A ug 2 00 9 An Oosterhoff Analysis of the Galactic Bulge Field RR Lyrae stars : Implications On Their Absolute Magnitudes

We present an analysis of the period-V -amplitude plane for RR0 Lyrae stars (fundamental mode pulsators) with “normal” light curves in the bulge using the MACHO bulge fields. Although bulge globular clusters have RR Lyraes that divide into two reasonable distinct groups according to the average period of the RR0 Lyraes (Oosterhoff 1939), there is no evidence of a gap between Oosterhoff I and II stars in the bulge field star sample. The majority of the bulge RR0 Lyrae field star population have a difference in period compared to the Oosterhoff I cluster M3 (∆logP) that is shifted by about 0.02 days with regard to the Milky Way Oosterhoff I population, and the sample includes stars with ∆logP > 0.06 days, a characteristic hardly seen in Milky Way globular clusters. The metal-rich RR0 Lyrae stars in the Galactic bulge sample have ∆logP values on the other side of the spectrum as those in the metal-rich globular clusters NGC 6388 and NGC 6441. We find that the V -amplitude for a given period is a function of ∆logP, and not of metal abundance, similar to the result found by Clement & Shelton (1999) for RR Lyrae stars in Milky Way globular clusters. A comparative study of the bulge field stars with similar metallicities but different Oosterhoff types is carried out. Bulge field RR0 Lyrae variables with ∆logP values similar to Oosterhoff II clusters are about 0.2 mag brighter than RR0 Lyrae variables with ∆logP similar to Oosterhoff I clusters. Reliance upon a single M V -[Fe/H] relation may be inappropriate when considering populations with different ∆logP. Subject headings: surveys — stars: abundances, distances, Population II — Galaxy: center