Spectroscopic Classification of Novae in M31

Details Spectroscopic Classification of Novae in M31 Spectroscopic Classification of Novae in M31

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007noao.prop..101s&link_type=abstract

NOAO Proposal ID #2007B-0101

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Scientific paper

The luminosity and frequency of occurrence of Classical Novae makes them potentially important tracers of the binary star populations of galaxies. Here, we propose to continue our successful HET program of spectroscopic follow-up of novae in M31. Novae for our spectroscopic survey are being discovered in both our ground-based imaging program and in other ongoing M31 imaging patrols (e.g. ROTSE and the Lick Observatory Supernova Search). Our primary objective is to gain further insight into the nova population in M31, and specifically to determine whether there are indeed two distinct nova populations, as our first year of data suggests there may be. This in turn may be directly related to fundamental properties of the progenitor binary (e.g. the mass and composition of the white dwarf component) and the stellar population (bulge or disk) in which a nova resides. These observations represent an important part of the most ambitious multi-site and multi- wavelength discovery and follow-up campaign on extragalactic novae to date.

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