| Issue |
A&A
Volume 587, March 2016
|
|
|---|---|---|
| Article Number | L4 | |
| Number of page(s) | 44 | |
| Section | Letters | |
| DOI | https://doi.org/10.1051/0004-6361/201527531 | |
| Published online | 25 February 2016 | |
A rigorous detection of interstellar CH3NCO: An important missing species in astrochemical networks⋆,⋆⋆
1 Grupo de Astrofísica Molecular, Instituto de CC. de Materiales de Madrid (ICMM-CSIC), Sor Juana Inés de la Cruz 3, Cantoblanco, 28049 Madrid, Spain
e-mail: jose.cernicharo@csic.es
2 Laboratory of Mm- and Submm- Spectroscopy, Institute of Physics, Polish Academy of Sciences, Al. Lotnikow 32/46, 02-668 Warszawa, Poland
e-mail: kisiel@ifpan.edu.pl
3 Grupo de Espectroscopía Molecular (GEM), Edificio Quifima, Área de Química-Física, Laboratorios de Espectroscopía y Bioespectroscopía, Parque Científico UVa, Unidad Asociada CSIC, Universidad de Valladolid, 47011 Valladolid, Spain
4 Department of Physics, The Ohio State University, 191 W. Woodruff Ave, Columbus, OH 43210, USA
5 Wright State University, 3640 Colonel Glenn Hwy, Dayton, OH 45435, USA
6 Institut des Sciences Chimiques de Rennes, École Nationale Supérieure de Chimie de Rennes, CNRS, UMR 6226, 11 Allée de Beaulieu, CS 50837, 35708 Rennes Cedex 7, France
Received: 9 October 2015
Accepted: 1 February 2016
The recent analysis of the composition of the frozen surface of comet 67P/Churyumov-Gerasimenko has revealed a significant number of complex organic molecules. Methyl isocyanate (CH3NCO) is one of the more abundant species detected on the comet surface. In this work we report extensive characterization of its rotational spectrum resulting in a list of 1269 confidently assigned laboratory lines and its detection in space towards the Orion clouds where 399 lines of the molecule have been unambiguously identified. We find that the limited mm-wave laboratory data reported prior to our work require some revision. The abundance of CH3NCO in Orion is only a factor of ten below those of HNCO and CH3CN. Unlike the molecular abundances in the coma of comets, which correlate with those of warm molecular clouds, molecular abundances in the gas phase in Orion are only weakly correlated with those measured on the comet surface. We also compare our abundances with those derived recently for this molecule towards Sgr B2 (Halfen et al. 2015, ApJ, 812, L5). A more accurate abundance of CH3NCO is provided for this cloud based on our extensive laboratory work.
Key words: ISM: abundances / ISM: individual objects: Orion KL / ISM: molecules / methods: laboratory: molecular / molecular data / ISM: clouds
This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00009.SV. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan) with NRC (Canada), NSC, and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work was also based on observations carried out with the IRAM 30-meter telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).
Full Table A.6 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/587/L4
© ESO, 2016
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