NGC452626の分子ガス運動学によるブラックホールの質量測定
Timothy A Davis1, Martin Bureau, Michele Cappellari
1European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching-bei-München, Germany. tdavis@eso.org
Nature
|February 1, 2013
まとめ
研究者は,分子ガスダイナミクスを用いて超大質量ブラックホールの質量を測定する新しい方法を開発しました. この技術は,ブラックホールの質量を正確に推定し,共進化の研究のためにアクセス可能な銀河の数を拡大します.
科学分野:
- 天体物理学 天体物理学
- 銀河の進化 銀河の進化 銀河の進化
- ブラックホール物理学 ブラックホール物理学
背景:
- 超大質量ブラックホール (SMBH) の質量は銀河の性質と相関しており,共進化を示唆しています.
- SMBHの質量を測定する現在の方法は,数と範囲が限られており,共進化の研究を妨げています.
- 既存のテクニックには,恒星とイオン化されたガスの動力学,およびマザー放射が含まれていますが,それらは普遍的に適用できません.
研究 の 目的:
- SMBHの質量を正確に推定するための新しい方法を開発し,検証する.
- SMBHの質量を確実に測定できる銀河のサンプルを拡大する.
- 銀河とそれらの中央のブラックホールの共同進化を調査する.
主な方法:
- 中央ブラックホールの重力の影響がガス分子動力学に及ぼす影響をモデル化.
- このダイナミックモデルを使用して,一酸化炭素 (CO) 排出量のインターフェロメトリック観測をフィッティングします.
- この方法を初期型銀河NGC4526に適用して,その中央ブラックホールの質量を導き出します.
主要な成果:
- この研究では,NGC 4526のSMBH質量は,太陽の質量4.5(+4.2)(-3.1) ×10^8であると成功裏に推定されました.
- 分子ガス運動法により,正確なブラックホールの質量推定が得られる.
- 次世代インターフェロメーターによる将来の観測は,数百の局所銀河の質量を数時間で測定することができる.
結論:
- 分子ガス動力学は,SMBHの質量を推定するための強力な新しいツールを提供します.
- この技術は,ブラックホールと銀河の共同進化を研究するためにアクセス可能な銀河の数を大幅に増加させます.
- この方法は,銀河系とブラックホールの進化に関する私たちの理解を,ローカル・ユニバース全体で前進させるのに有望である.
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