2007MNRAS.379.1390S


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.29CET01:33:15

2007MNRAS.379.1390S - Mon. Not. R. Astron. Soc., 379, 1390-1400 (2007/August-3)

The dust temperatures of the pre-stellar cores in the ρ Oph main cloud and in other star-forming regions: consequences for the core mass function.

STAMATELLOS D., WHITWORTH A.P. and WARD-THOMPSON D.

Abstract (from CDS):

We estimate the dust temperatures of the clumps in the ρ Oph main cloud taking into account the 3D geometry of the region, and external heating from the interstellar radiation field and from HD 147879, a nearby luminous B2V star, which is believed to dominate the radiation field in the region. We find that the regions where pre-stellar cores are observed (i.e. at optical visual extinctions >7 mag) are colder than ∼10 -11 K. These dust temperatures are smaller than those which previous studies of the same region have assumed. We use the new dust temperatures to estimate the masses of the pre-stellar cores in the ρ Oph main cloud from millimetre observations, and we find core masses that are larger than previous estimates by a factor of ∼2 -3. This affects the core mass function (CMF) of the region; we find that the mass at which the core mass spectrum steepens from a slope α ∼ 1.5 to a slope α ∼ 2.5 has moved from ∼0.5 to ∼1M. In contrast with the CMF in other star-forming regions (e.g. Orion), there is no indication for a turnover down to the completeness limit (∼0.2M), but the CMF may flatten at around ∼0.4M.

We generalize our results to the pre-stellar cores in Taurus and in Orion. In Taurus, the ambient radiation field heating the pre-stellar cores is believed to be weaker than that in ρ Oph. Hence, the dust temperatures of the cores in Taurus are expected to be below ∼10 -11 K. In Orion, the radiation field is believed to be 103 times stronger than the standard interstellar radiation field. Based on this assumption, we estimate that the dust temperatures of the pre-stellar cores in Orion are around ∼20 -30 K.


Abstract Copyright: 2007 The Authors. Journal compilation © 2007 RAS

Journal keyword(s): radiative transfer - methods: numerical - stars: formation - ISM: clouds - dust, extinction - ISM: structure

CDS comments: IRS43 = WLY 2-43

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 HD 14789 * 02 22 15.2899323687 -31 02 46.922891610   10.34 9.19     K1III 8 0
2 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3575 0
3 Barnard 220 DNe 04 41 38.8 +26 00 42           ~ 122 0
4 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 491 0
5 M 42 HII 05 35 17.3 -05 23 28           ~ 3756 0
6 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 868 1
7 HD 147889 pr* 16 25 24.3162969787 -24 27 56.570239619 8.56 8.73 7.90     B2III/IV 439 1
8 NAME rho Oph A Cloud MoC 16 26 26.4 -24 22 33           ~ 241 1
9 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 375 0
10 [SSG2006] MMS002 smm 16 26 26.50 -24 24 30.9           ~ 241 0
11 NAME rho Oph C Cloud MoC 16 26 53.1 -24 32 31           ~ 57 0
12 NAME rho Oph E MoC 16 27 02.0 -24 38 31           ~ 56 0
13 HD 147879 * 16 27.1 -52 24   11.1 11.0     A0 3 0
14 NAME rho Oph B Cloud MoC 16 27 11 -24 28.5           ~ 67 1
15 YLW 15 Y*O 16 27 26.93640 -24 40 50.8224           ~ 241 1
16 NAME rho Oph B2 Cloud PoC 16 27 27.9 -24 26 29           ~ 75 1
17 NAME rho Oph F MoC 16 27 37.3 -24 42 28           ~ 58 0
18 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3086 0
19 NAME Ophiuchus D MoC 16 28 29.2 -24 18 25           ~ 105 0
20 LDN 1689 DNe 16 32 22.5 -24 28 29           ~ 110 0
21 LDN 57 DNe 17 22 38.2 -23 49 34           ~ 284 1

    Equat.    Gal    SGal    Ecl

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2020.11.29-01:33:15

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