论文标题
Galaxy-Halo连接模型的扩展
Extensions to models of the galaxy-halo connection
论文作者
论文摘要
我们探索了两个广泛使用的经验模型，用于银河系 - 霍尔连接，次音丰度匹配（假）和光晕占用分布（HOD），并将其预测与流体动力学模拟Illustristng（TNG）进行比较，以量化$ n _ _ _ _ rm n _ rm的星系分布的一系列统计数据范围gal} \ lot1.3 \ times10^{ - 3} \，[{\ rm mpc}/h]^{ - 3} $。我们观察到，在它们最直接的实现中，这两个模型都无法重现在TNG中测得的两点聚类。我们发现使用放松速度构建的假模型，$ v _ {\ rm放松} $，以及峰值速度，$ v _ {\ rm peak} $，表现最佳，并且相当匹配群集，尽管两次模型都没有充分捕获一次性的一正聚集。将总样本分成子人群中，我们发现，假预测高质量，蓝色，恒星形成和晚期形成的星系以及较低的较低剂的聚类是低质量，红色，静态和早期形成的星系。我们还研究了各种重型效应，发现仅黑暗材料模拟中的Subhalos比其全体物理学对应物具有始终更高的假态性能值。然后，我们考虑使用辅助参数（环境，速度各向异性，$σ^2R _ {\ rm Halfmass} $增强的HOD模型的二维实现，并进行了调整）并进行了调整，以便匹配大型尺度上的Illustristng Galaxies的两点聚类。 We analyze these galaxy populations adopting alternative statistical tools such as galaxy-galaxy lensing, void-galaxy cross-correlations and cumulants of the smoothed density field, finding that the hydrodynamical galaxy distribution disfavors $σ^2 R_{\rm halfmass}$ and the total potential as secondary parameters, while the environment and velocity anisotropy samples are consistent with检查了所有统计探针的全体物理。
We explore two widely used empirical models for the galaxy-halo connection, subhalo abundance matching (SHAM) and the halo occupation distribution (HOD) and compare their predictions with the hydrodynamical simulation IllustrisTNG (TNG) for a range of statistics that quantify the galaxy distribution at $n_{\rm gal}\approx1.3\times10^{-3}\,[{\rm Mpc}/h]^{-3}$. We observe that in their most straightforward implementations, both models fail to reproduce the two-point clustering measured in TNG. We find that SHAM models constructed using the relaxation velocity, $V_{\rm relax}$, and the peak velocity, $V_{\rm peak}$, perform best, and match the clustering reasonably well, although neither model captures adequately the one-halo clustering. Splitting the total sample into sub-populations, we discover that SHAM overpredicts the clustering of high-mass, blue, star-forming, and late-forming galaxies and uderpredicts that of low-mass, red, quiescent, and early-forming galaxies. We also study various baryonic effects, finding that subhalos in the dark-mater-only simulation have consistently higher values of their SHAM-proxy properties than their full-physics counterparts. We then consider a two-dimensional implementation of the HOD model augmented with a secondary parameter (environment, velocity anisotropy, $σ^2R_{\rm halfmass}$, and total potential) and tuned so as to match the two-point clustering of the IllustrisTNG galaxies on large scales. We analyze these galaxy populations adopting alternative statistical tools such as galaxy-galaxy lensing, void-galaxy cross-correlations and cumulants of the smoothed density field, finding that the hydrodynamical galaxy distribution disfavors $σ^2 R_{\rm halfmass}$ and the total potential as secondary parameters, while the environment and velocity anisotropy samples are consistent with full-physics across all statistical probes examined.
