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レッドシフト 5.8 ~ 6.6 時の強い流出によってブラックホールの増殖を抑制する
M Bischetti1, C Feruglio2,3, V D'Odorico2,3,4
1INAF - Osservatorio Astronomico di Trieste, Trieste, Italy. manuela.bischetti@inaf.it.
Nature
|May 13, 2022
まとめ
初期の超大質量ブラックホールは 成長を遅らせた強力な風を示しています ブラックホールのフィードバックメカニズムの 始まりを示しています ブラックホールのフィードバックメカニズムは
科学分野:
- 宇宙の進化
- 天体物理学
- ブラックホール物理学
背景:
- 超大質量ブラックホールで動く明るいクエサーは再イオン化時代 (ビッグバンから50億~15億年後) に存在した.
- これらの初期のブラックホールの急速な形成と 質量の局所的な相関を超えることは 議論の余地があります
- ブラックホールの成長制御のメカニズムとタイミングはよく理解されていませんが,ブラックホールのフィードバックは疑わしいドライバーです.
研究 の 目的:
- 超大質量ブラックホールの成長を 制御する過程を調査する
- ブラックホールのフィードバックメカニズムの発生と特徴を特定する.
- 地元の宇宙で観察された 急速な初期成長から共生的な成長への移行を理解する
主な方法:
- 赤外線 5.8 から 6.6 のクエーザーの光学および近赤外線観測
- 流出の兆候である,広い,ブルーシフトの吸収線を特定するためのスペクトル分析.
- 低赤偏移 (z ≈ 2−4) のクエーザーとの流出特性の比較
主要な成果:
- 観測されたクエーザーの約半分は,z 5.8で広い,ブルーシフトの吸収谷を示している.
- これらの特徴は ブラックホールの駆動による 極端な流出速度を示すもので 光速の17%まで到達します
- このような流出風を持つクエザーの割合は,z ≈ 5.8でz ≈ 2-4に比べて約2.4倍高い.
結論:
- z 5.8の流出は 恒星間媒質にかなりのエネルギーを注入し 核ガスの蓄積を抑制し ブラックホールの成長を遅らせます
- ブラックホールのフィードバックの始まりです
- 赤色の光学的な色と 埃っぽい性質は 暗黒の蓄積と消火の初期段階にあることを示唆しています
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