AGB stars in the Magellanic Clouds

Details AGB stars in the Magellanic Clouds AGB stars in the Magellanic Clouds

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.217..121w&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 217, no. 1-2, p. 121-130

Astronomy and Astrophysics

Astronomy

6

Asymptotic Giant Branch Stars, Cepheid Variables, Infrared Astronomy, Magellanic Clouds, Near Infrared Radiation, Sky Surveys (Astronomy), Stellar Luminosity, Stellar Magnitude, Stellar Mass, Supergiant Stars, Astronomical Photometry, Carbon Stars, Charge Coupled Devices, Diagrams, Star Clusters

Scientific paper

The stars that will be detectable in the Magellanic Clouds by the Deep Near-Infrared Survey (DENIS) and Two Micron All Sky Survey (2MASS) near infrared surveys are enumerated. All thermally-pulsing Asymptotic Giant Branch (AGB) stars will be observable in I, J, H and K, along with the top two magnitudes of both the early-AGB and the first giant branch. All carbon stars will be visible, and normal (N type) C stars will be easily distinguished by their large J-K colors. However, it will not be possible to separate faint, warm C stars from K and M stars using the photometry alone. Photometry of AGB stars in clusters will allow an accurate evaluation of the AGB tip luminosities as a function of initial mass. Random phase K magnitudes of Long Period Variables (LPVs) and Cepheids should provide a better measure of the Large Magellanic Cloud (LMC) tilt and distortions in the Small Magellanic Cloud (SMC). The K survey should turn up 100 to 150 objects undergoing superwind mass loss, these objects being OH/IR stars and the dust-enshrouded C star equivalents of OH/IR stars. It is shown that crowding should not be a problem even in the LMC bar.

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