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ビッグバンから7億7千万年後の赤道移転7.51で,急速に星を形成している銀河
S L Finkelstein1, C Papovich, M Dickinson
1The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, Texas 78712, USA.
Nature
|October 25, 2013
まとめ
天文学者は,高い赤偏移 (z > 6.5) の銀河を調査した. 赤道偏移z = 7.51の1つの銀河が検出され,急速な濃縮と高い恒星形成率を示し,予想よりも早期の恒星形成がより強烈であることを示唆しました.
科学分野:
- 宇宙進化の宇宙進化について
- 銀河の形成と進化について
- 初期の宇宙 天体物理学
背景:
- レッドシフト (z) >7の銀河のスペクトル確認は,ライマンα放射検出により困難です.
- 以前の研究では,z>6.5で銀河間媒体の中性分数の急速な上昇が示唆され,ライマンα検出を妨げている.
- 以前の研究で限られたサンプルサイズと観察の深さにより,結論は暫定的であった.
研究 の 目的:
- 高赤偏移銀河 (z > 6.5) の深層近赤外線スペクトロスコピク調査を実施する.
- 初期の宇宙におけるライマンα放射の検出可能性を調査する.
- 初期の銀河の属性を特徴付けるため,金属含量と星形成率を含む.
主な方法:
- フォトメトリックで選択された43の銀河の,z > 6.5.5の深層近赤赤外線スペクトロスコーピーを実施しました.
- 放射線を分析して赤偏移を確認し,ライマンα放射を特定した.
- 銀河の色,金属含量,恒星形成率を計算した.
主要な成果:
- レッドシフト z = 7.51 (700万年後のビッグバン) のライマンα放射線を持つ単一の銀河を検出しました.
- 銀河は,金属の濃縮が著しくなり,銀河の急速な進化を示し,色合いを示しています.
- 年間約330太陽質量の恒星形成率を計算し,これは天の川の100倍以上です.
結論:
- ライマンα放射は,初期の宇宙では検出が困難であり,おそらくは銀河間媒体の特性によるものであることを確認した.
- これは,銀河が初期の宇宙で急速な化学的濃縮を経験していることを示唆している.
- これは,初期の宇宙には,これまで考えられていたよりも,より激しい恒星形成領域が含まれる可能性があることを示唆している.
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