2008A&A...482..197P


C.D.S. - SIMBAD4 rel 1.7 - 2020.03.29CEST18:17:54

2008A&A...482..197P - Astronomy and Astrophysics, volume 482, 197-208 (2008/4-4)

Submillimeter line emission from LMC N159W: a dense, clumpy PDR in a low metallicity environment.

PINEDA J.L., MIZUNO N., STUTZKI J., CUBICK M., ARAVENA M., BENSCH F., BERTOLDI F., BRONFMAN L., FUJISHITA K., GRAF U.U., HITSCHFELD M., HONINGH N., JAKOB H., JACOBS K., KAWAMURA A., KLEIN U., KRAMER C., MAY J., MILLER M., MIZUNO Y., MUELLER P., ONISHI T., OSSENKOPF V., RABANUS D., ROELLIG M., RUBIO M., SASAGO H., SCHIEDER R., SIMON R., SUN K., VOLGENAU N., YAMAMOTO H. and FUKUI Y.

Abstract (from CDS):

Star formation at earlier cosmological times took place in an interstellar medium with low metallicity. The Large Magellanic Cloud (LMC) is ideally suited to study star formation in such an environment. The physical and chemical state of the ISM in a star forming environment can be constrained by observations of submm and FIR spectral lines of the main carbon carrying species, CO, CI and CII, which originate in the surface layers of molecular clouds illuminated by the UV radiation of the newly formed, young stars. We present high-angular resolution sub-millimeter observations in the N159W region in the LMC obtained with the NANTEN2 telescope of the 12CO J=4 -3, J=7-6, and 13CO J=4-3 rotational and [CI] 3P1-3P0 and 3P2-3P1 fine-structure transitions. The 13CO J=4-3 and [CI] 3P2-3P1 transitions are detected for the first time in the LMC. We derive the physical and chemical properties of the low-metallicity molecular gas using an escape probability code and a self-consistent solution of the chemistry and thermal balance of the gas in the framework of a clumpy cloud PDR model. The separate excitation analysis of the submm CO lines and the carbon fine structure lines shows that the emitting gas in the N159W region has temperatures of about 80 K and densities of about 104cm–3. The estimated C to CO abundance ratio close to unity is substantially higher than in dense massive star-forming regions in the Milky Way. The analysis of all observed lines together, including the [CII] line intensity reported in the literature, in the context of a clumpy cloud PDR model constrains the UV intensity to about χ≃220 and an average density of the clump ensemble of about 105cm–3, thus confirming the presence of high density material in the LMC N159W region.

Abstract Copyright:

Journal keyword(s): astrochemistry - ISM: molecules - ISM: clouds - ISM: individual objects: N 159W

Status at CDS:  

Simbad objects: 15

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Number of rows : 15

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 Magellanic Clouds GrG 03 00 -71.0           ~ 5540 1
2 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14610 1
3 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 568 1
4 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 706 0
5 NAME Ori A MoC 05 38 -07.1           ~ 2646 0
6 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1706 1
7 LHA 120-N 159W MoC 05 39 32.510 -69 46 02.74           ~ 72 0
8 LHA 120-N 159 HII 05 39 46.650 -69 45 39.94           ~ 248 2
9 2MASS J05400074-6947129 Y*O 05 40 00.741 -69 47 12.91 14.808 15.690 15.072   14.336 ~ 32 0
10 LHA 120-N 159S MoC 05 40 03.750 -69 51 01.62           ~ 42 0
11 NAME N159 Blob in LMC HII 05 40 04.2 -69 44 43           ~ 34 0
12 LHA 120-N 159E MoC 05 40 10.980 -69 44 35.84           ~ 41 0
13 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2120 0
14 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 162 1
15 [MBS2007c] CygX-N44 Rad 20 39 01.01 +42 22 50.2           ~ 362 0

    Equat.    Gal    SGal    Ecl

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2020.03.29-18:17:54

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