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The Leo IV dwarf spheroidal galaxy: color-magnitude diagram and pulsating stars | | M. I. Moretti
; M. Dall'Ora
; V. Ripepi
; G. Clementini
; L. Di Fabrizio
; H. Smith
; N. De Lee
; C. Kuehn
; M. Catelan
; M. Marconi
; I. Musella
; T. Beers
; K. Kinemuchi
; | | Date: |
3 Jun 2009 | | 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, $<P{
m ab}>$=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 $<V_{
m RR}>= 21.48 pm 0.03$ 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. | | Source: | arXiv, 0906.0700 | | Services: | Forum | Review | PDF | Favorites | |
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