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高赤移転のスターバースト銀河の周りの冷たい分子ガスの大きな渦巻貯蔵庫
E Falgarone1, M A Zwaan2, B Godard1
1LERMA/LRA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Université Paris 06, Ecole normale supérieure, 75005 Paris, France.
Nature
|August 17, 2017
まとめ
スターバースト銀河は 銀河の風を利用して 渦巻状態を維持し スターバーストを延長します これらの風はガスを貯蔵庫に処理しますが 燃料の星形成には 合併や蓄積による追加的な質量投入が必要です
科学分野:
- 天文学と天体物理学
- 宇宙の進化
- 銀河の形成 と 進化
背景:
- スターバースト銀河は 恒星形成率が高い 強力な宇宙エンジンです
- これらの速度を維持するには,フィードバックプロセスにもかかわらず,かなりの冷たい分子ガスが必要です.
- メチリジンカチオン (CH+) は,非均衡ガスの条件のトレーサーであり,エネルギー分散を示します.
研究 の 目的:
- スターバースト銀河における 銀河のフィードバックの役割を調査する
- スターバースト銀河の内部と周辺のガスの物理的条件を 探査する
- 銀河の成長と反射の相互作用を理解するために
主な方法:
- レンズ状のスターバースト銀河におけるCH+ (J=1-0) 放射線と吸収線の検出 赤道偏移 ~2.5
- 線形特性 (幅,臨界密度) を分析してガスの状態と起源を推測する.
- ガス貯蔵庫と大量流出率のモデル化
主要な成果:
- CH+の放射線は 銀河の風が動かす 強い衝撃波を示しています
- CH+吸収線は,スターバーストの核を越えて広がる 渦巻く冷たいガス貯蔵庫を明らかにします.
- 銀河の風は多相貯水池を作り 星形成のバランスをとるのに 十分ではありません
結論:
- 銀河からのフィードバックと 渦巻感と重力が 星爆発の段階を延長します
- 恒星形成率を高く保つには 合併や冷流による 追加の質量投入が必要である.
- この研究は,初期の宇宙の恒星形成を支えるメカニズムについての洞察を提供します.
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