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arXiv 2106.01973astro-ph.GA
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星系HI -（次）晕连接和局域星系的HI空间成团

The galaxy HI-(sub)halo connection and the HI spatial clustering of local galaxies

A. R. Calette, Aldo Rodríguez-Puebla, Vladimir Avila-Reese, Claudia del P. Lagos

备注：
In press, 20 pages, 19 figures. Some corrections in text, references added. Results unchanged
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摘要：

我们扩展本地恒星星系（子）晕连接到原子氢（HI）的组成部分，通过播种半经验星系到一个大的N体暗物质（DM）模拟。构建模拟星系目录的主要输入是：我们的约束恒星质量（子）晕圆速度（$M_{\ast}$ - $V_{\rm DM}$）的关系，假设一个独立的任何星系属性的散射，和经验的$M_{\rm HI}$条件概率分布$M_{\ast}$为中心和卫星星系。我们发现$\langle\log M_{\rm HI}\rangle-\log M_{\rm DM}$关系不是单调递增函数。它随质量增加，直至$M_{\rm DM}\sim 10^{12}$ $M_{\odot}$，达到$\langle\log(M_{\rm HI}/M_{\odot})\rangle \sim 9.2$的最大值，在较高（亚）晕质量时，$\langle\log(M_{\rm HI})\rangle$随$M_{\rm DM}$略微降低。它周围的散射也很大，并且依赖于质量。二元$M_{\rm HI}$和$M_{\rm DM}$分布是宽的和双峰的，特别是在$M_{\rm DM}\gtrsim 10^{12}$ $M_\odot$处，其继承自输入$M_{\rm HI}$条件分布。我们还报告了总（中央+卫星）HI气体质量晕内，$\langle M^{\rm tot}_{\rm HI}(M_{\rm DM})\rangle$，作为$M_{\rm DM}$的函数。平均$M^{\rm tot}_{\rm HI}-M_{\rm DM}$关系是单调递增函数。星系的空间聚集随$M_{\rm HI}$阈值的增加而微弱地增加。我们的HI模拟星系集群相比，盲目的HI ALCAFA（阿雷西博快速遗产ALFA）调查，但我们表明，这主要是由于选择效应。我们讨论了我们的研究结果的影响，从半解析模型和流体力学模拟星系演化的预测。

英文摘要：

We extend the local stellar galaxy-(sub)halo connection to the atomic hydrogen (HI) component by seeding semi-empirically galaxies into a large N-body dark matter (DM) simulation. The main input to construct the mock galaxy catalogue are: our constrained stellar mass-to-(sub)halo circular velocity ($M_{\ast}$-$V_{\rm DM}$) relation, assuming a scatter independent of any galaxy property, and the empirical $M_{\rm HI}$ conditional probability distributions given $M_{\ast}$ for central and satellite galaxies. We find that the $\langle\log M_{\rm HI}\rangle-\log M_{\rm DM}$ relation is not a monotonic increasing function. It increases with mass up to $M_{\rm DM}\sim 10^{12}$ $M_{\odot}$, attaining a maximum of $\langle\log(M_{\rm HI}/M_{\odot})\rangle \sim 9.2$, and at higher (sub)halo masses, $\langle\log(M_{\rm HI})\rangle$ decreases slightly with $M_{\rm DM}$. The scatter around it is also large and mass dependent. The bivariate $M_{\rm HI}$ and $M_{\rm DM}$ distribution is broad and bimodal, specially at $M_{\rm DM}\gtrsim 10^{12}$ $M_\odot$, which is inherited from the input $M_{\rm HI}$ conditional distributions. We also report the total (central+satellites) HI gas mass within halos, $\langle M^{\rm tot}_{\rm HI}(M_{\rm DM})\rangle$, as a function of $M_{\rm DM}$. The mean $M^{\rm tot}_{\rm HI}-M_{\rm DM}$ relation is an increasing monotonic function. The galaxy spatial clustering increases weakly as the $M_{\rm HI}$ threshold increases. Our HI mock galaxies cluster more in comparison to the blind HI ALFALFA (Arecibo Fast Legacy ALFA) survey but we show that it is mainly due to the selection effects. We discuss the implications of our results in the light of predictions from semi-analytical models and hydrodynamics simulations of galaxy evolution.

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