Journal
ASTROPHYSICAL JOURNAL
Volume 833, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/0004-637X/833/1/21
Keywords
Galaxy: halo; stars: abundances; stars: atmospheres; stars: individual (HE 0020-1741); stars: Population II; techniques: spectroscopic
Categories
Funding
- National Science Foundation [PHY-1430152]
- NSF [AST-1255160]
- Future Fellowship of the Australian Research Council [FT120100363]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1255160] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1430152] Funding Source: National Science Foundation
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We report on the first high-resolution spectroscopic analysis of HE. 0020-1741, 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, HE 0020-1741 is subclassified as a carbon-enhanced metal-poor star without enhancements in neutron-capture elements (CEMP-no). We show that the light-element abundance pattern of HE. 0020-1741 is consistent with predicted yields from a massive (M = 21.5 M circle dot), 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 10-100 M circle dot), 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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