Bibcode
Allende Prieto, C.; Koesterke, L.; Hubeny, I.; Bautista, M. A.; Barklem, P. S.; Nahar, S. N.
Bibliographical reference
Astronomy and Astrophysics, Volume 618, id.A25, 7 pp.
Advertised on:
10
2018
Journal
Citations
56
Refereed citations
52
Description
Context. Models of stellar spectra are necessary for interpreting light
from individual stars, planets, integrated stellar populations, nebulae,
and the interstellar medium. Aims: We provide a comprehensive and
homogeneous collection of synthetic spectra for a wide range of
atmospheric parameters and chemical compositions. Methods: We
compile atomic and molecular data from the literature. We adopt the
largest and most recent set of ATLAS9 model atmospheres, and use the
radiative code ASSɛT. Results: The resulting collection
of spectra is made publicly available at medium and high-resolution (R
≡ λ/δλ = 10 000, 100 000 and 300 000) spectral
grids, which include variations in effective temperature between 3500 K
and 30 000 K, surface gravity (0 ≤ log g ≤ 5), and metallicity (-5
≤ [Fe/H] ≤ +0:5), spanning the wavelength interval 120-6500 nm. A
second set of denser grids with additional dimensions, [α/Fe] and
micro-turbulence, are also provided (covering 200-2500 nm). We compare
models with observations for a few representative cases.
Data files are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/618/A25
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Chemical Abundances in Stars
Stellar spectroscopy allows us to determine the properties and chemical compositions of stars. From this information for stars of different ages in the Milky Way, it is possible to reconstruct the chemical evolution of the Galaxy, as well as the origin of the elements heavier than boron, created mainly in stellar interiors. It is also possible to
Carlos
Allende Prieto