Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.217..159h&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 217, no. 1-2, p. 159
Astronomy and Astrophysics
Astronomy
Asymptotic Giant Branch Stars, Dwarf Stars, Galaxies, Giant Stars, Infrared Astronomy, Mira Variables, Sky Surveys (Astronomy), Stellar Evolution, Stellar Temperature, Detection, Metals, Stellar Color, Stellar Magnitude
Scientific paper
Concerning the separation of disk Miras and semiregular variables using just Deep Near-Infrared Survey (DENIS) and Infrared Astronomy Satellite (IRAS) data, I refer to the paper by Hron & Kerschbaum (1994). For those stars for which at least IRAS 12 micrometer fluxes are available, (K-(12)) is a good selection criterion, otherwise (I-K) is reasonably useful. Contamination by the expected large number of M dwarfs should not be a problem because these stars will be found at much fainter K magnitudes than the galactic Asymptotic Giant Branch (AGB) stars. However, the bluest of the AGB variables will be indistinguishable from the non-variable M giants, both in their colors and their apparent magnitudes. (H-K) should probably allow a good distinction between Miras and semiregulars, even if one considers the scatter in this color index due to variability. With regard to short period Miras, there is evidence for the existence of both disk and metal poor stars among the Miras with periods less than 200 days. The metal poor stars are systematically hotter (at constant period) than the disk stars, with the temperature difference between the disk and non-disk stars being consistent with a metallicity difference of about -0.6 dex. The scale heights of the disk and non-disk stars are in agreement with the corresponding values for the old and the thick disk. If these short period Miras can be reliably identified in the DENIS and/or Two Micron All Sky Survey (2MASS) databases, they would allow an investigation of the large scale properties of the thick disk.
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