2009A&A...503..859B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST23:13:58

2009A&A...503..859B - Astronomy and Astrophysics, volume 503, 859-867 (2009/9-1)

Multiple low-turbulence starless cores associated with intermediate- to high-mass star formation.

BEUTHER H. and HENNING T.

Abstract (from CDS):

Characterizing the gas and dust properties prior to and in the neighborhood of active intermediate- to high-mass star formation. Two Infrared Dark Clouds (IRDCs) - IRDC19175-4 and IRDC19175-5 - that are located in the vicinity of the luminous massive star-forming region IRAS19175+1357, but that remain absorption features up to 70µm wavelength, were observed with the Plateau de Bure Interferometer in the 3.23mm dust continuum as well as the N2H+(1-0) and 13CS(2-1) line emission. While IRDC19175-4 is clearly detected in the 3.23mm continuum, the second source in the field, IRDC19175-5, is only barely observable above the 3σ continuum detection threshold. However, the N2H+(1-0) observations reveal 17 separate sub-sources in the vicinity of the two IRDCs. Most of them exhibit low levels of turbulence (Δv≤1km/s), indicating that the fragmentation process in these cores may be dominated by the interplay of thermal pressure and gravity, but not so much by turbulence. Combining the small line widths with the non-detection up to 70µm and the absence of other signs of star formation activity, most of these 17 cores with masses between sub-solar to ∼10M are likely still in a starless phase. The N2H+ column density analysis indicates significant abundance variations between the cores. Furthermore, we find a large CS depletion factor of the order 100. Although the strongest line and continuum peak is close to virial equilibrium, its slightly broader line width compared to the other cores is consistent with it being in a contraction phase potentially at the verge of star formation. Based on the 3.23mm upper limits, the other cores may be gravitationally stable or even transient structures. The relative peak velocities between neighboring cores are usually below 1km/s, and we do not identify streaming motions along the filamentary structures. Average densities are between 105 and 106cm–3 (one to two orders of magnitude larger than for example in the Pipe nebula) implying relatively small Jeans-lengths that are consistent with the observed core separations of the order 5000AU. Environmental reasons potentially determining these values are discussed. These observations show that multiple low- to intermediate-mass low-turbulence starless cores can exist in the proximity of more turbulent active intermediate- to high-mass star-forming regions. While masses and levels of turbulence are consistent with low-mass starless core regions, other parameters like the densities or Jeans-lengths differ considerably. This may be due to environmental effects. The quest for high-mass starless cores prior to any star formation activity remains open.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: individual: IRDC19175-4, IRDC19175-5 - techniques: interferometric - line: formation - line: profiles - turbulence

VizieR on-line data: <Available at CDS (J/A+A/503/859): maps.dat fig/*>

CDS comments: Paragraph.3.3 L1571E is a probable misprint for LDN 1521E.

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME [BM89] L1521E DNe 04 29 21.0 +26 14 19           ~ 85 1
2 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2001 1
3 NGC 1985 RNe 05 37 47.8 +31 59 24           ~ 130 2
4 NAME NGC 6334-I Cl* 17 20 53.35 -35 47 01.5           ~ 269 0
5 OH 351.41 +0.64 Mas 17 20 53.4 -35 47 01           ~ 58 1
6 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 333 1
7 ICRF J183005.9+061915 QSO 18 30 05.9399600344 +06 19 15.947596681       19.5   ~ 71 1
8 NAME Dragon Nebula DNe 18 42 50.6 -04 03 30           ~ 112 0
9 [PWC2006] NH3 G28.34+0.06 P1 cor 18 42 50.9 -04 03 14           ~ 37 0
10 IRAS 19175+1357 cor 19 19 49.22 +14 02 46.8           ~ 26 0
11 [BSM2002] 19175+1357 5 cor 19 19 49.59 +14 01 08.7           ~ 2 0
12 [BSM2002] 19175+1357 4 cor 19 19 50.58 +14 01 22.4           ~ 7 0
13 [VV2006] J192332.2-210433 QSO 19 23 32.18981466 -21 04 33.3330547   15.32 17.50 16.70   ~ 125 2
14 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 707 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-23:13:58

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