2013A&A...550A..10L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST20:37:35

2013A&A...550A..10L - Astronomy and Astrophysics, volume 550A, 10-10 (2013/2-1)

The distribution of warm gas in the G327.3-0.6 massive star-forming region.

LEURINI S., WYROWSKI F., HERPIN F., VAN DER TAK F., GUESTEN R. and VAN DISHOECK E.F.

Abstract (from CDS):

Most studies of high-mass star formation focus on massive and/or luminous clumps, but the physical properties of their larger scale environment are poorly known. In this work, we aim at characterising the effects of clustered star formation and feedback of massive stars on the surrounding medium by studying the distribution of warm gas through mid-J 12CO and 13CO observations. We present APEX 12CO(6-5), (7-6), 13CO(6-5), (8-7) and HIFI 13CO(10-9) maps of the star forming region G327.36-0.6 with a linear size of ∼3pcx4pc. We infer the physical properties of the emitting gas on large scales through a local thermodynamic equilibrium analysis, while we apply a more sophisticated large velocity gradient approach on selected positions. Maps of all lines are dominated in intensity by the photon dominated region around the HII region G327.3-0.5. Mid-J 12CO emission is detected over the whole extent of the maps with excitation temperatures ranging from 20K up to 80K in the gas around the HII region, and H2 column densities from few 1021cm–2 in the inter-clump gas to 3x1022/cm2 towards the hot core G327.3-0.6. The warm gas (traced by 12 and 13CO(6-5) emission) is only a small percentage (∼10%) of the total gas in the infrared dark cloud, while it reaches values up to ∼35% of the total gas in the ring surrounding the HII region. The 12CO ladders are qualitatively compatible with photon dominated region models for high density gas, but the much weaker than predicted 13CO emission suggests that it comes from a large number of clumps along the line of sight. All lines are detected in the inter-clump gas when averaged over a large region with an equivalent radius of 50"(∼0.8pc), implying that the mid-J 12CO and 13CO inter-clump emission is due to high density components with low filling factor. Finally, the detection of the 13CO(10-9) line allows to disentangle the effects of gas temperature and gas density on the CO emission, which are degenerate in the APEX observations alone.

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Journal keyword(s): stars: formation - HII regions - ISM: individual objects: G327.3-0.6

Simbad objects: 9

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Number of rows : 9

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 OMC-1 MoC 05 35 14 -05 22.4           ~ 1015 2
2 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2001 1
3 M 42 HII 05 35 17.3 -05 23 28           ~ 3724 0
4 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 716 0
5 [MAB2009] SMM6 cor 15 53 00.9 -54 37 40           ~ 3 0
6 GAL 327.30-00.60 HII 15 53 05.0 -54 35 24           ~ 122 0
7 SSTGLMC G327.3009-00.5791 AB? 15 53 11.18568 -54 36 48.4272           ~ 6 0
8 NGC 6334 HII 17 20 51 -36 06.9           ~ 585 0
9 W 51 SNR 19 23 50 +14 06.0           ~ 1143 1

    Equat.    Gal    SGal    Ecl

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2020.07.11-20:37:35

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