Asymptotic Giant Branch Stars in the Phoenix Dwarf Galaxy

Details Asymptotic Giant Branch Stars in the Phoenix Dwarf Galaxy Asymptotic Giant Branch Stars in the Phoenix Dwarf Galaxy

2007-12-29

arxiv.org/abs/0801.0038v1

Astronomy and Astrophysics

Astrophysics

9 Pages, 7 figures, accepted for MNRAS

Scientific paper

10.1111/j.1365-2966.2008.12907.x

JHKs near-infrared photometry of stars in the Phoenix dwarf galaxy is presented and discussed. Combining these data with the optical photometry of Massey et al. allows a rather clean separation of field stars from Phoenix members. The discovery of a Mira variable (P = 425 days), which is almost certainly a carbon star, leads to an estimate of the distance modulus of 23.10+/-0.18 that is consistent with other estimates and indicates the existence of a significant population of age ~2 Gyr. The two carbon stars of Da Costa have M{bol} = -3.8 and are consistent with belonging to a population of similar age; some other possible members of such a population are identified. A Da Costa non-carbon star is Delta Ks~0.3 mag brighter than these two carbon stars. It may be an AGB star of the dominant old population. The nature of other stars lying close to it in the Ks,(J-Ks) diagram needs studying.

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