J/MNRAS/496/3482 Accretion history of massive stars (Peretto+, 2020)
The accretion history of high-mass stars:
an ArTeMiS pilot study of infrared dark clouds
Peretto N., Rigby A., Andre P., Konyves V., Fuller G., Zavagno A.,
Schuller F., Arzoumanian D., Bontemps S., Csengeri T., Didelon P.,
Duarte-Cabral A., Palmeirim P., Pezzuto S., Reveret V., Roussel H.,
Shimajiri Y.
<Mon. Not. R. Astron. Soc. 496, 3482-3501 (2020)>
=2020MNRAS.496.3482P 2020MNRAS.496.3482P (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds ; Infrared sources ;
Photometry, millimetric/submm ; Stars, masses
Keywords: accretion - stars: protostars stars: formation -
Abstract:
The mass growth of protostars is a central element to the
determination of fundamental stellar population properties such as the
initial mass function. Constraining the accretion history of
individual protostars is therefore an important aspect of star
formation research. The goal of the study presented here is to
determine whether high-mass (proto)stars gain their mass from a
compact (<0.1pc) fixed-mass reservoir of gas, often referred to as
dense cores, in which they are embedded, or whether the mass growth of
high-mass stars is governed by the dynamical evolution of the
parsec-scale clump that typically surrounds them. To achieve this
goal, we performed a 350micron continuum mapping of 11 infrared dark
clouds, along side some of their neighbouring clumps, with the ArTeMiS
camera on APEX. By identifying about 200 compact ArTeMiS sources, and
matching them with Herschel Hi-GAL 70micron sources, we have been able
to produce mass vs. temperature diagrams. We compare the nature (i.e.
starless or protostellar) and location of the ArTeMiS sources in these
diagrams with modelled evolutionary tracks of both core-fed and
clump-fed accretion scenarios. We argue that the latter provide a
better agreement with the observed distribution of high-mass
star-forming cores. However, a robust and definitive conclusion on the
question of the accretion history of high-mass stars requires larger
number statistics.
Description:
This table presents the properties of each of 203 compact ArTeMiS
sources identified in the images analysed in the paper. These sources
have been identified across 5 fields: SDC326, SDC328, SDC340, SDC343,
SDC345.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 123 203 Properties of the 203 ArTeMiS compact sources
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See also:
J/A+A/565/A75 : ATLASGAL: dust condensations in Galactic plane
(Csengeri+, 2014)
J/MNRAS/471/100 : Hi-GAL compact source catalog. -71.0<l<67.0 (Elia+, 2017)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Name Field name (SDC326,SDC328,SDC340,SDC343,SDC345)
9- 11 I3 --- ID Identification number of the ArTeMiS source
14- 21 F8.4 deg GLON Galactic longitude
24- 30 F7.4 deg GLAT Galactic latitude
33- 37 F5.1 Jy/beam Sp Peak ArTeMiS 350micron flux density
40- 43 F4.1 Jy/beam e_Sp Uncertainty on Sp
46- 50 F5.1 Jy/beam Spf Filtered ArTeMiS 350micron flux density
53- 56 F4.1 Jy/beam e_Spf Uncertainty on Spf
59- 63 F5.1 K Td Dust temperature of source on 0.1pc scale
66- 69 F4.1 K e_Td Uncertainty on Td
72- 76 F5.1 Msun M Mass of the ArTeMiS source on 0.1pc scale
79 A1 --- --- [-] Sign of the lower bound uncertainty on M
80- 83 F4.1 Msun e_M Lower bound uncertainty on M
86 A1 --- --- [+] Sign of the upper bound uncertainty on M
87- 90 F4.1 Msun E_M Upper bound uncertainty on M
93- 98 F6.2 10+3Lsun Lint Internal luminosity of the ArTeMiS source
101 A1 --- --- [-] Sign of the lower bound uncertainty on Lint
102-106 F5.2 10+3Lsun e_Lint Lower bound uncertainty on Lint
109 A1 --- --- [+] Sign of the upper bound uncertainty on Lint
110-114 F5.2 10+3Lsun E_Lint Upper bound uncertainty on Lint
117 A1 --- Hcl [y/n] Association with Herschel clump (1)
120 A1 --- Atl [y/n] Association with ATLASGAL clump (2)
123 A1 --- IRvisu [y/n] IR source association (3)
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Note (1): Association with Herschel clump flag as follows:
y = ArTeMiS source is associated with a Herschel clump from
Elia et al., 2017, Cat. J/MNRAS/471/100
n = ArTeMiS source is not associated with a Herschel clump from
Elia et al., 2017, Cat. J/MNRAS/471/100
Note (2): Association with ATLASGAL clump flag as follows:
y = ArTeMiS source is associated with a ATLASGAL clump from
Csengeri et al., 2014, Cat. J/A+A/565/A75
n = ArTeMiS source is not associated with a ATLASGAL clump from
Csengeri et al., 2014, Cat. J/A+A/565/A75
Note (3): IR source association flag as follows:
y = ArTeMiS source is visually associated with a Herschel 70micron and/or
Spitzer 8micron source
n = ArTeMiS source is not visually associated with a Herschel 70micron and/or
Spitzer 8micron source
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Acknowledgements:
Nicolas Peretto, nicolas.peretto(at)astro.cf.ac.uk
(End) Nicolas Peretto [Cardiff Univ., UK], Patricia Vannier [CDS] 29-Jun-2020