Atmospheric parameters for 1273 stars (Wu+, 2011)

Details Atmospheric parameters for 1273 stars (Wu+, 2011) Atmospheric parameters for 1273 stars (Wu+, 2011)

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010ycat..35259071w&link_type=abstract

VizieR On-line Data Catalog: J/A+A/525/A71. Originally published in: 2011A&A...525A..71W

Other

Stars: Atmospheres, Atlases, Effective Temperatures, Abundances: [Fe/H]

Scientific paper

Empirical libraries of stellar spectra play an important role in different fields. For example, they are used as reference for the automatic determination of atmospheric parameters, or for building synthetic stellar populations to study galaxies. The CFLIB (Coude-feed library, Indo-US) database is at present one of the most complete libraries, in terms of its coverage of the atmospheric parameters space (Teff, logg and [Fe/H]) and wavelength coverage 3460-9464Å at a resolution of ~1Å FWHM. Although the atmospheric parameters of most of the stars were determined from detailed analyses of high-resolution spectra, for nearly 300 of the 1273 stars of the library at least one of the three parameters is missing. For the others, the measurements, compiled from the literature, are inhomogeneous.
In this paper, we re-determine the atmospheric parameters, directly using the CFLIB spectra, and compare them to the previous studies. Methods. We use the ULySS program to derive the atmospheric parameters, using the ELODIE library as a reference.
Based on comparisons with several previous studies we conclude that our determinations are unbiased. For the 958 F,G, and K type stars the precision on Teff, logg, and [Fe/H] is respectively 43K, 0.13dex and 0.05dex. For the 53 M stars they are 82K, 0.22dex and 0.28dex. And for the 260 OBA type stars the relative precision on Teff is 5.1%, and on logg, and [Fe/H] the precision is respectively 0.19 dex and 0.16 dex. These parameters will be used to re-calibrate the CFLIB fluxes and to produce synthetic spectra of stellar populations.
(3 data files).

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