Volume 571, November 2014
|Number of page(s)||29|
|Section||Atomic, molecular, and nuclear data|
|Published online||06 November 2014|
CH in stellar atmospheres: an extensive linelist⋆
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles
CP 226, Boulevard du Triomphe,
2 Laboratoire Univers et Particules de Montpellier , Université Montpellier 2, CNRS, 34095 Montpellier, France
3 Service de Chimie quantique et Photophysique, Université Libre de Bruxelles, CP160/09, avenue F.D. Roosevelt 50, 1050 Bruxelles, Belgium
4 Department of Chemistry & Biochemistry, Old Dominion University, Norfolk, VA, USA
5 University of Heidelberg, Zentrum für Astronomie, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany
Accepted: 2 June 2014
The advent of high-resolution spectrographs and detailed stellar atmosphere modelling has strengthened the need for accurate molecular data. Carbon-enhanced metal-poor (CEMP) stars spectra are interesting objects with which to study transitions from the CH molecule. We combine programs for spectral analysis of molecules and stellar-radiative transfer codes to build an extensive CH linelist, including predissociation broadening as well as newly identified levels. We show examples of strong predissociation CH lines in CEMP stars, and we stress the important role played by the CH features in the Bond-Neff feature depressing the spectra of barium stars by as much as 0.2 mag in the λ = 3000−5500 Å range. Because of the extreme thermodynamic conditions prevailing in stellar atmospheres (compared to the laboratory), molecular transitions with high energy levels can be observed. Stellar spectra can thus be used to constrain and improve molecular data.
Key words: molecular data / techniques: spectroscopic / stars: carbon
Full Table 14 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/571/A47
© ESO, 2014
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