Toward a Pop II Mass-Luminosity Relation

Details Toward a Pop II Mass-Luminosity Relation Toward a Pop II Mass-Luminosity Relation

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop..116r&link_type=abstract

NOAO Proposal ID #1999B-0116

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Scientific paper

The observing runs contained within this proposal are part of a long term goal of constraining the variation of the Mass-Luminosity Relation as a function of composition. Using a sequence of Mosaic II images (U,V,R,I & H-alpha) we propose to make a detailed study of binaries and the general population of 2 globular clusters and three open clusters. The specific clusters were selected to have a wide range of chemical composition, from -2.2 <=[Fe/H]<=0.2. I will make a sensitive search for main-sequence binary stars, blue straggler stars, SX Phe pulsators and cataclysmic variables and construct a precise CMD to search for evidence of a binary sequence. The luminosity function of M30 will be compared with that derived from my team's HST data of that cluster's core (HST-GO-7379). Comparison of these two data sets, combined with Yale stellar evolutionary models (with co-I Demarque) will allow me to study the degree of mass segregation in this dynamically evolved cluster. As part of my ongoing project to constrain the Pop II Mass-Luminosity Relation (NSF-9902667) I will follow-up the detection of any detached main-sequence binaries with spectroscopic observations (with co-Is Orosz & Deliyannis) to determine the masses of the components. We also propose to obtain spectroscopic observations of an uncrowded binary candidate detected during previous work on NGC 6752. If this object and other binaries we hope to detect are double- lined spectroscopic binaries, our observations of radial velocity variations will allow the precise determination of masses. Single-lined spectroscopic binaries will allow us to derive the mass-ratio of the systems and begin to constrain the unknown mass-ratio distribution of binaries in clusters. I will be spending this coming year at CTIO on an NSF fellowship specifically to pursue this project.

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