Infrared giants vs. supergiants. I. Far infrared-to-CO(1-0) intensity-ratio.

Details Infrared giants vs. supergiants. I. Far infrared-to-CO(1-0) intensity-ratio. Infrared giants vs. supergiants. I. Far infrared-to-CO(1-0) intensity-ratio.

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...315l..23j&link_type=abstract

Astronomy and Astrophysics, v.315, p.L23-L26

Astronomy and Astrophysics

Astrophysics

3

Circumstellar Matter, Stars: Late Type, Stars: Mass Loss, Stars: Agb And Post-Agb, Supergiants, Infrared: Stars, Radio Lines: Stars

Scientific paper

Until recently, the correlation between the IRAS flux density at 60μm, S_60_, and the intensity of the CO(1-0) line seemed well established for O-rich evolved stars with intermediate mass-loss rates (~10^-6^ to 10^-5^ Msun_/yr). This observational correlation was in agreement with theory of mass-loss rates. On the basis of more sensitive CO(1-0) observations performed with the IRAM-30m antenna, we show that a large group of infrared sources do not follow this correlation. Almost 50% of the infrared O-rich sources in our sample (IRAS flux ratio S_25_/S_12_ from 0.69 to 1.20) have "weak" CO emission relative to S_60_. These sources are more concentrated towards the Galactic plane. The majority of them have early spectral types and low IRAS variability index, and are thus probably supergiants, as it is already established for many of them and can be understood from theoretical considerations, mainly related to the large luminosity of the supergiants. We conclude that all those with "normal" CO emission (i.e. a low S_60_/T_mb_(1-0) ratio) are AGB stars. Possible origins of the "weak" CO emission observed in a few AGB stars are briefly discussed.

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