年轻恒星形成星系在红移9到11的强度减弱的莱曼α吸收
Kasper E Heintz1,2, Darach Watson1,2, Gabriel Brammer1,2
1Cosmic Dawn Center, Copenhagen, Denmark.
概括
早期的星系含有惊人的大量中性原子 (H I),对于恒星形成至关重要. 这项使用JWST的发现挑战了早期宇宙和星系演变的先前模型.
科学领域:
- 宇宙学
- 银河系的演变
- 天体物理学
背景情况:
- 原始中性原子气体 (H I) 对于星系的恒星形成至关重要.
- 在早期星系中对H I的直接约束很少.
- 了解早期银河系的气体含量是宇宙进化的关键.
研究的目的:
- 在早期宇宙时代限制中性原子 (H I) 的数量 (红移 8).
- 在早期宇宙中研究年轻的恒星形成星系的气体丰富性.
主要方法:
- 詹姆斯·韦伯太空望远镜 (JWST) 近红外光谱数据的分析.
- 在遥远的星系中发现强度减弱的莱曼α吸收特征.
- 用光谱测量红移来确定宇宙距离.
主要成果:
- 三个红移值为8.8,10.2和11.4的星系 (大爆炸后的4亿到6亿年) 显示出强烈的H I吸收.
- 这些星系的HI柱密度超过10^22cm^2.
- 这些密度高于中性星系间介质的预期.
结论:
- 早期形成恒星的星系可以显著富含中性原子气.
- 这些发现表明H I的储量比早期宇宙的模型更大.
- 这种星系群可能在早期宇宙结构形成中发挥了关键作用.
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