arXivDaily arXiv每日学术速递 周一至周五更新
arXiv 2006.12102astro-ph.GA
收藏

氢原子-晕质量关系的物理驱动

The physical drivers of the atomic hydrogen-halo mass relation

Garima Chauhan, Claudia del P. Lagos, Adam R. H. Stevens, Danail Obreschkow, Chris Power, Martin Meyer

备注：
Accepted for publication in MNRAS
阅读 PDF
arXiv 页面 ↗HTML 原文 ↗

摘要：

我们使用SHARK，一个半解析的星系形成模型，研究在$0\leq z \leq 2$的HI晕质量关系的形状，散射和演化所涉及的物理过程。我们比较SHARK与HI聚类和光谱叠加的HI晕质量关系来自观测发现与前者的良好协议和HI在SHARK在$M_{\rm vir}\approx 10^{12-13} M_{\odot}$在后者的不足，但在质量阈值以下和以上的大协议。在SHARK中，我们发现HI质量随着晕质量的增加而增加，直到$\approx 10^{11.8} M_{\odot}$的临界质量;在$\sim 10^{11.8}-10^{13}M_{\odot}$之间，关系中的分散度平均增加0.7 dex，HI质量随着晕质量的增加而减少;在$M_{\rm vir} \geq 10^{13} M_{\odot}$中，HI含量继续随着晕质量的增加而增加。我们发现，$\approx 10^{12} M_{\odot}$的临界晕质量很大程度上是由活动星系核（AGN）的反馈设置的，和HI晕质量关系的确切形状和分散周围的质量是非常敏感的活动星系核反馈是如何建模，与其他物理过程中发挥不太重要的作用。我们确定的主要次要参数负责的HI晕质量关系的分散，即在$M_{\rm vir}\leq 10^{11.8} M_{\odot}$的晕自旋参数，和从子结构的总晕质量的分数贡献$M_{\rm vir}\geq 10^{13} M_{\odot}$。在$10^{11.8}<M_{\rm vir}<10^{13} M_{\odot}$的散射是最好的描述黑洞恒星质量比的中央星系，反映活动星系核反馈的相关性。我们提出了一个数值模型填充暗物质的模拟与HI在$0\leq z \leq 2$的基础上，完全晕参数，在这样的模拟是可测量的。

英文摘要：

We use SHARK, a semi-analytic galaxy formation model, to investigate the physical processes involved in dictating the shape, scatter and evolution of the HI-halo mass relation at $0\leq z \leq 2$. We compare SHARK with HI clustering and spectral stacking of the HI-halo mass relation derived from observations finding excellent agreement with the former and a deficiency of HI in SHARK at $M_{\rm vir}\approx 10^{12-13} M_{\odot}$ in the latter, but otherwise great agreement below and above that mass threshold. In SHARK, we find that the HI mass increases with the halo mass up to a critical mass of $\approx 10^{11.8} M_{\odot}$; between $\sim 10^{11.8}-10^{13}M_{\odot}$, the scatter in the relation increases by 0.7 dex and the HI mass decreases with the halo mass on average; at $M_{\rm vir} \geq 10^{13} M_{\odot}$, the HI content continues to increase with halo mass. We find that the critical halo mass of $\approx 10^{12} M_{\odot}$ is largely set by feedback from Active Galactic Nuclei (AGN), and the exact shape and scatter of the HI-halo mass relation around that mass is extremely sensitive to how AGN feedback is modelled, with other physical processes playing a less significant role. We determine the main secondary parameters responsible for the scatter of the HI-halo mass relation, namely the halo spin parameter at $M_{\rm vir}\leq 10^{11.8} M_{\odot}$, and the fractional contribution from substructure to the total halo mass for $M_{\rm vir}\geq 10^{13} M_{\odot}$. The scatter at $10^{11.8}<M_{\rm vir}<10^{13} M_{\odot}$ is best described by the black-hole-to-stellar mass ratio of the central galaxy, reflecting the AGN feedback relevance. We present a numerical model to populate dark matter-only simulations with HI at $0\leq z \leq 2$ based solely on halo parameters that are measurable in such simulations.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

↑