[C ii] 158-μmの放射は,リマン・アルファ系を阻害した宿主銀河から発生する
Marcel Neeleman1, Nissim Kanekar2, J Xavier Prochaska3
1University of California Observatories-Lick Observatory, University of California, Santa Cruz, CA 95064, USA. marcel@ucsc.edu.
Science (New York, N.Y.)
|March 25, 2017
まとめ
天文学者は[C ii]線と高赤偏移吸収体付近の銀河からの塵の放射を検出しました これらの銀河は 膨大で豊かなガス貯蔵庫を持つ 巨大な恒星系に似ています
科学分野:
- 天文学と天体物理学
- 宇宙学
背景:
- 高赤偏移の銀河の周りのガスを研究することは 宇宙の進化を理解するために不可欠です
- これらの銀河の観測は 背景のクエーサーと比べると 薄いため 難しいものです
研究 の 目的:
- 高赤偏差 (z ~ 4) で吸収線系に関連する銀河を特定し,特徴づけること.
- 銀河の物理的性質と 周囲のガスを調べるため
主な方法:
- アタカマの大型ミリメートル/亜ミリメートル配列 (ALMA) を利用する.
- [C ii]158μmラインとダスト連続体放射を検出する.
主要な成果:
- [C ii]と2つの銀河からの塵の連続放射をz ~ 4で成功裏に検出しました.
- これらの銀河は高金属性吸収系と関連しています
- 宿主銀河は 巨大な恒星形成銀河に似た性質を示しています
結論:
- この研究は,これらの銀河の星間媒介を超えて広がる,濃縮された中性水素ガス貯蔵庫の存在を確認しています.
- これは初期の銀河の環銀河媒体の新しい洞察を提供します.
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