论文标题
银河系恒星对半洛的质量关系对星系形态的依赖性
The dependence of the galaxy stellar-to-halo mass relation on galaxy morphology
论文作者
论文摘要
我们研究了局部星系恒星对升压质量关系（SHMR）对星系形态的依赖性。我们使用Sloan Digital Sky调查DR7的数据以及Galaxy Zoo的形态分类，并与Eagle宇宙学模拟进行比较。在质量范围内的固定光环质量下，$ 10^{11.7} -10^{12.9} m _ {\ odot} $，SDSS盘式星系的中位数恒星质量比其椭圆形相对方的中位数高1.4倍。但是，当我们从Kauffmann等人的恒星群众切换时。对于Chang等人计算的。或Brinchmann等人，圆盘和椭圆形的中位数SHMR在此质量范围内重合。对于大于$ 10^{13} m _ {\ odot} $的光环质量，碟片在同一质量光环中的圆盘不如椭圆形，无论我们使用谁出色的质量估计。但是，我们发现对于这些高光晕质量，椎间盘的结果可能会受到中央/卫星错误分类的影响。 Eagle模拟预测，与Kauffmann等人一致，圆盘的圆盘量比与$ 10^{13} M _ {\ odot} $相比，固定在同一质量光环中的椭圆星系高1.5倍。数据。带有$ 10^{11.5} $的质量和$ 10^{12} m _ {\ odot} $的光环，主机盘式星系的组装早于寄托的椭圆形早。这表明椎间盘更大，因为它们有更多的时间积聚和恒星形成。在$ 10^{12} -10^{12.5} m _ {\ odot} $光环中，椭圆星系中的中央黑孔增长得更快，并且比在椎间星系中的对应物变得更大。这表明在这个光晕质量范围内，椭圆形的质量较小，因为AGN反馈弹出了更多的晕气体储层，减少了恒星的形成，并抑制了恒星圆盘的（RE）生长。
We investigate the dependence of the local galaxy stellar-to-halo mass relation (SHMR) on galaxy morphology. We use data from the Sloan Digital Sky Survey DR7 with morphological classifications from Galaxy Zoo, and compare with the EAGLE cosmological simulation. At fixed halo mass in the mass range $10^{11.7}-10^{12.9}M_{\odot}$, the median stellar masses of SDSS disc galaxies are up to a factor of 1.4 higher than the median masses of their elliptical counterparts. However, when we switch from the stellar masses from Kauffmann et al. to those calculated by Chang et al. or Brinchmann et al., the median SHMR from discs and ellipticals coincide in this mass range. For halo masses larger than $10^{13}M_{\odot}$, discs are less massive than ellipticals in same-mass haloes, regardless of whose stellar mass estimates we use. However, we find that for these high halo masses the results for discs may be affected by central/satellite misclassifications. The EAGLE simulation predicts that discs are up to a factor of 1.5 more massive than elliptical galaxies residing in same-mass haloes less massive than $10^{13}M_{\odot}$, in agreement with the Kauffmann et al. data. Haloes with masses between $10^{11.5}$ and $10^{12}M_{\odot}$, that host disc galaxies, were assembled earlier than those hosting ellipticals. This suggests that the discs are more massive because they had more time for gas accretion and star formation. In $10^{12}-10^{12.5}M_{\odot}$ haloes, the central black holes in elliptical galaxies grew faster and became more massive than their counterparts in disc galaxies. This suggests that in this halo mass range the ellipticals are less massive because AGN feedback ejected more of the halo's gas reservoir, reducing star formation, and suppressing the (re)growth of stellar discs.
