再イオン化時代における高赤偏移銀河からの酸素放射線の検出
Akio K Inoue1, Yoichi Tamura2, Hiroshi Matsuo3
1College of General Education, Osaka Sangyo University, 3-1-1 Nakagaito, Daito, Osaka 574-8530, Japan. akinoue@las.osaka-sandai.ac.jp.
まとめ
宇宙再イオン化の初期 銀河は酸素と塵が少ない この研究では 酸素の放出が検出され 星間塵と中性ガスが稀な銀河を明らかにし 陽子の脱出を可能にしました
科学分野:
- 天文学と天体物理学
- 宇宙学
- 銀河の進化
背景:
- 初期の銀河の星間介質 (ISM) を理解することは,再イオン化の時代にとって極めて重要です.
- 銀河間の媒質に電離放射線の逃亡に影響する.
研究 の 目的:
- 初期の宇宙における 銀河の物理的性質と元素の豊富さを調べる
- 宇宙再イオン化における 銀河のISMの役割を決定する
主な方法:
- アタカマの大型ミリメートル/サブミリメートル配列 (ALMA) を観測に使用した.
- 88ミクロメートルの酸素放射線を検出した
- 遠赤外線と炭素放射線を探した
主要な成果:
- ビッグバンから7億年後の 銀河から酸素の放出が検出されました
- 推定酸素の豊富さは太陽の ~ 10% です.
- 恒星間塵の不足と 異常に少量の中性ガスを観測した
結論:
- 銀河の金属と塵の含有量が低いので イオン化フォトンの 効率的な脱出が考えられます
- これらの性質は 宇宙の再イオン化における 銀河の役割を支えています
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