一个恒星形成星系在红移2.3的冷气体燃料的签名
N Bouché1, M T Murphy, G G Kacprzak
1CNRS/IRAP, Toulouse, France. nicolas.bouche@irap.omp.eu
概括
发现了气体积聚给星系的直接证据. 观测揭示了轨道气体的独特动力学特征,证实了它在银河系生长和恒星形成中的作用.
科学领域:
- 天文学和天体物理学
- 宇宙气体动力学 宇宙气体动力学
- 银河系的进化 银河系的进化
背景情况:
- 理论上,星系通过连续的星系间气体积累来成长.
- 对这种气体积聚过程的直接观测证据很少.
- 预计积聚的气体将围绕银河系光环运行,影响恒星形成和银河系动力学.
研究的目的:
- 提供直接的观测证据,证明气体积聚为遥远的恒星形成星系提供燃料.
- 为了研究与银河系光环中积累的气体相关的动力学特征.
- 量化气体积聚对星系生长的贡献.
主要方法:
- 利用背景类星体视线来探测围绕一个遥远的恒星形成星系的气体.
- 分析了从宿主星系预计距离26千帕塞克的气体动力学.
- 根据观测数据估计了气体积聚率.
主要成果:
- 在环银河系介质中检测到明显的动力学特征,与轨道上积累的气体一致.
- 证实了从恒星形成银河系显著距离 (26 kpc) 的气体存在.
- 估计的气体积聚率被发现与银河系的恒星形成率相当.
结论:
- 气体积聚对星系生长起着重要作用,为恒星形成提供燃料.
- 观察到的动力学特征为银河间气体的积累提供了有力的证据.
- 这项研究为银河系进化和进化的理论模型提供了直接的观测支持.
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