
temperature of protostellar cores
estimated from Rout, Lproto and
e_Lproto (5)
45- 47 I3 K MeanTcore Average dust temperature of protostellar
cores from TcorePPMAP and TcoreLproto
(6)
49- 50 I2 K e_MeanTcore Error on the average dust temperature of
protostellar cores, using TcorePPMAP,
e_TcorePPMAP, TcoreLproto and
e_TcoreLproto (6)
52 A1 --- l_Mass Limit flag on Mass
53- 57 F5.1 Msun Mass ?=- Protostellar core mass (7)
59- 62 F4.1 Msun e_Mass ?=- Error on the protostellar
core mass (7)
64- 86 A23 --- Comments Comments on the core nature (8)
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Note (1): Protostellar core ID numbers.
Note (2): Outer radius of protostellar cores, assumed to be equal to their FWHM
(thetacore of tablec6.dat or tablec7.dat), deconvolved by the beam and
set at their distance to the Sun (Motte et al. 2022A&A...662A...8M 2022A&A...662A...8M).
Note (3): Protostellar luminosity, and its error, estimated from their
luminosity contribution to their host PPMAP luminosity peak (Lbol, e_Lbol and
ContribL of tablec6.dat or tablec7.dat) in Sect. 4.3.
Note (4): Mass-averaged temperature of protostellar cores, and its error,
estimated from the PPMAP temperature (PPMAPTdust and e_PPMAPTdust of
tablec6.dat or tablec7.dat) and outer radius (Rout) in Sect. 4.2.
Note (5): Mass-averaged dust temperature of protostellar cores, and its error,
estimated from their outer radius and protostellar luminosity (Rout, Lproto
and e_Lproto) Sect. 4.1.
Note (6): Average value of the dust temperatures, and its error, taken from
TcorePPMAP, e_TcorePPMAP, TcoreLproto and e_TcoreLproto.9.
Note (7): Mass of protostellar cores and its error computed from its 1.3mm
(peak and integrated) fluxes measured in the catalogs of Pouteau et al.
2022A&A...664A..26P 2022A&A...664A..26P, Cat. J/A+A/664/A26, Nony et al. 2023A&A...674A..75N 2023A&A...674A..75N,
and Armante et al. 2024A&A...686A.122A 2024A&A...686A.122A, and the temperature and error of
MeanTcore and e_MeanTcore in Eq. 11. When necessary, fluxes have been
corrected for contamination by free-free and line emission.
Note (8): Protostellar cores driving an outflow (tag "O", Nony et al.
2020A&A...636A..38N 2020A&A...636A..38N, Cat. J/A+A/636/A38, Nony et al. 2023A&A...674A..75N 2023A&A...674A..75N,
Valeille-Manet et al., 2024, in prep.), coincident with a hot core candidate
(tag "hot-core", Bonfand et al. 2024A&A...687A.163B 2024A&A...687A.163B), and/or whose flux is
corrected for contamination by free-free emission (tag "FF corrected",
Armante et al. 2024A&A...686A.122A 2024A&A...686A.122A).
Masses are uncertain when the core flux is corrected for free-free
contamination.
--------------------------------------------------------------------------------
Acknowledgements:
Frederique Motte, frederique.motte(at)univ-grenoble-alpes.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
Towner et al., Paper IX 2024ApJ...960...48T 2024ApJ...960...48T
Armante et al., Paper X 2024A&A...686A.122A 2024A&A...686A.122A
Bonfand et al., Paper XI 2024A&A...687A.163B 2024A&A...687A.163B
Dell'Ova et al., Paper XII 2024A&A...687A.217D 2024A&A...687A.217D, Cat. J/A+A/687/A217
Alvarez-Gutierrez et al., Paper XIII 2024A&A...689A..74A 2024A&A...689A..74A
Galvan-Madrid et al., Paper XIV 2024ApJS..274...15G 2024ApJS..274...15G
Louvet et al., Paper XV 2024A&A...690A..33L 2024A&A...690A..33L, Cat. J/A+A/690/A33
(End) Patricia Vannier [CDS] 06-Jan-2025