Volume 589, May 2016
|Number of page(s)||10|
|Section||Numerical methods and codes|
|Published online||18 April 2016|
1 Department of Physics and Astronomy, Notre Dame University-Louaize, PO Box 72, Zouk Mikaël, Lebanon
2 Université de Toulouse, UPS-Observatoire Midi-Pyrénées, IRAP, 31000 Toulouse, France
3 CNRS, Institut de Recherche en Astrophysique et Planétologie, 14 av. E. Belin, 31400 Toulouse, France
4 LESIA, UMR 8109, Observatoire de Paris, place J. Janssen, Meudon, France
5 Laboratoire Lagange, Université de Nice Sophia, Parc Valrose, 06100 Nice, France
Received: 28 December 2015
Accepted: 2 March 2016
Context. We present an automated procedure that simultaneously derives the effective temperature Teff, surface gravity log g, metallicity [Fe/H], and equatorial projected rotational velocity vsini for “normal” A and Am stars. The procedure is based on the principal component analysis (PCA) inversion method, which we published in a recent paper .
Aims. A sample of 322 high-resolution spectra of F0-B9 stars, retrieved from the Polarbase, SOPHIE, and ELODIE databases, were used to test this technique with real data. We selected the spectral region from 4400−5000 Å as it contains many metallic lines and the Balmer Hβ line.
Methods. Using three data sets at resolving powers of R = 42 000, 65 000 and 76 000, about ~6.6 × 106 synthetic spectra were calculated to build a large learning database. The online power iteration algorithm was applied to these learning data sets to estimate the principal components (PC). The projection of spectra onto the few PCs offered an efficient comparison metric in a low-dimensional space. The spectra of the well-known A0- and A1-type stars, Vega and Sirius A, were used as control spectra in the three databases. Spectra of other well-known A-type stars were also employed to characterize the accuracy of the inversion technique.
Results. We inverted all of the observational spectra and derived the atmospheric parameters. After removal of a few outliers, the PCA-inversion method appeared to be very efficient in determining Teff, [Fe/H], and vsini for A/Am stars. The derived parameters agree very well with previous determinations. Using a statistical approach, deviations of around 150 K, 0.35 dex, 0.15 dex, and 2 km s-1 were found for Teff, log g, [Fe/H], and vsini with respect to literature values for A-type stars.
Conclusions. The PCA inversion proves to be a very fast, practical, and reliable tool for estimating stellar parameters of FGK and A stars and for deriving effective temperatures of M stars.
Key words: stars: fundamental parameters / stars: early-type / methods: numerical
Table 2 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/589/A83
© ESO, 2016
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