The Leo IV dwarf spheroidal galaxy: color-magnitude diagram and pulsating stars

Details The Leo IV dwarf spheroidal galaxy: color-magnitude diagram and pulsating stars The Leo IV dwarf spheroidal galaxy: color-magnitude diagram and pulsating stars

2009-06-03

arxiv.org/abs/0906.0700v1

Astrophys.J.699:L125-L129,2009

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

14 pages, 4 figures, accepted for publication on The Astrophysical Journal Letters

Scientific paper

10.1088/0004-637X/699/2/L125

We present the first V, B-V color-magnitude diagram of the Leo IV dwarf spheroidal galaxy, a faint Milky Way satellite recently discovered by the Sloan Digital Sky Survey. We have obtained B,V time-series photometry reaching about half a magnitude below the Leo IV turnoff, which we detect at V= 24.7 mag, and have performed the first study of the variable star population. We have identified three RR Lyrae stars (all fundamental-mode pulsators, RRab) and one SX Phoenicis variable in the galaxy. In the period-amplitude diagram the Leo IV RR Lyrae stars are located close to the loci of Oosterhoff type I systems and the evolved fundamental-mode RR Lyrae stars in the Galactic globular cluster M3. However, their mean pulsation period, $$=0.655 days, would suggest an Oosterhoff type II classification for this galaxy. The RR Lyrae stars trace very well the galaxy's horizontal branch, setting its average magnitude at $= 21.48 \pm 0.03$ mag (standard deviation of the mean). This leads to a distance modulus of $\mu_{0}=20.94 \pm 0.07$ mag, corresponding to a distance of $154 \pm 5$ kpc, by adopting for the Leo IV dSph a reddening $E(B-V) = 0.04 \pm 0.01$ mag and a metallicity of [Fe/H] = -2.31 $\pm$ 0.10.

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