A lambda 2 mm molecular line survey of the C-star envelope IRC+10216

Details A lambda 2 mm molecular line survey of the C-star envelope IRC+10216 A lambda 2 mm molecular line survey of the C-star envelope IRC+10216

Mar 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26as..142..181c&link_type=abstract

Astronomy and Astrophysics Supplement, v.142, p.181-215

Astronomy and Astrophysics

Astrophysics

121

Line Identification, Surveys, Stars: Agb And Post-Agb, Stars: Carbon, Stars: Circumstellar Matter, Stars: Individual: Irc+10216, Ism: Molecules, Radio Lines: Stars

Scientific paper

The mm-wave spectrum of the C-star envelope IRC+10216 has been continuously surveyed between 129.0 and 172.5 GHz with the IRAM 30-m telescope. 380 lines are detected, of which 317 have been identified. The identified lines arise from 30 different molecules and radicals which, in their vast majority, are not observed in hot and dense interstellar clouds such as Orion A or W3(OH). Actually, half of the molecular species identified in the mm-wave spectrum of IRC+10216 were first observed in the course of this spectral survey. The new species include several carbon-chain molecules and radicals, as well as silicon and metallic compounds. They also include molecules containing rare isotopes of C, Mg, Si, S and Cl, whose elemental abundance ratios in the envelope are redetermined. We observe, in particular, four 13C isotopomers of C_4H, three of C_3N and HC_3N, and four doubly-substituted isotopomers of SiS and CS. 63 lines remain unidentified. Probably, a large fraction of those are rotational transitions inside the excited bending states of the abundant species NaCN, C_5H, and C_6H. We can also expect some lines to be ground state transitions of poorly known silicon and metal compounds, such as the slightly asymmetrical top molecule SiCSi. Tables 2 to 9 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html or\hfill\break http://www.edpsciences.org

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