The Oosterhoff Dichotomy as a Signature of Different Halo Formation Histories

Details The Oosterhoff Dichotomy as a Signature of Different Halo Formation Histories The Oosterhoff Dichotomy as a Signature of Different Halo Formation Histories

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.propq..86l&link_type=abstract

NOAO Proposal ID #2000A-0086

Physics

Scientific paper

In the recent study of Lee & Carney (AJ, 118, 1373), we showed that there is a discontinuity in the M_V(RR) - [Fe/H] relation using two clusters with similar metallicities. The RR Lyraes in the Oosterhoff II cluster M2 are about 0.2 mag brighter than those in the Oosterhoff I cluster M3. We suggested that a difference in age is responsible for the RR Lyrae luminosity difference. We propose the further test using main sequence fitting and a period-shift analysis of NGC 5986, in the former class, relative to NGC 3201, an example of the latter class. We request observing time with the 4m telescope to obtain main sequence photometry for NGC 5986. We also request observing time with the 0.9m telescope to better define the RR Lyrae light curves and pulsational parameters for both clusters.

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