Volume 517, July 2010
|Number of page(s)||37|
|Section||Interstellar and circumstellar matter|
|Published online||17 August 2010|
A line confusion limited millimeter survey of Orion KL I. Sulfur carbon chains*
I. Sulfur carbon chains
Centro de Astrobiología (CSIC-INTA), Departamento de
Astrofísica Molecular, Ctra. de Aljalvir Km 4, 28850
Torrejón de Ardoz, Madrid, Spain e-mail: [belen;pardo]@damir.iem.csic.es; [jcernicharo;jr.goicoechea]@cab.inta-csic.es
Accepted: 15 April 2010
We perform a sensitive (line confusion limited), single-side band spectral survey towards Orion KL with the IRAM 30 m telescope, covering the following frequency ranges: 80–115.5 GHz, 130–178 GHz, and 197–281 GHz. We detect more than 14 400 spectral features of which 10 040 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 210 K, 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.
Key words: surveys / stars: formation / ISM: abundances / ISM: clouds / ISM: molecules / radio lines: ISM
Appendices A and B are only available in electronic form at http://www.aanda.org
© ESO, 2010
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