黑暗中的隆隆声：超大质量黑洞动力学和星系密度剖面中自相互作用暗物质的特征
A rumble in the dark: signatures of self-interacting dark matter in Super-Massive Black Hole dynamics and galaxy density profiles
摘要：
首次探讨了流体动力学宇宙学模拟中自相互作用暗物质（SIDM）对大质量星系中暗物质（DM）和重子分布的影响，包括显式重子物理处理.一种新的实现超大质量黑洞（SMBH）的形成和演化的使用，在Tremmel等人。(2015，2016），允许明确遵循星系中心的SMBH动力学。选择高SIDM恒定横截面，$σ$ =10 $\rm cm^2/gr$，以放大与CDM模型的差异。类似银河系的星系在SIDM中形成的DM密度分布比在CDM中形成的DM密度分布更浅，差异已经达到20 kpc尺度。这表明，即使对于最大质量的螺旋，SIDM的影响也超过了重子引起的绝热收缩。引人注目的是，SMBHs的动态在SIDM和参考CDM情况下不同。在SIDM和CDM运行中，大质量螺旋中的SMBH都沉到了宿主星系的中心，而在较小质量的星系中，SIDM运行中大约有80个$\%$的SMBH人口偏离了中心，而在CDM运行中，$\sim$ 90个$\%$的SMBH已经到达了宿主星系的中心。SMBH被发现在距离SIDM星系中心$\sim$ 9千秒差距的地方。这种差异是由于SIDM星系中DM密度较CDM低而导致的动力学摩擦时间尺度增加，从而导致“核心失速”。这项试点工作突出了在一个完整的流体动力学背景下，不同的DM模型相结合的SMBH物理模拟的重要性，研究它们对星系形成的影响。
英文摘要：
We explore for the first time the effect of self-interacting dark matter (SIDM) on the dark matter (DM) and baryonic distribution in massive galaxies formed in hydrodynamical cosmological simulations, including explicit baryonic physics treatment. A novel implementation of Super-Massive Black Hole (SMBH) formation and evolution is used, as in Tremmel et al.(2015, 2016), allowing to explicitly follow SMBH dynamics at the center of galaxies. A high SIDM constant cross-section is chosen, $σ$=10 $\rm cm^2/gr$, to amplify differences from CDM models. Milky Way-like galaxies form a shallower DM density profile in SIDM than they do in CDM, with differences already at 20 kpc scales. This demonstrates that even for the most massive spirals the effect of SIDM dominates over the adiabatic contraction due to baryons. Strikingly, the dynamics of SMBHs differs in the SIDM and reference CDM case. SMBHs in massive spirals have sunk to the centre of their host galaxy in both the SIDM and CDM run, while in less massive galaxies about 80$\%$ of the SMBH population is off-centered in the SIDM case, as opposed to the CDM case in which $\sim$90$\%$ of SMBHs have reached their host's centre. SMBHs are found as far as $\sim$9 kpc away from the centre of their host SIDM galaxy. This difference is due to the increased dynamical friction timescale caused by the lower DM density in SIDM galaxies compared to CDM, resulting in 'core stalling'. This pilot work highlights the importance of simulating in a full hydrodynamical context different DM models combined to SMBH physics to study their influence on galaxy formation.
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