2010A&A...517A..96T


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST03:29:58

2010A&A...517A..96T - Astronomy and Astrophysics, volume 517, A96-96 (2010/7-1)

A line confusion limited millimeter survey of Orion KL. I. Sulfur carbon chains.

TERCERO B., CERNICHARO J., PARDO J.R. and GOICOECHEA J.R.

Abstract (from CDS):

We perform a sensitive (line confusion limited), single-side band spectral survey towards Orion KL with the IRAM 30m telescope, covering the following frequency ranges: 80-115.5GHz, 130-178GHz, and 197-281GHz. We detect more than 14400 spectral features of which 10040 have been identified up to date and attributed to 43 different molecules, including 148 isotopologues and lines from vibrationally excited states. In this paper, we focus on the study of OCS, HCS+, H2CS, CS, CCS, C3S, and their isotopologues. In addition, we map the OCS J=18-17 line and complete complementary observations of several OCS lines at selected positions around Orion IRc2 (the position selected for the survey). We report the first detection of OCS ν2=1 and ν3=1 vibrationally excited states in space and the first detection of C3S in warm clouds. Most of CCS, and almost all C3S, line emission arises from the hot core indicating an enhancement of their abundances in warm and dense gas. Column densities and isotopic ratios have been calculated using a large velocity gradient (LVG) excitation and radiative transfer code (for the low density gas components) and a local thermal equilibrium (LTE) code (appropriate for the warm and dense hot core component), which takes into account the different cloud components known to exist towards Orion KL, the extended ridge, compact ridge, plateau, and hot core. The vibrational temperature derived from OCS ν2=1 and ν3=1 levels is ≃210K, similar to the gas kinetic temperature in the hot core. These OCS high energy levels are probably pumped by absorption of IR dust photons. We derive an upper limit to the OC3S, H2CCS, HNCS, HOCS+, and NCS column densities. Finally, we discuss the D/H abundance ratio and infer the following isotopic abundances: 12C/13C=45±20, 32S/34S=20±6, 32S/33S=75±29, and 16O/18O=250±135.

Abstract Copyright:

Journal keyword(s): surveys - stars: formation - ISM: abundances - ISM: clouds - ISM: molecules - radio lines: ISM

Simbad objects: 11

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Number of rows : 11

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 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 257 0
2 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1053 3
3 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1359 0
4 QSO J0530+13 QSO 05 30 56.41672 +13 31 55.1495     20.0 19.35   ~ 879 1
5 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2001 1
6 JCMTSE J053514.4-052232 Y*? 05 35 14.488 -05 22 32.10           ~ 46 0
7 NAME Orion Core ? 05 35 14.5 -05 22 30           ~ 175 0
8 [RLK73] IRc 2 IR 05 35 14.51548 -05 22 30.5943           ~ 572 1
9 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2133 0
10 GAL 327.30-00.60 HII 15 53 05.0 -54 35 24           ~ 122 0
11 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1909 1

    Equat.    Gal    SGal    Ecl

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2020.07.04-03:29:58

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