| Authors | Moretti, Maria Ida; Dall'Ora, Massimo; Ripepi, Vincenzo; Clementini, Gisella; Di Fabrizio, Luca; Smith, Horace A.; DeLee, Nathan; Kuehn, Charles; Catelan, Márcio; Marconi, Marcella; Musella, Ilaria; Beers, Timothy C.; Kinemuchi, Karen |
| Abstract | 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, langPabrang = 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 langV RRrang = 21.48 ± 0.03 mag (standard deviation of the mean). This leads to a distance modulus of μ0 = 20.94 ± 0.07 mag, corresponding to a distance of 154 ± 5 kpc, by adopting for the Leo IV dSph a reddening E(B - V) = 0.04 ± 0.01 mag and a metallicity of [Fe/H] = -2.31 ± 0.10. Based on data collected at the 2.5 m Isaac Newton Telescope, La Palma, Canary Island, Spain, at the 4.2 m William Herschel Telescope, Roche de los Muchachos, Canary Islands, Spain, and at the 4.1 m Southern Astrophysical Research Telescope, Cerro Pachón, Chile. |
