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ハッブル・ディープ・フィールドのz ≈ 5.2の銀河の過剰密度の強いスターバースト HDF 850.1は,ハッブル・ディープ・フィールドのz ≈ 5.2の銀河の過剰密度の強いスターバーストである
Fabian Walter1, Roberto Decarli, Chris Carilli
1Max-Planck Institut für Astronomie, Königstuhl 17, D-69117, Heidelberg, Germany. walter@mpia.de
Nature
|June 16, 2012
まとめ
天文学者は,深空観測を用いて,遠い銀河であるHDF850.1を特定した. この銀河は赤道偏移が大きい (z=5.183),これは宇宙の初期に形成され,活発な恒星形成地域であることを示している.
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
- 観測天体物理学について
背景:
- ハッブル・ディープ・フィールド (HDF) は,遥かなる宇宙の深い多波長視点を提供し,何千もの銀河を明らかにします.
- HDF850.1は850ミクロメートルのHDFで最も明るい光源で,10年以上前に特定されましたが,より短い波長での同位体がなく,特徴付けが困難でした.
研究 の 目的:
- 謎のHDF850.1.1.の赤偏移,大きさ,質量を決定する.
- この強烈な恒星形成の銀河の性質と宇宙の文脈を調査するために.
主な方法:
- ミリメートル波の分子線スキャンを行い,スペクトル線を検出しました.
- ディープフィールド観測と多波長データ分析を活用した.
主要な成果:
- HDF850.1の正確な赤偏移z = 5.183を決定し,ビッグバン後の11億年の宇宙年齢で銀河の過剰密度に置きました.
- 5キロパルセックスケールで空間的にその源を解明し,恒星形成の速度は年間850太陽質量であり,動的質量は約1.3×10^11太陽質量であり,有意な分子ガス成分がある.
- この赤道偏移は,以前に特定されたほとんどのサブミリメートルの明るい銀河よりも高いことが判明しました.
結論:
- HDF850.1は,初期の宇宙の非常に活発で巨大な銀河を表しています.
- 正確な位置付けにもかかわらず,星光を放つ同位体は検出されず,異常な性質または遮蔽された形成を示唆しています.
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