NUCLEOSYNTHESIS IN A PRIMORDIAL SUPERNOVA: CARBON AND OXYGEN ABUNDANCES IN SMSS J031300.36-670839.3

被引：61

作者：

Bessell, Michael S. ^{[1
]}

Collet, Remo ^{[1
]}

Keller, Stefan C. ^{[1
,9
]}

Frebel, Anna ^{[2
,3
]}

Heger, Alexander ^{[4
,10
,11
,12
]}

Casey, Andrew R. ^{[5
]}

Masseron, Thomas ^{[5
]}

Asplund, Martin ^{[1
]}

Jacobson, Heather R. ^{[3
]}

Lind, Karin ^{[6
]}

Marino, Anna F. ^{[1
]}

Norris, John E. ^{[1
]}

Yong, David ^{[1
]}

Da Costa, Gary ^{[1
]}

Chan, Conrad ^{[4
]}

Magic, Zazralt ^{[7
]}

Schmidt, Brian ^{[1
]}

Tisserand, Patrick ^{[8
,12
]}

机构：

[1] Australian Natl Univ, CPMS, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia

[2] MIT, Dept Phys, Cambridge, MA 02139 USA

[3] MIT, Kavli Inst Astrophys & Space Sci, Cambridge, MA 02139 USA

[4] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia

[5] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[6] Uppsala Univ, Dept Phys & Astron, SE-75120 Uppsala, Sweden

[7] Max Planck Inst Astrophys, D-85741N Garching, Germany

[8] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France

[9] Australian Govt, Dept Def, Canberra, ACT 2610, Australia

[10] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA

[11] Shanghai Jiao Tong Univ, Dept Phys & Astron, CNA, Shanghai 200240, Peoples R China

[12] UPMC, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2015年 / 806卷 / 01期

基金：

澳大利亚研究理事会; 美国国家科学基金会;

关键词：

stars: Population III; supernovae: general; supernovae: individual (SMSS J031300.36); STARS; HE-0107-5240; HE-1327-2326; SIGNATURES;

D O I：

10.1088/2041-8205/806/1/L16

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

SMSS J031300.36-670839.3 (hereafter SM0313-6708) is a sub-giant halo star, with no detectable Fe lines and large overabundances of C and Mg relative to Ca. We obtained Very Large Telescope-Ultraviolet and Visual Echelle Spectrograph (UVES) spectra extending to 3060 angstrom showing strong OH A-X band lines enabling an oxygen abundance to be derived. The OH A-X band lines in SM0313-6708 are much stronger than the CH C-X band lines. Spectrum synthesis fits indicate an [O/C] ratio of 0.02 +/- 0.175. Our high signal-to-noise ratio UVES data also enabled us to lower the Fe abundance limit to [Fe/H](< 3D >,NLTE) < -7.52 (3 sigma). These data support our previous suggestion that the star formed from the iron-poor ejecta of a single massive star Population III supernova.

引用

页数：6

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