Near-UV Spectra of Andromeda Globular Clusters Compared to Spectral Calculations

Details Near-UV Spectra of Andromeda Globular Clusters Compared to Spectral Calculations Near-UV Spectra of Andromeda Globular Clusters Compared to Spectral Calculations

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8371p&link_type=abstract

HST Proposal ID #8371

Computer Science

Hst Proposal Id #8371 Galaxy Populations And Interactions

Scientific paper

The near-ultraviolet spectrum of an old stellar population offers the best hope for determining its age and metallicity, since it is dominated by stars near the main-sequence turnoff. We have begun the first step towards this goal by calculating spectra from first principles from 2400Angstrom to 3200Angstrom for late F and early G stars near the main sequence. The calculations span metallicities 0.1 to 5* solar, and agree well at the low end with stellar IUE and HST spectra. Here we propose to compare archival near-UV spectra of four globular clusters in M31 against theoretical composite spectra to be derived from the grid. Calculated spectra for stars of various temperature and gravity will be weighted and coadded at each of several levels of overall metallicity and relative light-element abundance. We will check the validity of each satisfactory near-UV match against the available color-magnitude diagram and optical spectroscopy for each cluster. The results should show, at each cluster metallicity, how accurately age and metallicity may be derived from near-UV spectra alone and what observational requirements on wavelength coverage, S/N, and resolution are entailed for extragalactic objects which cannot be spatially resolved or optically observed.

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