论文标题
在MW Halos中阐明Sidm和Baryons之间的相互作用：定义Baryons决定传热
Unraveling the interplay between SIDM and baryons in MW halos: defining where baryons dictate heat transfer
论文作者
论文摘要
我们提出了一套新的宇宙缩放模拟，对MW样星系进行了首次介绍，该模拟首次包括弹性速度依赖性的自我相互作用的暗物质（SIDM）和Illustristng物理学。通过这些模拟，我们研究了SIDM与Baryons之间的相互作用及其对星系演化过程的影响。我们还引入了一组新型的修改DMO模拟集，这些模拟可以合理地复制完全实现的流体动力学对DM光环的影响，同时简化分析并降低计算成本。我们发现，Baryons比MW样星系的SIDM散射更大程度地改变了光环的中央区域的热结构。此外，我们发现类似MW的光环的新热结构会导致SIDM产生尖锐的中央密度而不是核心，因为SIDM散射通过将热量从星系中心转移来消除热支撑。我们发现，这种效果是由Baryon收缩引起的，开始影响星系，其出色的质量为$ 10^8 $ M $ _ \ odot $，并增加了MW-Mass量表的强度。这意味着任何用于约束具有恒星质量$ 10^8 $和至少$ 10^{11} $ m $ _ \ odot $的星系的SIDM横截面的模拟都将需要Baryons来进行准确的预测。
We present a new set of cosmological zoom-in simulations of a MW-like galaxy which for the first time include elastic velocity-dependent self interacting dark matter (SIDM) and IllustrisTNG physics. With these simulations we investigate the interaction between SIDM and baryons and its effects on the galaxy evolution process. We also introduce a novel set of modified DMO simulations which can reasonably replicate the effects of fully realized hydrodynamics on the DM halo while simplifying the analysis and lowering the computational cost. We find that baryons change the thermal structure of the central region of the halo to a greater extent than the SIDM scatterings for MW-like galaxies. Additionally, we find that the new thermal structure of the MW-like halo causes SIDM to create cuspier central densities rather than cores because the SIDM scatterings remove the thermal support by transferring heat away from the center of the galaxy. We find that this effect, caused by baryon contraction, begins to affect galaxies with a stellar mass of $10^8$ M$_\odot$ and increases in strength to the MW-mass scale. This implies that any simulations used to constrain the SIDM cross sections for galaxies with stellar masses between $10^8$ and at least $10^{11}$ M$_\odot$ will require baryons to make accurate predictions.
