Laboratory and Astronomical Detection of the Negative Molecular Ion C3N−

doi:10.1086/528947

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The Astrophysical Journal Volume 677 Number 2 Create an alert RSS this journal

P. Thaddeus et al. 2008 ApJ 677 1132 doi:10.1086/528947

Laboratory and Astronomical Detection of the Negative Molecular Ion C₃N⁻

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P. Thaddeus¹, C. A. Gottlieb¹, H. Gupta^1,2, S. Brünken¹, M. C. McCarthy¹, M. Agúndez³, M. Guélin⁴ and J. Cernicharo³

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pthaddeus@cfa.harvard.edu cgottlieb@cfa.harvard.edu hgupta@cfa.harvard.edu sbruenken@cfa.harvard.edu mccarthy@cfa.harvard.edu marce@damir.iem.csic.es cerni@damir.iem.csic.es guelin@iram.fr

¹ Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, and School of Engineering and Applied Sciences, Harvard University, 29 Oxford Street, Cambridge, MA 02138
² Institute for Theoretical Chemistry, Departments of Chemistry and Biochemistry, The University of Texas at Austin, TX 78712
³ Department of Molecular and Infrared Astrophysics, Instituto de Estructura de la Materia, CSIC, Serrano 121, 28006 Madrid, Spain
⁴ Insitut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38406 St. Martin d'Hères, France, and LERMA/Ecole Normale Superieure, 24 rue Lohmond, 75231 Paris, France

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Abstract References Cited By

The negative molecular ion C₃N⁻ has been detected at millimeter wavelengths in a low-pressure laboratory discharge, and then with frequencies derived from the laboratory data in the molecular envelope of IRC+10216. Spectroscopic constants derived from laboratory measurements of 12 transitions between 97 and 378 GHz allow the rotational spectrum to be calculated well into the submillimeter-wave band to 0.03 km s⁻¹ or better in equivalent radial velocity. Four transitions of C₃N⁻ were detected in IRC+10216 with the IRAM 30 m telescope at precisely the frequencies calculated from the laboratory measurements. The column density of C₃N⁻ is 0.5% that of C₃N, or approximately 20 times greater than that of C₄H⁻ relative to C₄H. The C₃N⁻ abundance in IRC+10216 is compared with a chemical model calculation by Petrie & Herbst. An upper limit in TMC-1 for C₃N⁻ relative to C₃N (<0.8%) and a limit for C₄H⁻ relative to C₄H (<0.004%) that is 5 times lower than that found in IRC+10216, were obtained from observations with the NRAO 100 m Green Bank Telescope (GBT). The fairly high concentration of C₃N⁻ achieved in the laboratory implies that other molecular anions containing the CN group may be within reach.

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