Carbon monoxide emission from stars in the IRAS and revised AFGL catalogs. II - Massive carbon stars

Details Carbon monoxide emission from stars in the IRAS and revised AFGL catalogs. II - Massive carbon stars Carbon monoxide emission from stars in the IRAS and revised AFGL catalogs. II - Massive carbon stars

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...304..401z&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 304, May 1, 1986, p. 401-408.

Astronomy and Astrophysics

Astrophysics

154

Carbon Monoxide, Carbon Stars, Emission Spectra, Infrared Stars, Stellar Mass Ejection, Astronomical Catalogs, Flow Velocity, Milky Way Galaxy, Molecular Clouds, Radial Velocity, Spectral Line Width, Stellar Envelopes, Stellar Evolution

Scientific paper

We surveyed infrared bright stars in the IRAS and Revised AFGL catalogs in the J = 1 → 0 and, to a lesser extent, J = 2 → 1 rotational transitions of carbon monoxide. Broad lines were detected in 25 objects not previously seen in CO emission, including some stars first discovered in the IRAS survey about which very little is known. We discovered a number of carbon-rich stars at low Galactic latitude with large outflow velocity V, which are very likely to be among the most massive and luminous carbon-rich objects in the Galaxy. Two of these had V ≍ 34 km s-1, which is comparable to molecular outflow velocities measured for oxygen-rich stars with supergiant luminosities. By way of contrast, the high-latitude prototypical carbon star with a large mass loss rate, IRC + 10216, has a very modest V of ˜15 km s-1. We suggest that IRC + 10216 is considerably closer to Earth than is commonly believed, perhaps as close as 100-150 pc. We also found CO emission from a few stars with large radial velocities with respect to the local standard of rest, including V CrB, for which V = - 100km s-1. We detected strong narrow CO emission associated with IRAS 0423+4336 and AFGL 5497, both of which we identify as young stars embedded in molecular clouds.

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