Stellar and weak lensing profiles of massive galaxies in the Hyper-Suprime Cam survey and in hydrodynamic simulations
Stellar and weak lensing profiles of massive galaxies in the Hyper-Suprime Cam survey and in hydrodynamic simulations
复制标题
DOI：
10.1093/mnras/staa3215
复制
发表时间：
2020-09
影响因子：
4.8
通讯作者：
F. Ardila;Song Huang;A. Leauthaud;B. Diemer;A. Pillepich;Rajdipa Chowdhury;D. Fiacconi;J. Greene;Andrew P. Hearin;L. Hernquist;P. Madau;L. Mayer;S. Peirani;E. Xhakaj
中科院分区：
文献类型：
--
作者：
F. Ardila;Song Huang;A. Leauthaud;B. Diemer;A. Pillepich;Rajdipa Chowdhury;D. Fiacconi;J. Greene;Andrew P. Hearin;L. Hernquist;P. Madau;L. Mayer;S. Peirani;E. Xhakaj
我们执行一个一致的质量和质量配置文件的质量（M> 1011.4 M）的中央星系在z = 0.4从深超Suprime-Cam（HSC）的观测和从Illustris，TNG 100，和Ponos模拟。来自HSC的弱透镜测量使得能够在固定晕质量下进行测量，并且提供对不同晕质量尺度下的反馈的强度和影响的约束。我们比较了恒星质量函数（SMF）和恒星晕质量关系（SHMR）在不同的半径，并表明进行比较的半径是很重要的。一般来说，Illustris和TNG 100显示更陡峭的α值，其中$M_{\星星} \propto M_{\rm vir}^{\alpha }$。这些差异对于Illustris比TNG 100更明显，并且在星系的内部而不是外部区域。内部区域的差异可能表明，TNG 100在Mvir 1013 M处淬灭原位星星形成的效率太高，但在Mvir 1014 M处不够有效。外层恒星的质量与我们在Mvir 1013 M <$3的观测结果非常一致，但Illustris和TNG 100都显示出Mvir 1014 M <$3的额外质量（分别为10.25和10.12 dex）。我们认为，在M_\星星\sim 10^{9-10} \，\mathrm{M}_{\odot }$星系中，减少早期的恒星生长将有助于防止这种质量尺度下的过度异位生长。Ponos的模拟没有实现AGN反馈，在r < 30 kpc时，与HSC相比，显示出超过0.5 dex的质量，这表明中心区域过冷和过量的星星形成。Ponos和HSC内部轮廓的比较表明，活动星系核中心限制星星形成的物理尺度为r = 20 kpc。弱透镜和星系恒星轮廓之间的联合比较是对模拟是否在正确的暗物质晕中建立和存款星系质量的直接测试，从而对反馈和星系生长的物理学提供强大的约束。我们的星系和弱透镜轮廓是公开的，以方便与其他模拟进行比较。
We perform a consistent comparison of the mass and mass profiles of massive (M⋆ > 1011.4 M⊙) central galaxies at z ∼ 0.4 from deep Hyper Suprime-Cam (HSC) observations and from the Illustris, TNG100, and Ponos simulations. Weak lensing measurements from HSC enable measurements at fixed halo mass and provide constraints on the strength and impact of feedback at different halo mass scales. We compare the stellar mass function (SMF) and the Stellar-to-Halo Mass Relation (SHMR) at various radii and show that the radius at which the comparison is performed is important. In general, Illustris and TNG100 display steeper values of α where $M_{\star } \propto M_{\rm vir}^{\alpha }$. These differences are more pronounced for Illustris than for TNG100 and in the inner rather than outer regions of galaxies. Differences in the inner regions may suggest that TNG100 is too efficient at quenching in situ star formation at Mvir ≃ 1013 M⊙ but not efficient enough at Mvir ≃ 1014 M⊙. The outer stellar masses are in excellent agreement with our observations at Mvir ≃ 1013 M⊙, but both Illustris and TNG100 display excess outer mass as Mvir ≃ 1014 M⊙ (by ∼0.25 and ∼0.12 dex, respectively). We argue that reducing stellar growth at early times in $M_\star \sim 10^{9-10} \, \mathrm{M}_{\odot }$ galaxies would help to prevent excess ex-situ growth at this mass scale. The Ponos simulations do not implement AGN feedback and display an excess mass of ∼0.5 dex at r < 30 kpc compared to HSC which is indicative of overcooling and excess star formation in the central regions. The comparison of the inner profiles of Ponos and HSC suggests that the physical scale over which the central AGN limits star formation is r ≲ 20 kpc. Joint comparisons between weak lensing and galaxy stellar profiles are a direct test of whether simulations build and deposit galaxy mass in the correct dark matter haloes and thereby provide powerful constraints on the physics of feedback and galaxy growth. Our galaxy and weak lensing profiles are publicly available to facilitate comparisons with other simulations.