论文标题
TNG50模拟中的银河系状星系的环境介质-I：光晕气体和SMBH反馈的作用
The Circumgalactic Medium of Milky Way-like Galaxies in the TNG50 Simulation -- I: Halo Gas Properties and the Role of SMBH Feedback
论文作者
论文摘要
我们分析了来自宇宙磁磁性磁通动力学仿真TNG50的132银河介质（CGM）中气体的物理特性。样品中CGM气体的特性和丰度是多种多样的，不同阶段（冷，温暖和热）以及中性HI质量和金属质量的分数预算差异很大。 Over our stellar mass range of $10^{10.5} < M_\star / \rm{M}_\odot < 10^{10.9}$, radial profiles of gas physical properties from $0.15 < R\rm{ / R_{\rm 200c}} < 1.0$ reveal great CGM structural complexity, with significant variations both at fixed distance around individual galaxies, and跨不同的星系。 CGM气体是多相的：密度，温度和熵的分布都是多模式的，而金属性和热压分布是单峰的；一切都广泛。我们介绍了类似MW的光环中的磁场的预测：内部光环中的$ | B | \ sim \，1μ$ g的中间场强度在较大距离下迅速减小，而磁压仅在$ \ sim0.2 \ sim0.2 \ times \ rm {r_ {r_ {r_ {r_ {r_ {200c}} $之内占主导地位。 $ \ sim 10^6 \，$ k的病毒温度气体具有次级优势，$ <10^5 \，$ k分量在近似压力平衡下。最后，CGM的物理特性紧密连接到银河恒星的形成速率，进而取决于超级质量黑洞（SMBHS）的反馈。在TNG50中，我们发现来自SMBH驱动的动力风的能量会产生高速流出（$ \ gtrsim 500-2000 $ km/s），将气体加热到超级病毒温度（$> 10^{6.5-7-7} $ K），并调节流入的净额net vers vers vers offus in vers of usflos in quas ques quas ques ques ques ques ques ques ques ques ques ques quous static。
We analyze the physical properties of gas in the circumgalactic medium (CGM) of 132 Milky Way (MW)-like central galaxies at $z=0$ from the cosmological magneto-hydrodynamical simulation TNG50, part of the IllustrisTNG project. The properties and abundance of CGM gas across the sample are diverse, and the fractional budgets of different phases (cold, warm, and hot), as well as neutral HI mass and metal mass, vary considerably. Over our stellar mass range of $10^{10.5} < M_\star / \rm{M}_\odot < 10^{10.9}$, radial profiles of gas physical properties from $0.15 < R\rm{ / R_{\rm 200c}} < 1.0$ reveal great CGM structural complexity, with significant variations both at fixed distance around individual galaxies, and across different galaxies. CGM gas is multi-phase: the distributions of density, temperature and entropy are all multimodal, while metallicity and thermal pressure distributions are unimodal; all are broad. We present predictions for magnetic fields in MW-like halos: a median field strength of $|B|\sim\,1μ$G in the inner halo decreases rapidly at larger distance, while magnetic pressure dominates over thermal pressure only within $\sim0.2 \times \rm{R_{200c}}$. Virial temperature gas at $\sim 10^6\,$K coexists with a sub-dominant cool, $< 10^5\,$K component in approximate pressure equilibrium. Finally, the physical properties of the CGM are tightly connected to the galactic star formation rate, in turn dependent on feedback from supermassive black holes (SMBHs). In TNG50, we find that energy from SMBH-driven kinetic winds generates high-velocity outflows ($\gtrsim 500-2000$ km/s), heats gas to super-virial temperatures ($> 10^{6.5-7}$ K), and regulates the net balance of inflows versus outflows in otherwise quasi-static gaseous halos.
