RR Lyrae stars in the Sagittarius dwarf galaxy: Period analysis

Abstract

(Abridged) We carried out a period analysis on ~3700 RR Lyrae stars spread over ~50 square degrees towards the Sagittarius dwarf galaxy (Sgr). The RR Lyraes are distributed almost evenly between Sgr and the Milky Way. For Sgr members, the average periods are 0.574 day and 0.322 day for RRab and RRc stars respectively. This places Sgr in the long-period tail of the Oosterhoff I group. We report the detection of 53 double-mode RR Lyrae stars (RRd) within our sample. The magnitude of 40 of these stars is consistent with membership in Sgr whereas 13 RRds are located within our Galaxy. We also found 13 RR Lyraes (5 in Sgr and 8 in the Galaxy) exhibiting two closely spaced frequencies, most probably related to non-radial pulsations. The period distribution of the RR Lyrae variables in Sgr is compared to those of other Milky Way satellites. We find a remarkable similarity between the RR Lyrae populations in Sgr and the Large Magellanic Cloud (LMC), suggesting that these galaxies have similar horizontal branch morphologies. This may indicate that Sgr and the LMC started their formation under similar conditions. Using various photometric indicators, we estimate the metallicity of the RR Lyrae stars in Sgr and find <[Fe/H]>~-1.6 dex with a dispersion of ~ +/-0.5 dex around this value and a minor but significant population at <-2.0 dex. We do not find evidence for a spatial metallicity gradient in the RR Lyrae population of Sgr. From the spatial distribution of RR Lyraes, we estimate the RRab content and total luminosity of this galaxy and find MV(Sgr)~-14.7 mag, a value that would be consistent with the empirical metallicity/luminosity relation for Dsph galaxies.