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arXiv · 0801.0038

Asymptotic Giant Branch Stars in the Phoenix Dwarf Galaxy

John Menzies·Michael Feast·Patricia Whitelock·Enrico Olivier·Noriyuki Matsunaga·Gary Da Costa
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Abstract

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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John Menzies, Michael Feast, Patricia Whitelock, Enrico Olivier, Noriyuki Matsunaga, Gary Da Costa. 2007-12-29. Asymptotic Giant Branch Stars in the Phoenix Dwarf Galaxy. https://doi.org/10.1111/j.1365-2966.2008.12907.x

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