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Updated: Jun 7, 2025

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来自环银河系介质的辐射的MUSE源盲调查
Huanian Zhang1,2, Dennis Zaritsky2
1Department of Astronomy, Huazhong University of Science and Technology, Wuhan, Hubei 430074, China.
Science advances
|November 20, 2024
概括
这项研究使用光学发射线绘制了银河系周围冷的环银河系介质 (CGM). 它揭示了高达130 kiloparsec的CGM结构,显示了动荡和连贯的运动.
科学领域:
- 天文学和天体物理学
- 宇宙结构的形成宇宙结构的形成
背景情况:
- 环银河系介质 (CGM) 对银河系进化至关重要,但对其进行研究具有挑战性.
- 之前的研究依赖于堆叠的光谱,限制了单个星系的CGM绘图.
- 光学发射线为探测酷酷的CGM提供了一个有希望的途径.
研究的目的:
- 使用窄带成像进行环银河系介质 (CGM) 辐射源盲调查.
- 将单个星系的冷 (∼10^4 K) CGM映射到一个广泛的红移范围 (z ∼0 到 5).
- 描述CGM的物理特性和动态.
主要方法:
- 使用非常大望远镜 (VLT) 上的MUSE仪器的档案数据.
- 对排放线源进行广场,源盲窄带成像调查.
- 分析检测到的来源以确定CGM结构并测量其属性.
主要成果:
- 编目已解决的排放线源,追踪到130千帕克的CGM结构.
- 确定了一个与一个低质量星系的CGM (恒星质量~10^8.78 M) 相关的Hα源,z=0.1723.3.
- 在z=3.9076的星系周围检测到一个Lyα结构 (60 kpc) 和在z=1.2480.0的相互作用星系周围检测到一个[O II]特征 (130 kpc).
结论:
- 低质量银河系的CGM表现出比其银河系盘更多的动荡运动.
- 相互作用的星系在周围的CGM中显示大规模的连贯运动.
- 这项调查表明,有可能在单个星系绘制冷CGM的地图.
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