论文标题
反馈重塑光环，霍洛郊区及以后的巴里昂分布：从矮人到巨大的簇的闭合半径
Feedback reshapes the baryon distribution within haloes, in halo outskirts, and beyond: the closure radius from dwarfs to massive clusters
论文作者
论文摘要
我们探索三组宇宙学流体动力学模拟，Illustristng，Eagle和Simba，以研究影响在空光中及周围在光晕周围分布的物理过程中，前所未有的质量范围为$ 10^8 <m _ {\ rm 200C}/{\ rm m _ {\ rm m _ {\ rm m _ {大于$ 30 \，r _ {\ rm 200c} $。我们证明，重型反馈机制显着重新分配气体，降低了光环内部的bary级分数，同时将这种材料堆积在病毒半径之外。为了理解这种大规模的重型重新分布并确定负责的主要物理过程，我们检查了几种TNG的变体，它们有选择地排除了恒星和AGN的反馈，冷却和辐射。我们发现，低质量光环中的紫外线背景，中间质量光环中的恒星反馈和AGN反馈分组（$ 10^{12} \ leq m _ {\ rm 200C}/{\ rm m _ {\ rm m _ {\ odot}} <10^{14} $）是统治。星系群是受这些过程在大尺度上影响最小的。我们引入了一个新的Halo质量依赖性特征刻度，即闭合半径$ r _ {\ rm c} $，其中所有与光环相关的重子被发现。对于组和群集，我们在此量表和光环baryon部分之间介绍了一个普遍的关系：$ r _ {\ rm c}/r _ {\ rm 200c，500c}，500c} -1 =β（z）（z）（1-f _ {\ rm b} b，cosmic}）$，其中$β（z）=α\，（1+z）^γ$，$α$和$α$和$γ$是使用模拟的免费参数。因此，我们预测在$ r _ {\ rm c} \ sim 1.5-2.5 r _ {\ rm 200c} $之内，可以找到与观察到的X射线光环相关的所有重子。我们的结果可用于约束理论模型，尤其是超新星和AGN反馈的物理学，以及它们与环境过程的相互作用，通过与当前和未来的X射线和SZ观测值进行比较。
We explore three sets of cosmological hydrodynamical simulations, IllustrisTNG, EAGLE, and SIMBA, to investigate the physical processes impacting the distribution of baryons in and around haloes across an unprecedented mass range of $10^8<M_{\rm 200c}/{\rm M_{\odot}}<10^{15}$, from the halo centre out to scales as large as $30\,R_{\rm 200c}$. We demonstrate that baryonic feedback mechanisms significantly redistribute gas, lowering the baryon fractions inside haloes while simultaneously accumulating this material outside the virial radius. To understand this large-scale baryonic redistribution and identify the dominant physical processes responsible, we examine several variants of TNG that selectively exclude stellar and AGN feedback, cooling, and radiation. We find that heating from the UV background in low-mass haloes, stellar feedback in intermediate-mass haloes, and AGN feedback in groups ($10^{12} \leq M_{\rm 200c}/{\rm M_{\odot}}<10^{14}$) are the dominant processes. Galaxy clusters are the least influenced by these processes on large scales. We introduce a new halo mass-dependent characteristic scale, the closure radius $R_{\rm c}$, within which all baryons associated with haloes are found. For groups and clusters, we introduce a universal relation between this scale and the halo baryon fraction: $R_{\rm c}/R_{\rm 200c,500c}-1=β(z)(1-f_{\rm b}(<R_{\rm 200c,500c})/f_{\rm b,cosmic})$, where $β(z)=α\,(1+z)^γ$, and $α$ and $γ$ are free parameters fit using the simulations. Accordingly, we predict that all baryons associated with observed X-ray haloes can be found within $R_{\rm c}\sim 1.5-2.5 R_{\rm 200c}$. Our results can be used to constrain theoretical models, particularly the physics of supernova and AGN feedback, as well as their interplay with environmental processes, through comparison with current and future X-ray and SZ observations.
