Affiliation:
1. Department of Physics and Astronomy, Washington State University, Pullman, WA 99164, USA
Abstract
ABSTRACT
We investigate the frequency of occurrence of Galactic carbon stars as a function of progenitor mass using Gaia data. Small number statistics limit fidelity, but C-star frequency agrees with that observed in the Magellanic Clouds (MCs) down to m ≈ 1.67 M⊙. At m ≈ 1.38 M⊙, the frequency rises by a factor of three even though the frequency appears to drop to zero for the MCs. In fact this is due to a lack of clusters at the key age range in the MCs. At m ≈ 1.24 M⊙ and below, no C-stars are observed, corresponding to ages older than 4 Gyr. Within uncertainties, C-star frequency in M 31 is consistent with that of the Galaxy and the MCs. We find an ambiguous C-star candidate at ∼7 M⊙.
Funder
European Space Agency
CDS
National Aeronautics and Space Administration
NED
California Institute of Technology
Publisher
Oxford University Press (OUP)
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
1 articles.
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