Variable stars in the ultra-faint dwarf spheroidal galaxy Ursa Major i

Abstract

We have performed the first study of the variable star population of Ursa Major I (UMa I), an ultra-faint dwarf satellite recently discovered around the Milky Way (MW) by the Sloan Digital Sky Survey. Combining time series observations in the B and V bands from four different telescopes, we have identified seven RR Lyrae stars in UMa I, of which five are fundamental-mode (RRab) and two are first-overtone pulsators (RRc). Our V, B-V color-magnitude diagram of UMa I reaches V 23 mag (at a signal-to-noise ratio of 6) and shows features typical of a single old stellar population. The mean pulsation period of the RRab stars 〈Pab〉 = 0.628, σ = 0.071 days (or 〈Pab〉 = 0.599, σ = 0.032 days, if V4, the longest period and brightest variable, is discarded) and the position on the period-amplitude diagram suggest an Oosterhoff-intermediate classification for the galaxy. The RR Lyrae stars trace the galaxy horizontal branch (HB) at an average apparent magnitude of 〈V(RR)〉 = 20.43 ± 0.02 mag (average on six stars and discarding V4), giving in turn a distance modulus for UMa I of (m-M)0 = 19.94 ± 0.13 mag, distance d = kpc, in the scale where the distance modulus of the Large Magellanic Cloud is 18.5 ± 0.1 mag. Isodensity contours of UMa I red giants and HB stars (including the RR Lyrae stars identified in this study) show that the galaxy has an S-shaped structure, which is likely caused by the tidal interaction with the MW. Photometric metallicities were derived for six of the UMa I RR Lyrae stars from the parameters of the Fourier decomposition of the V-band light curves, leading to an average metal abundance of [Fe/H] = -2.29 dex (σ = 0.06 dex, average on six stars) on the Carretta et al. metallicity scale. © 2013. The American Astronomical Society. All rights reserved.