How do galaxies populate dark matter haloes
How do galaxies populate dark matter haloes
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DOI：
10.1111/j.1365-2966.2010.16341.x
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发表时间：
2009-09
影响因子：
4.8
通讯作者：
Q. Guo;S. White;Cheng Li;M. Boylan-Kolchin
中科院分区：
文献类型：
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作者：
Q. Guo;S. White;Cheng Li;M. Boylan-Kolchin
对于任何假设的标准恒星初始质量函数，斯隆数字巡天（SDSS）给出了在整个恒星质量范围108 M（圆点）< M（*）< 1012 M（圆点）内星系丰度的精确测定。在和谐的拉姆达冷暗物质（拉姆达CDM）宇宙学中，千禧年模拟给出了精确的晕丰度作为星系形成的所有晕的质量和红移的函数。在星系的恒星质量是其晕所达到的最大质量的增函数这一合理假设下，这些结果联合收割机给出了晕质量作为恒星质量的函数。结果同意相当好的观测估计的平均晕质量作为恒星质量的函数从叠加分析的引力透镜信号和卫星动力学的SDSS星系。对于M（*）类似于5.5 x 1010 M（圆点），通常假设银河系（MW）的恒星质量，隐含的晕质量类似于2 x 1012 M（圆点），与最近的直接估计和MW/M31时间参数的推论一致。与每个晕相关的重子在其中心星系中以恒星形式存在的比例在质量略低于MW时达到最大值20%，在质量较高和较低时福尔斯都迅速下降。这些转换效率比几乎所有最近的高分辨率星系形成模拟都要低，这表明这些还不是星系群典型成员形成的可行模型。当插入到千禧年-II模拟，我们推导出的恒星质量和晕质量之间的关系预测恒星质量的自相关函数与直接在SDSS测量的非常一致。隐含的塔利-费舍尔关系似乎也与观测相一致，这表明星系光度函数和塔利-费舍尔关系可以在Lambda CDM宇宙学中同时重现。
For any assumed standard stellar initial mass function, the Sloan Digital Sky Survey (SDSS) gives a precise determination of the abundance of galaxies as a function of their stellar mass over the full stellar mass range 108 M(circle dot) < M(*) < 1012 M(circle dot). Within the concordance Lambda cold dark matter (Lambda CDM) cosmology, the Millennium Simulations give precise halo abundances as a function of mass and redshift for all haloes within which galaxies can form. Under the plausible hypothesis that the stellar mass of a galaxy is an increasing function of the maximum mass ever attained by its halo, these results combine to give halo mass as a function of stellar mass. The result agrees quite well with observational estimates of mean halo mass as a function of stellar mass from stacking analyses of the gravitational lensing signal and the satellite dynamics of SDSS galaxies. For M(*) similar to 5.5 x 1010 M(circle dot), the stellar mass usually assumed for the Milky Way (MW), the implied halo mass is similar to 2 x 1012 M(circle dot), consistent with most recent direct estimates and inferences from the MW/M31 timing argument. The fraction of the baryons associated with each halo which are present as stars in its central galaxy reaches a maximum of 20 per cent at masses somewhat below that of the MW and falls rapidly at both higher and lower masses. These conversion efficiencies are lower than in almost all recent high-resolution simulations of galaxy formation, showing that these are not yet viable models for the formation of typical members of the galaxy population. When inserted in the Millennium-II Simulation, our derived relation between stellar mass and halo mass predicts a stellar mass autocorrelation function in excellent agreement with that measured directly in the SDSS. The implied Tully-Fisher relation also appears consistent with observation, suggesting that galaxy luminosity functions and Tully-Fisher relations can be reproduced simultaneously in a Lambda CDM cosmology.