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The Reionization History and Early Metal Enrichment Inferred from the Gamma-Ray Burst Rate
https://doi.org/10.24517/00010248
https://doi.org/10.24517/0001024861cdb9fc-0018-435b-9bb7-26e94d05b5cc
| 名前 / ファイル | ライセンス | アクション |
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SC-PR-YONETOKU-D-13.pdf (142.7 kB)
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| アイテムタイプ | 学術雑誌論文 / Journal Article(1) | |||||||||
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| 公開日 | 2017-10-03 | |||||||||
| タイトル | ||||||||||
| タイトル | The Reionization History and Early Metal Enrichment Inferred from the Gamma-Ray Burst Rate | |||||||||
| 資源タイプ | ||||||||||
| 資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||||||
| 資源タイプ | journal article | |||||||||
| ID登録 | ||||||||||
| ID登録 | 10.24517/00010248 | |||||||||
| ID登録タイプ | JaLC | |||||||||
| 著者 |
Murakami, Toshio
× Murakami, Toshio× Yonetoku, Daisuke× Umemura, M.× Matsubayashi, T.× Yamazaki, R. |
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| 著者別表示 |
村上, 敏夫
× 村上, 敏夫
× 米德, 大輔
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| 提供者所属 | ||||||||||
| 内容記述タイプ | Other | |||||||||
| 内容記述 | 金沢大学大学院自然科学研究科物理学 | |||||||||
| 書誌情報 |
The Astrophysical Journal 巻 625, 号 1, p. L13-L16, 発行日 2005-05-20 |
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| ISSN | ||||||||||
| 収録物識別子タイプ | ISSN | |||||||||
| 収録物識別子 | 0004-637X | |||||||||
| NCID | ||||||||||
| 収録物識別子タイプ | NCID | |||||||||
| 収録物識別子 | AA00553242 | |||||||||
| DOI | ||||||||||
| 関連タイプ | isVersionOf | |||||||||
| 識別子タイプ | DOI | |||||||||
| 関連識別子 | 10.1086/430828 | |||||||||
| 出版者 | ||||||||||
| 出版者 | American Astronomical Society | |||||||||
| 抄録 | ||||||||||
| 内容記述タイプ | Abstract | |||||||||
| 内容記述 | Based on the gamma-ray burst event rate at redshifts of 4 ≤ z ≤ 12, which is assessed by the spectral peak energy-to-luminosity relation recently found by Yonetoku et al., we observationally derive the star formation rate (SFR) for Population III (Pop. III) stars in a high-redshift universe. As a result, we find that Pop. III stars could form continuously at 4 ≤ z ≤ 12. Using the derived Pop. III SFR, we attempt to estimate the ultraviolet (UV) photon emission rate at 7 ≤ z ≤ 12 in which redshift range no observational information has been hitherto obtained on ionizing radiation intensity. We find that the UV emissivity at 7 ≤ z ≤ 12 can make a noticeable contribution to the early reionization. The maximal emissivity is higher than the level required to keep ionizing the intergalactic matter (IGM) at 7 ≤ z ≤ 12. However, if the escape fraction of ionizing photons from Pop. III objects is smaller than 10%, then the IGM can be neutralized at some redshift, which may lead to the double reionization. As for the enrichment, the ejection of all metals synthesized in Pop. III objects is marginally consistent with the IGM metallicity, although the confinement of metals in Pop. III objects can reduce the enrichment significantly. © 2005. The American Astronomical Society. All rights reserved. | |||||||||
| 著者版フラグ | ||||||||||
| 出版タイプ | AM | |||||||||
| 出版タイプResource | http://purl.org/coar/version/c_ab4af688f83e57aa | |||||||||
