HIandMIGHTEE: From gas to galaxies with the MIGHTEE survey

HIandMIGHTEE：通过 MIGHTEE 调查从气体到星系

• 批准号: EP/X026639/1
• 负责人: Matthew Jarvis
• 金额: $ 262.98万
• 依托单位: University of Oxford
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2022
• 资助国家: 英国
• 起止时间: 2022 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=EP%2FX026639%2F1
• 关键词: HIandMIGHTEE; gas; galaxies; MIGHTEE; survey

One of the key elements in the formation and evolution of galaxies is the exchange of gas between the space between the stars within galaxies, their surrounding gaseous environment and the larger-scale filamentary structure in which galaxies are largely embedded. The atomic hydrogen component of this gas, which is the building block of all the objects we see in the Universe, can be traced using an emission line which is found at 21cm in the radio waveband. However, this is a very weak emission line and the vast majority of previous studies have been restricted to the very local Universe.In this project we will, for the first time, be able to detect and measure where this atomic hydrogen exists, covering a time range of around half the age of the Universe. We can therefore understand how where this gas resides has evolved over the past 6 billion years, providing much needed information on how gas cools and condenses to form the stars and galaxies we see in the Universe today.One of the novel approaches we will undertake is to use the wealth of data at other wavelengths in order to paint a complete picture of galaxy evolution, but also to be able to dig deep into the noisy data which contains the atomic hydrogen signal. We can do this as we know the position at distance of the galaxy from other data, which allows us to then extract the signal from the right place in the radio data in order to obtain a measurement of the atomic hydrogen line, regardless of whether it is detected or not. The by combining all these data we can reconstruct how much atomic hydrogen there is using advanced statistical methods.

星系形成和演化的关键要素之一是星系内恒星之间的空间、周围的气体环境以及星系大部分嵌入的更大规模的丝状结构之间的气体交换。这种气体的原子氢成分是我们在宇宙中看到的所有物体的组成部分，可以使用无线电波段 21 厘米处的发射线进行追踪。然而，这是一条非常弱的发射线，之前的绝大多数研究都仅限于非常局部的宇宙。在这个项目中，我们将第一次能够探测和测量这种原子氢存在的位置，覆盖的时间范围约为宇宙年龄的一半。因此，我们可以了解这种气体所在的位置在过去 60 亿年中是如何演化的，从而提供了有关气体如何冷却和凝结形成我们今天在宇宙中看到的恒星和星系的急需信息。我们将采取的新颖方法之一是利用其他波长的大量数据来描绘星系演化的完整图景，同时也能够深入挖掘包含原子氢信号的噪声数据。我们可以做到这一点，因为我们从其他数据中知道了星系的距离位置，这使得我们能够从无线电数据中的正确位置提取信号，以获得原子氢谱线的测量值，无论它是否被检测到。通过结合所有这些数据，我们可以使用先进的统计方法重建原子氢的含量。

项目成果

Cosmology from LOFAR Two-metre Sky Survey Data Release 2: angular clustering of radio sources

LOFAR 两米巡天数据发布 2 的宇宙学：无线电源的角聚类

• DOI: 10.1093/mnras/stad3088
• 发表时间: 2024
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Hale C

Spectral age distribution for radio-loud active galaxies in the XMM -LSS field

XMM -LSS 场中射电响亮活动星系的光谱年龄分布

• DOI: 10.1093/mnras/stad1432
• 发表时间: 2023
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Pinjarkar S

MIGHTEE-H i : the H i size-mass relation over the last billion years

MIGHTEE-H i ：过去十亿年的 H i 尺寸与质量关系

• DOI: 10.1093/mnras/stac693
• 发表时间: 2022
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Rajohnson S

MIGHTEE: deep 1.4 GHz source counts and the sky temperature contribution of star-forming galaxies and active galactic nuclei

MIGHTEE：深 1.4 GHz 源计数以及恒星形成星系和活动星系核对天空温度的贡献

• DOI: 10.1093/mnras/stac3320
• 发表时间: 2023
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Hale C

MIGHTEE: Multi-wavelength counterparts in the COSMOS field

MIGHTEE：COSMOS 领域的多波长对应物

• DOI: 10.1093/mnras/stad3307
• 发表时间: 2024
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: Whittam I