超大質量ブラックホールのフィードバックとサブパーセックスケールで観測されたフィードバック

Takuma Izumi^1,2,3, Keiichi Wada^4,5,6, Masatoshi Imanishi^1,3

¹National Astronomical Observatory of Japan, Tokyo 181-8588, Japan.

Science (New York, N.Y.)

|November 2, 2023

まとめ

活発な銀河は超大質量ブラックホールに供給されますがガスの大半は蓄積ではなく流出で放出されますこの研究は密度が高く不安定なガスの円盤がサーキヌス銀河の核内での蓄積を促す仕組みを明らかにしています

科学分野:

天体物理学
銀河の進化
ブラックホールの蓄積

背景:

活発な銀河には超大質量ブラックホール (SMBH) が存在し周囲の銀河物質の蓄積によって成長します
活発な銀河の中央10パーセック内の蓄積過程の直接観測は,小さな角の大きさのために困難です.

研究の目的:

サーキヌス銀河の活発な核の亜パーセックスケールでの蓄積プロセスとガスダイナミクスを調査する.
近隣の活発な銀河の核の蓄積メカニズムを解明するためです

主な方法:

サーキヌス銀河の活性核を観察するために,サブミリメートル干渉計が使われました.
分析は,サブパーセックスケールでのガス流入と流出を解決することに焦点を当てました.

主要な成果:

密度の高い分子ガスの流れがサーキヌス銀河の亜パーセックスケールで検出されました
入気ガスの3%未満はSMBHによって蓄積され,残りは多相流出によって排出されます.
流入を囲む重力的に不安定で密集したガスの円盤が特定され,中央パーセック内の蓄積を促した.

結論:

活発な銀河の核に流入するガスのほとんどは放出され,銀河のフィードバックに重要な役割を果たします.
密度の高いガスの円盤の重力不安定は,最も内部の地域におけるSMBHへの蓄積を促す重要なメカニズムです.

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