Observational constraints on first-star nucleosynthesis: II. spectroscopy of an ultra metal-poor CEMP-no star
We report on the first high-resolution spectroscopic analysis of HE0020-1741, a bright (V=12.9), ultra metal-poor ([Fe/H] = -4.1), carbon-enhanced ([C/Fe] = +1.7) star selected from the Hamburg/ESO Survey. This star exhibits low abundances of neutron-capture elements ([Ba/Fe] = -1.1), and an absolut...
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| Main Authors: | , |
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| Format: | Article (Journal) Chapter/Article |
| Language: | English |
| Published: |
September 8, 2016
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| In: |
Arxiv
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| Online Access: | Verlag, kostenfrei, Volltext: http://arxiv.org/abs/1609.02134
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| Author Notes: | Vinicius M. Placco, Anna Frebel, Timothy C. Beers, Jinmi Yoon, Anirudh Chiti, Alexander Heger, Conrad Chan, Andrew R. Casey, and Norbert Christlieb |
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| 245 | 1 | 0 | |a Observational constraints on first-star nucleosynthesis |b II. spectroscopy of an ultra metal-poor CEMP-no star |c Vinicius M. Placco, Anna Frebel, Timothy C. Beers, Jinmi Yoon, Anirudh Chiti, Alexander Heger, Conrad Chan, Andrew R. Casey, and Norbert Christlieb |
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| 520 | |a We report on the first high-resolution spectroscopic analysis of HE0020-1741, a bright (V=12.9), ultra metal-poor ([Fe/H] = -4.1), carbon-enhanced ([C/Fe] = +1.7) star selected from the Hamburg/ESO Survey. This star exhibits low abundances of neutron-capture elements ([Ba/Fe] = -1.1), and an absolute carbon abundance A(C) = 6.1; based on either criterion, HE0020-1741 is sub-classified as a CEMP-no star. We show that the light-element abundance pattern of HE0020-1741 is consistent with predicted yields from a massive (M = 21.5 Mo), primordial composition, supernova (SN) progenitor. We also compare the abundance patterns of other ultra metal-poor stars from the literature with available measures of C, N, Na, Mg, and Fe abundances with an extensive grid of SN models (covering the mass range 10 Mo - 100 Mo), in order to probe the nature of their likely stellar progenitors. Our results suggest that at least two classes of progenitors are required at [Fe/H] < -4.0, as the abundance patterns for more than half of the sample studied in this work (7 out of 12 stars) cannot be easily reproduced by the predicted yields. | ||
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