标题： 来自E-MOSAICS模拟的透镜状星系现今球状星团动力学及其与星系组装历史的关系 显示英文标题

标题： The present-day globular cluster kinematics of lenticular galaxies from the E-MOSAICS simulations and their relation to the galaxy assembly histories

摘要： 我们研究了来自E-MOSAICS星系形成模拟的50个透镜状（S0）星系样本中球状星团（GC）系统的现今旋转速度（$V_{rot}$）和速度弥散（${\sigma}$）分布。 我们发现，82%的星系中的球状星团沿着星系的测光主轴旋转（$aligned$），而其余18%的星系则没有（$misaligned$）。 这与SLUGGS巡天的观测结果总体上是一致的。 对于被分类为$peaked$ $and$ $outwardly$ $decreasing$ （49%）、$flat$（24%）和$increasing$（27%）的$aligned$个星系，这些分类基于大半径范围内的$V_{rot}/{\sigma}$轮廓，我们并未发现这些当前 GCs 的$V_{rot}/{\sigma}$轮廓与 S0 星系过去的合并历史之间存在任何明确的相关性，这与之前关于星系恒星的模拟结果不同。 对于大约一半的$misaligned$星系，我们发现球状星团的错配是过去 100 亿年内一次主要合并事件的结果，因此根据合并星系的轨道构型，$ex$-$situ$球状星团相对于$in$-$situ$球状星团的错配角度在 0{\deg }（同向旋转）到 180{\deg }（反向旋转）之间。 对于剩余的$misaligned$个星系，我们认为早期形成的金属贫乏的星团 ($in$-$situ$) 经历了比金属丰富的星团 ($in$-$situ$) 更频繁的动力学扰动。 我们还发现，吸积较早的球状星团和$in$-$situ$的球状星团主要位于三维相空间图中星系中心 0.2 倍视向半径（$R_{200}$）以内。 显示英文摘要

摘要： We study the present-day rotational velocity ($V_{rot}$) and velocity dispersion (${\sigma}$) profiles of the globular cluster (GC) systems in a sample of 50 lenticular (S0) galaxies from the E-MOSAICS galaxy formation simulations. We find that 82% of the galaxies have GCs that are rotating along the photometric major axis of the galaxy ($aligned$), while the remaining 18% of the galaxies do not ($misaligned$). This is generally consistent with the observations from the SLUGGS survey. For the $aligned$ galaxies, classified as $peaked$ $and$ $outwardly$ $decreasing$ (49%), $flat$ (24%) and $increasing$ (27%) based on the $V_{rot}/{\sigma}$ profiles out to large radii, we do not find any clear correlation between these present-day $V_{rot}/{\sigma}$ profiles of the GCs and the past merger histories of the S0 galaxies, unlike in previous simulations of galaxy stars. For just over half of the $misaligned$ galaxies, we find that the GC misalignment is the result of a major merger within the last 10 Gyr so that the $ex$-$situ$ GCs are misaligned by an angle between 0{\deg} (co-rotation) to 180{\deg} (counter-rotation) with respect to the $in$-$situ$ GCs, depending on the orbital configuration of the merging galaxies. For the remaining $misaligned$ galaxies, we suggest that the $in$-$situ$ metal-poor GCs, formed at early times, have undergone more frequent kinematic perturbations than the $in$-$situ$ metal-rich GCs. We also find that the GCs accreted early and the $in$-$situ$ GCs are predominantly located within 0.2 virial radii ($R_{200}$) from the centre of galaxies in 3D phase-space diagrams.