Investigation of a sample of carbon-enhanced metal-poor stars observed with 
FORS and GMOS

Caffau, E.; Gallagher, A. J.; Bonifacio, P.; Spite, M.; Duffau, S.; Spite, F.; Monaco, L.; Sbordone, L.

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Investigation of a sample of carbon-enhanced metal-poor stars observed with FORS and GMOS

MPS-Authors

Caffau, E.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gallagher, A. J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Bonifacio, P.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Spite, M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Duffau, S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Spite, F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Monaco, L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sbordone, L.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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https://ui.adsabs.harvard.edu/abs/2018A&A...614A..68C
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Citation

Caffau, E., Gallagher, A. J., Bonifacio, P., Spite, M., Duffau, S., Spite, F., et al. (2018). Investigation of a sample of carbon-enhanced metal-poor stars observed with FORS and GMOS. Astronomy and Astrophysics, 614.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CE9C-4

Abstract

Aims: Carbon-enhanced metal-poor (CEMP) stars represent a sizeable fraction of all known metal-poor stars in the Galaxy. Their formation and composition remains a significant topic of investigation within the stellar astrophysics community.
Methods: We analysed a sample of low-resolution spectra of 30 dwarf stars, obtained using the visual and near UV FOcal Reducer and low dispersion Spectrograph for the Very Large Telescope (FORS/VLT) of the European Southern Observatory (ESO) and the Gemini Multi-Object Spectrographs (GMOS) at the GEMINI telescope, to derive their metallicity and carbon abundance.
Results: We derived C and Ca from all spectra, and Fe and Ba from the majority of the stars.
Conclusions: We have extended the population statistics of CEMP stars and have confirmed that in general, stars with a high C abundance belonging to the high C band show a high Ba-content (CEMP-s or -r/s), while stars with a normal C abundance or that are C-rich, but belong to the low C band, are normal in Ba (CEMP- no). Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 099.D-0791.Based on observations obtained at the Gemini Observatory (processed using the Gemini IRAF package), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil).Tables 1 and 2 are also available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/614/A68">http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/614/A68</A>