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Observational Studies01:11

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Super-resolution Imaging of the Bacterial Division Machinery
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Published on: January 21, 2013

赤道偏移 z = 6.96 の銀河です.

Masanori Iye1, Kazuaki Ota, Nobunari Kashikawa

  • 1National Astronomical Observatory, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan. iye@optik.mtk.nao.ac.jp

Nature
|September 15, 2006
PubMed
まとめ

初期の銀河の形成は,赤道偏移 z = 6.96 でスペクトロスコープで特定された銀河によって確認されており,ビッグバンから7億5000万年後の年代です. この発見は,銀河の集まりが宇宙の歴史のずっと早い時期に活発であったことを明らかにしています.

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科学分野:

  • コスモロジー・コスモロジーとは
  • 銀河の形成と進化について
  • 初期の宇宙 天体物理学

背景:

  • 初期の宇宙における銀河形成の正確なタイミングはよく理解されていません.
  • 宇宙マイクロ波背景研究によると,再イオン化は赤道移転 z = 6 と 14 の間に発生したことを示唆しています.
  • 銀河に関する以前のスペクトル測定は,より高い赤偏移の光度測定候補にもかかわらず,z < 6.6に限定されていました.

研究 の 目的:

  • 非常に高い赤偏移 (z > 7) での銀河の存在をスペクトル顕微鏡で確認する.
  • 初期の宇宙における銀河形成の始まりと恒星形成の活動を調査する.
  • zの銀河の数密度を約7で判別する.

主な方法:

  • 高赤偏移で銀河候補のスペクトル観測.
  • 銀河のスペクトルを分析して,放射線,特にライマン-アルファを特定する.
  • 銀河の赤道移転の決定と恒星形成率の推定.

主要な成果:

  • 銀河のスペクトル赤道偏移はz = 6.96で,ビッグバンから7億5000万年後に得られた.
  • 銀河のスペクトルには顕著なライマン・アルファ放射があり,活発な恒星形成を示しています.
  • 推定される恒星形成率は,年間約10太陽質量である.

結論:

  • 銀河の形成は,宇宙が現在の年齢の約6%しかなかったときに活発に起こっていました.
  • z約7の銀河の密度は,z = 6.6.6の銀河よりも (18-36%) 明らかに低い.
  • この発見は,確認された初期の銀河形成の観測境界を押し広げている.