Deep HST Imaging of Sextans A. II. Cepheids and Distance

Details Deep HST Imaging of Sextans A. II. Cepheids and Distance Deep HST Imaging of Sextans A. II. Cepheids and Distance

2002-11-21

arxiv.org/abs/astro-ph/0211486v1

Astron.J. 125 (2003) 1261-1290

Astronomy and Astrophysics

Astrophysics

59 pages, 24 figures Scheduled for publication in March 2003 AJ

Scientific paper

10.1086/346279

We have identified 82 short-period variable stars in Sextans A from deep WFPC2 observations. All of the periodic variables appear to be short-period Cepheids, with periods as small as 0.8 days for fundamental-mode Cepheids and 0.5 days for first-overtone Cepheids. These objects have been used, along with measurements of the RGB tip and red clump, to measure a true distance modulus to Sextans A of (m-M)_0 = 25.61 +/- 0.07, corresponding to a distance of d = 1.32 +/- 0.04 Mpc. Comparing distances calculated by these techniques, we find that short-period Cepheids (P < 2 days) are accurate distance indicators for objects at or below the metallicity of the SMC. As these objects are quite numerous in low-metallicity star-forming galaxies, they have the potential for providing extremely precise distances throughout the Local Group. We have also compared the relative distances produced by other distance indicators. We conclude that calibrations of RR Lyraes, the RGB tip, and the red clump are self-consistent, but that there appears to be a small dependence of long-period Cepheid distances on metallicity. Finally, we present relative distances of Sextans A, Leo A, IC 1613, and the Magellanic Clouds.

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