论文标题
Illustristng模拟中的银河角动量 - I.与形态，光环和黑洞质量的连接
Galactic angular momentum in the IllustrisTNG simulation -- I. Connection to morphology, halo spin, and black hole mass
论文作者
论文摘要
我们使用Illustristng项目的TNG100模拟来调查$ \ sim $ \ sim $ 12,000中央星系在$ z = 0 $中的恒星特定的角动量（$ j _ {\ ast} $），并在完整的宇宙学上，带有$ m_ {$ m _ {\ ast} $ 10^$ 10^$ 10}^$ 10^^$ 10^^$ {}^9}， {\ rm m} _ {\ odot} $。 We find that the $j_{\ast}$-$M_{\ast}$ relations for early-type and late-type galaxies in IllustrisTNG are in good overall agreement with observations, and that these galaxy types typically `retain' $\sim$10-20 and $\sim$50-60 per cent of their host haloes' specific angular momenta, respectively, with some dependence on the用于测量星系形态的方法。我们介绍了模拟星系的运动学和视觉样形态测量结果。接下来，我们将探索$ j _ {\ ast} $ - $ m _ {\ ast} $的散布相对于暗物质光环的旋转和银河系中心的超质量黑洞（BH）的质量。我们发现，居住在更快的旋转光环以及托管较少BHS的星系中倾向于具有较高特异性的角动量。我们还发现，在固定的星系或光晕质量上，光环自旋和BH质量相互相关，这可能是由于在缓慢旋转系统中朝着银河系中心的气体流向银河系中心的效率更高。最后，我们表明，光环旋转在确定星系尺寸的尺寸 - 较大的旋转光环中的较大盘形成 - 尽管趋势趋于趋势，这些趋势破裂了$ m _ {\ ast} \ gtrsim 10^{11}}}}} \，{\ rm m} _ at {被积聚的恒星主导。
We use the TNG100 simulation of the IllustrisTNG project to investigate the stellar specific angular momenta ($j_{\ast}$) of $\sim$12,000 central galaxies at $z=0$ in a full cosmological context, with stellar masses ($M_{\ast}$) ranging from $10^{9}$ to $10^{12} \, {\rm M}_{\odot}$. We find that the $j_{\ast}$-$M_{\ast}$ relations for early-type and late-type galaxies in IllustrisTNG are in good overall agreement with observations, and that these galaxy types typically `retain' $\sim$10-20 and $\sim$50-60 per cent of their host haloes' specific angular momenta, respectively, with some dependence on the methodology used to measure galaxy morphology. We present results for kinematic as well as visual-like morphological measurements of the simulated galaxies. Next, we explore the scatter in the $j_{\ast}$-$M_{\ast}$ relation with respect to the spin of the dark matter halo and the mass of the supermassive black hole (BH) at the galactic centre. We find that galaxies residing in faster spinning haloes, as well as those hosting less massive BHs, tend to have a higher specific angular momentum. We also find that, at fixed galaxy or halo mass, halo spin and BH mass are anticorrelated with each other, probably as a consequence of more efficient gas flow toward the galactic centre in slowly rotating systems. Finally, we show that halo spin plays an important role in determining galaxy sizes - larger discs form at the centres of faster-rotating haloes - although the trend breaks down for massive galaxies with $M_{\ast} \gtrsim 10^{11} \, {\rm M}_{\odot}$, roughly the mass scale at which a galaxy's stellar mass becomes dominated by accreted stars.
