銀河のH2Oマイクロ波放射源のスペクトル,変数,サイズ,および極化

S H Knowles, C H Mayer, A C Cheung

Science (New York, N.Y.)

|March 7, 1969

まとめ

天文学者は,銀河の8つの源泉で水分子からのラジオスペクトル線放射を測定しました. これらの小さな,強烈に明るい光源は,複雑なスペクトル特性,極化,および急速な強度変化を示します.

科学分野:

ラジオ天文学ラジオ天文学
天体物理学天体物理学
分子スペクトロスコーピーは分子スペクトロスコーピーを用います.

背景:

水 (H2O) マザーは,銀河のエネルギープロセスの重要なトレーサーです.
以前の観測では,多数のウォーターマザー源が特定されましたが,それらの詳細な性質については,さらなる調査が必要です.

研究の目的:

銀河の小さな,高輝度温度源からの水分子によるラジオスペクトル線放射を調査するために.
これらの銀河の水マザー源のスペクトル特性,極化,および変動性を特徴づけるために.

主な方法:

水 (H2O) のスペクトル線放射を,波長1.35cmで観測した.
8つの異なる銀河の源からのラジオ放射の分析.
源直径,輝度温度,スペクトル特徴,極化,時間経過による強度変動の測定.

主要な成果:

8つの銀河系からの水スペクトル線放射が検出され,全て直径1弧分未満です.
これらの光源で非常に高い明るさの温度を観測した.
数多くの複雑なスペクトル特徴を特定し,その中にはわずかな極化を示すものもあります.
週間の間にわたっていくつかのスペクトル特徴の有意な強度変化を記録した.

結論:

観測された特徴は,これらの銀河の水マザー源がエネルギー現象と関連していることを示唆しています.
急速な変動と偏極化は,これらのコンパクトな天体内のダイナミックなプロセスを示している.
これらの水質マザー源のさらなる研究により,星形成と流出領域の洞察が得られます.

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