The molecular emission-line spectrum of IRC +10216 between 330 and 358 GHz

Details The molecular emission-line spectrum of IRC +10216 between 330 and 358 GHz The molecular emission-line spectrum of IRC +10216 between 330 and 358 GHz

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apjs...94..147g&link_type=abstract

The Astrophysical Journal Supplement Series, vol. 94, no. 1, p. 147-162

Astronomy and Astrophysics

Astronomy

46

Carbon Stars, Emission Spectra, Infrared Astronomy, Molecular Spectra, Stellar Envelopes, Submillimeter Waves, Abundance, Broadband, Cosmic Dust, Molecular Excitation, Rotational States, Vibrational Spectra

Scientific paper

We have conducted a spectral line survey of IRC +10216 using the Caltech Submillimeter Observatory to an average sensitivity of approximately less than 95 mK. A deconvolution algorithm has been used to derive the continuous single-sideband spectrum from 330.2 to 358.1 GHz. A total of 56 spectral lines were detected of which 54 have been identified with 8 molecules and a total of 18 isotopomers. The observed lines are used to derive column densities and relative abundances for the detected species. Within this frequency range the spectral lines detected contribute the majority of the total flux emitted by IRC +10216. We use the derived column densities and excitation temperatures to simulate the molecular line emission (assuming local thermodynamic equilibrium (LTE) at frequencies up to 1000 GHZ. The observed and simulated flux from line emission is compared to broadband total flux measurements and to dust emission assuming a power-law variation of the dust emissivity. We conclude that significant corrections for the line flux must be made to broadband flux measurements of IRC +10216 at wavelengths longer than approximately 750 micrometers.

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