Volume 574, February 2015
|Number of page(s)||27|
|Section||Interstellar and circumstellar matter|
|Published online||23 January 2015|
Purple Mountain Observatory & Key Laboratory for Radio Astronomy,
Chinese Academy of Sciences, 2 West
Beijing Road, 210008, Nanjing,
2 Max-Planck Institute für Radioastronomy, Auf dem Hügel 69, 53121 Bonn, Germany
3 University of Chinese Academy of Sciences, No. 19A Yuquan Road, 100049 Beijing, PR China
4 Astronomy Department, King Abdulaziz University, PO Box 80203, 21589 Jeddah, Saudi Arabia
5 I. Physikalisches Institut, Universität zu Köln, 50937 Köln, Germany
6 University of Applied Sciences Bonn-Rhein-Sieg, Grantham-Allee 20, 53757 Sankt Augustin, Germany
Received: 15 August 2014
Accepted: 19 November 2014
Context. IRC +10216 is the prototypical carbon star exhibiting an extended molecular circumstellar envelope. Its spectral properties are therefore the template for an entire class of objects.
Aims. The main goal is to systematically study the λ ~ 1.3 cm spectral line characteristics of IRC +10216.
Methods. We carried out a spectral line survey with the Effelsberg-100 m telescope toward IRC +10216. It covers the frequency range between 17.8 GHz and 26.3 GHz (K-band).
Results. In the circumstellar shell of IRC +10216, we find 78 spectral lines, among which 12 remain unidentified. The identified lines are assigned to 18 different molecules and radicals. A total of 23 lines from species known to exist in this envelope are detected for the first time outside the solar system and there are additional 20 lines first detected in IRC +10216. The potential orgin of “U” lines is also discussed. Assuming local thermodynamic equilibrium (LTE), we then determine rotational temperatures and column densities of 17 detected molecules. Molecular abundances relative to H2 are also estimated. A non-LTE analysis of NH3 shows that the bulk of its emission arises from the inner envelope with a kinetic temperature of 70 ± 20 K. Evidence for NH3 emitting gas with higher kinetic temperature is also obtained, and potential abundance differences between various 13C-bearing isotopologues of HC5N are evaluated. Overall, the isotopic 12C/13C ratio is estimated to be 49 ± 9. Finally, a comparison of detected molecules in the λ ~ 1.3 cm range with the dark cloud TMC-1 indicates that silicate-bearing molecules are more predominant in IRC +10216.
Key words: astrochemistry / ISM: molecules / stars: individual: IRC +10216 / radio lines: stars
Appendices are available in electronic form at http://www.aanda.org
Spectra as FITS files are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/574/A56
© ESO, 2015
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