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Why Are Some Gamma-Ray Bursts Hosted by Oxygen-rich Galaxies?
Hashimoto, Tetsuya1; Chaudhary, Ravi2; Ohta, Kouji3; Goto, Tomotsugu1; Hammer, Francois4; Kong, Albert K. H.1; Nomoto, Ken'ichi5; Mao JR(毛基荣)6
Source PublicationASTROPHYSICAL JOURNAL
2018-08-10
Volume863Issue:1Pages:14
DOI10.3847/1538-4357/aad2d1
Contribution Rank第6完成单位
Indexed BySCI
KeywordGalaxies: Abundances Gamma-ray Burst: Individual (980425,080517)
Abstract

Theoretically long gamma-ray bursts (GRBs) are expected to happen in low-metallicity environments, because in a single massive star scenario, low iron abundance prevents loss of angular momentum through stellar wind, resulting in ultra-relativistic jets and the burst. In this sense, not just a simple metallicity measurement but also low iron abundance ([Fe/H] less than or similar to -1.0) is essentially important. Observationally, however, oxygen abundance has been measured more often due to stronger emission. In terms of oxygen abundance, some GRBs have been reported to be hosted by high-metallicity star-forming galaxies, in tension with theoretical predictions. Here we compare iron and oxygen abundances for the first time for GRB host galaxies (GRB 980425 and 080517) based on the emissionline diagnostics. The estimated total iron abundances, including iron in both gas and dust, are well below the solar value. The total iron abundances can be explained by the typical value of theoretical predictions ([Fe/H] less than or similar to -1.0), despite high oxygen abundance in one of them. According to our iron abundance measurements, the single massive star scenario still survives even if the oxygen abundance of the host is very high, such as the solar value. Relying only on oxygen abundance could mislead us on the origin of the GRBs. The measured oxygen-to-iron ratios, [O/Fe], can be comparable to the highest values among the iron-measured galaxies in the Sloan Digital Sky Survey. Possible theoretical explanations of such high [O/Fe] include the young age of the hosts, top-heavy initial mass function, and fallback mechanism of the iron element in supernova explosions.

Funding ProjectMinistry of Science and Technology of Taiwan[NSC 103-2112-M-007-002-MY3] ; Ministry of Science and Technology of Taiwan[105-2112-M-007-003-MY3] ; World Premier International Research Center Initiative (WPI Initiative) ; MEXT, Japan ; JSPS KAKENHI[JP26400222] ; JSPS KAKENHI[JP16H02168] ; JSPS KAKENHI[JP17K05382] ; Endowed Research Unit (Dark side of the universe) by Hamamatsu Photonics KK
Funding OrganizationMinistry of Science and Technology of Taiwan[NSC 103-2112-M-007-002-MY3, 105-2112-M-007-003-MY3] ; World Premier International Research Center Initiative (WPI Initiative) ; MEXT, Japan ; JSPS KAKENHI[JP26400222, JP16H02168, JP17K05382] ; Endowed Research Unit (Dark side of the universe) by Hamamatsu Photonics KK
Language英语
Subject Area天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
WOS IDWOS:000441711100004
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordDigital Sky Survey ; Star-forming Galaxies ; Mass-metallicity Relation ; Metal-poor Stars ; Interstellar-medium ; Chemical-composition ; Abundance Ratios ; Formation Rates ; High-redshift ; Evolution
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/17830
Collection丽江天文观测站(南方基地)
Corresponding AuthorHashimoto, Tetsuya
Affiliation1.Institute of Astronomy, National Tsing Hua University 101, Section 2. Kuang-Fu Road, Hsinchu, 30013, Taiwan
2.Department of Physics, Indian Institute of Technology Delhi Hauz Khas, New Delhi, 110016, India
3.Department of Astronomy, Kyoto University Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto, Kyoto, 606-8588, Japan
4.Laboratoire Galaxies Étoiles Physique et Instrumentation, Observatoire de Paris-Meudon 5 place Jules Janssen, F-92195 Meudon Cedex, France
5.Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Kashiwa, Chiba 277-8583, Japan
6.Yunnan Observatories, Chinese Academy of Sciences 650011 Kunming, Yunnan Province, People's Republic of China
Recommended Citation
GB/T 7714
Hashimoto, Tetsuya,Chaudhary, Ravi,Ohta, Kouji,et al. Why Are Some Gamma-Ray Bursts Hosted by Oxygen-rich Galaxies?[J]. ASTROPHYSICAL JOURNAL,2018,863(1):14.
APA Hashimoto, Tetsuya.,Chaudhary, Ravi.,Ohta, Kouji.,Goto, Tomotsugu.,Hammer, Francois.,...&Mao JR.(2018).Why Are Some Gamma-Ray Bursts Hosted by Oxygen-rich Galaxies?.ASTROPHYSICAL JOURNAL,863(1),14.
MLA Hashimoto, Tetsuya,et al."Why Are Some Gamma-Ray Bursts Hosted by Oxygen-rich Galaxies?".ASTROPHYSICAL JOURNAL 863.1(2018):14.
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