The White Dwarf Cooling Age and Initial-Final Mass Relationship -- Constraints from Open Star Clusters.

Details The White Dwarf Cooling Age and Initial-Final Mass Relationship -- Constraints from Open Star Clusters. The White Dwarf Cooling Age and Initial-Final Mass Relationship -- Constraints from Open Star Clusters.

Aug 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002noao.prop...99h&link_type=abstract

NOAO Proposal ID #2002B-0099

Physics

Scientific paper

We propose to use the combination of GMOS (imaging and spectroscopy) and results from the CFHT Open Star Cluster Survey (Kalirai et al. 2001a) to establish a global semi-empirical relationship for the white dwarf initial-final mass relation (WDIFMR) and therefore constrain the evolution and star formation history of the Galaxy. We have identified all white dwarf (WD) candidates as faint as V = 25 in several of the richest clusters in the Northern Hemisphere, and now, for the first time, can obtain spectra for hundreds of white dwarfs for which the distances are accurately known.

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