Astronomy and Astrophysics, volume 485, 823-835 (2008/7-3)
Probing Atlas model atmospheres at high spectral resolution. Stellar synthesis and reference template validation.
BERTONE E., BUZZONI A., CHAVEZ M. and RODRIGUEZ-MERINO L.H.
Abstract (from CDS):
The fast improvement of spectroscopic observations makes mandatory a strong effort on the theoretical side to better reproduce the spectral energy distribution (SED) of stars at high spectral resolution. In this regard, relying on the Kurucz Atlas/Synthe original codes we computed the Bluered library, consisting of 832 synthetic SED of stars, that cover a large parameter space at very high spectral resolution (R=500000) along the 3500-7000Å wavelength range. Bluered synthetic spectra have been used to assess in finer detail the intrinsic reliability and the performance limits of the Atlas theoretical framework. The continuum-normalized spectra of the Sun
, and Vega
, plus a selected list of 45 bright stars with high-quality SEDs from the Prugniel & Soubiran E lodie catalog, form our sample designed to probe the global properties of synthetic spectra across the entire range of H-R parameters.Atlas models display a better fitting performance with increasing stellar temperature. High-resolution spectra of Vega, the Sun, and Arcturus have been reproduced at R=100000, respectively, within a 0.7%, 4.5%, and 8.8% relative scatter in residual flux. In all the three cases, the residual flux distribution shows a significant asymmetry (skewness parameter γ=-2.21, -0.98, -0.67, respectively), which neatly confirms an overall ``excess'' of theoretical line blanketing. For the Sun, this apparent discrepancy is alleviated, but not recovered, by a systematic decrease (-40%) of the line oscillator strengths, log (gf), especially referring to iron transitions. Definitely, a straight ``astrophysical'' determination of log(gf) for each individual atomic transition has to be devised to overcome the problem. By neglecting overblanketing effects in theoretical models when fitting high-resolution continuum-normalized spectra of real stars, we lead to a systematically warmer effective temperature (between +80 and +300K for the solar fit) and a slightly poorer metal content.
Sun: atmosphere - stars: atmospheres - stars: individual: Arcturus - stars: individual: Vega - fundamental parameters - stars: line: profiles
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