2019ApJ...873...31K


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.16CEST11:25:33

2019ApJ...873...31K - Astrophys. J., 873, 31-31 (2019/March-1)

The core mass function in the infrared dark cloud G28.37+0.07.

KONG S.

Abstract (from CDS):

In this paper, we analyze the 1.3 mm continuum ALMA data that cover the majority of the infrared dark cloud (IRDC) G28.37+0.07. With a spatial resolution of 0.''5 (2500 au at 5 kpc), the continuum image reveals five groups of dense cores. Each core group has a projected physical scale of about 1 pc, with core masses spanning a dynamic range of about 100. We use the dendrogram method (astrodendro) and a newly developed graph method (astrograph) to identify individual cores. The core masses are estimated through the millimeter continuum flux, assuming constant temperature and using an NH3-based gas temperature. We construct core mass functions (CMFs) based on the two methods and fit a power-law relation dN/d log M ∝ M–α to the CMFs for M > 0.79 M. In the constant-temperature scenario, astrograph gives α = 0.80 ± 0.10, while astrodendro gives α = 0.71 ± 0.11, both significantly shallower than the Salpeter-type initial mass function with α = 1.35. In the scenario where the NH3 gas temperature is applied to cores, astrograph gives α = 1.37 ± 0.06, while astrodendro gives α = 0.87 ± 0.07. Regional CMF slope variation is seen between the core groups. We also compare CMFs in three different environments, including IRDC G28.37+0.07, IRDC clumps, and G286.21+0.17, using the identical dendrogram method. Results show that IRDCs have smaller α than the cluster-forming cloud G286.21+0.17.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): dust, extinction - ISM: clouds - ISM: structure - stars: formation - stars: luminosity function, mass function - stars: protostars

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1131 0
2 NAME f-Shaped Filament in Orion Cld 05 35.0 -05 30           ~ 77 0
3 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1217 0
4 NAME Orion A South MoC 05 43.0 -08 40           ~ 15 0
5 [DBS2003] 127 cor 10 38 33 -58 19.3           ~ 20 0
6 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3156 1
7 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 351 1
8 SDC G14.225-0.506 DNe 18 18 11.49 -16 49 29.6           ~ 18 0
9 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 967 2
10 NAME Serpens Core CD Cluster Cl* 18 29 52 +01 15.4           ~ 25 0
11 AGAL G028.364+00.121 cor 18 42 40.01 -04 00 34.4           ~ 24 0
12 [TKZ2016] C1-Sa Y*O 18 42 46.442901 -04 04 14.94456           ~ 10 0
13 AGAL G028.324+00.067 Y*O 18 42 46.7 -04 04 08           ~ 44 0
14 AGAL G028.354+00.072 MoC 18 42 49.34 -04 02 27.3           ~ 28 0
15 AGAL G028.344+00.061 cor 18 42 50.45 -04 03 17.7           ~ 71 0
16 NAME Dragon Nebula DNe 18 42 50.6 -04 03 30           ~ 122 0
17 AGAL G028.398+00.081 cor 18 42 51.86 -03 59 43.3           ~ 45 0
18 [RJS2006] MSXDC G028.37+00.07 MM14 MoC 18 42 52.59 -04 02 44.3           ~ 14 0
19 AGAL G028.361+00.054 cor 18 42 54.37 -04 02 31.7           ~ 27 1
20 AGAL G028.388+00.037 MoC 18 42 59.99 -04 01 33.1           ~ 21 0
21 AGAL G030.818-00.056 cor 18 47 47.0 -01 54 28           ~ 117 0

    Equat.    Gal    SGal    Ecl

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2021.04.16-11:25:33

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