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dc.contributor.authorBandyopadhyay, A-
dc.contributor.authorSivarani, T-
dc.contributor.authorSusmitha, A-
dc.contributor.authorBeers, T. C-
dc.contributor.authorGiridhar, S-
dc.contributor.authorArun Surya-
dc.contributor.authorMasseron, T-
dc.identifier.citationThe Astrophysical Journal, Vol. 859, No. 2, 114en_US
dc.descriptionRestricted Accessen_US
dc.description.abstractSDSS J082625.70+612515.10 (V = 11.4 [Fe/H] = ‑3.1) and SDSS J134144.60+474128.90 (V = 12.4 [Fe/H] = ‑3.2) were observed with the SDSS 2.5m telescope as part of the SDSS MARVELS spectroscopic pre-survey and identified as extremely metal-poor (EMP; [Fe/H] < ‑3.0) stars during the high-resolution follow-up using the Hanle Echelle Spectrograph (HESP) on the 2.0-m Himalayan Chandra Telescope. In this paper, the first science results using HESP, we present a detailed analysis of their chemical abundances. Both stars exhibit under-abundances in their neutron capture elements, while one of them (SDSS J134144.60+474128.90) is clearly enhanced in carbon. Lithium was also detected in this star at a level of about A(Li) = 1.95. The spectra were obtained over a span of 6–24 months, and indicate that both stars could be members of binary systems. We compare the elemental abundances derived for these two stars along with other carbon-enhanced metal-poor (CEMP) and EMP stars, in order to understand the nature of their parent supernovae. We find that CEMP-no stars and EMP-dwarfs show a very similar trend in their lithium abundances at various metallicities. We also find indications of CEMP-no stars having larger abundances of Cr and Co at given metallicities compared to EMP stars.en_US
dc.publisherIOP Publishingen_US
dc.rights© The American Astronomical Society-
dc.subjectStars: abundancesen_US
dc.subjectStars: carbonen_US
dc.subjectStars: chemically peculiaren_US
dc.subjectStars: early-typeen_US
dc.subjectStars: neutronen_US
dc.subjectStars: Population IIIen_US
dc.titleChemical Composition of Two Bright, Extremely Metal-poor Stars from the SDSS MARVELS Pre-surveyen_US
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