I will describe an automated method for classifying low-resolution
stellar spectra extracted from objective-prism plates. The technique
is based on a model describing the transformation of theoretical
spectra from model atmosphere calculations to photographic spectra.
The spectra can thus be classified in a physical parameter space,
effective temperature and surface gravity, by applying a Chi-square
minimization scheme. This has been used to identify potential white
dwarf stars in a set of some 1 Mio. spectra.
©Andreas Voigt
Last modified: 02/21/2002