クワザール宿主銀河からの恒星光の検出 赤い偏移6以上
Xuheng Ding1,2, Masafusa Onoue3,4,5, John D Silverman6,7,8
1Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan. xuheng.ding@ipmu.jp.
Nature
|June 28, 2023
まとめ
JWSTで赤道偏移が6より大きい2つの 巨大でコンパクトな宿主銀河を検出しました これはブラックホールと恒星の質量関係が 宇宙の初期に確立されたことを示唆しています
科学分野:
- 宇宙学
- 銀河の進化
- ブラックホールの天体物理学
背景:
- クワザール宿主銀河を宇宙の夜明け (赤道偏移> 6) で検出することは困難です.
- 以前の検出には重力レンズが必要であり,より高い赤偏移 (z=4.5) に限られていた.
- 低光度クエーザーは 初期の銀河の形成を研究する 新しい道を開きます
研究 の 目的:
- 赤道偏移 > 6 のクエーサーの宿主銀河を検出し,特徴づけること.
- 初期の宇宙における 超大質量ブラックホールと 宿主銀河の共同進化を 研究するためです
- ブラックホールと恒星の質量関係が 初期宇宙時代に存在していたことを確認するためです
主な方法:
- ジェームズ・ウェブ宇宙望遠鏡 (JWST) の近赤外線画像 (1.5 と 3.6 μm) と光譜を用いた.
- 宿主銀河の放射を隔離するためにクエーサー光減量技術を使用した.
- ホスト銀河とブラックホールの質量測定のための恒星吸収線とガス運動を分析した.
主要な成果:
- 巨大な (1.3 x 10^10 と 3.4 x 10^10 M) とコンパクトな円盤状の宿主銀河をz > 6で検出した.
- 近赤外線で恒星の吸収線を介して宿主銀河の検出を確認しました.
- ブラックホールの質量 (1.4 x 10^9 と 2.0 x 10^8 M) を測定し,局所ブラックホールと恒星の質量関係と一致した.
結論:
- ブラックホールと恒星の質量関係は ビッグバンから10億年以内に確立されました
- JWSTは初期のクエーサー宿主銀河の 研究を可能にし 宇宙の誕生に関する理解を深めています
- 初期の巨大な銀河と 中央のブラックホールは すでに共進化していました
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