CH in stellar atmospheres: an extensive linelist

By T. Masseron, B. Plez, S. V. Eck, Réginald Colin, I. Daoutidis, M. Godefroid, Pierre-François Coheur, P. Bernath, A. Jorissen, N. Christlieb. 2014

190 citations recorded by the source corpus.

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 A 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.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a70c2c6b88306fbd222e66789d5c1431aa902d7e

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Citations in the corpus

The ExoMol database: Molecular line lists for exoplanet and other hot atmospheres (2016, background): “[139] Empirical NH 1 5000 1 12150 MoLLIST 4 Brooke et al.”
The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres (2020, background): “[139] Empirical NH 1 5000 1 12150 MoLLIST 4 Brooke et al.”