The Scatter Matters: Circumgalactic Metal Content in the Context of the M–σ Relation
The Scatter Matters: Circumgalactic Metal Content in the Context of the M–σ Relation
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DOI：
10.3847/1538-4357/ad39eb
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发表时间：
2023-05
期刊：
影响因子：
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通讯作者：
N. N. Sanchez-N.;J. Werk;C. Christensen;O. Telford;M. Tremmel;T. Quinn;Jennifer Mead;Ray S. Sharma;A. Brooks
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文献类型：
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作者：
N. N. Sanchez-N.;J. Werk;C. Christensen;O. Telford;M. Tremmel;T. Quinn;Jennifer Mead;Ray S. Sharma;A. Brooks
超大质量黑洞（SMBH）反馈与环星系介质（CGM）之间的相互作用一直是星系演化中的一个悬而未决的问题。在我们的研究中，我们使用光滑粒子流体动力学模拟探索SMBH反馈对银河系金属保留和金属和气体进入和通过CGM的L* 星系的运动的影响。我们研究了140个星系从25兆秒差距的宇宙体积Romulus 25，与恒星质量之间的log（M */M）= 9.5-11.5。我们测量了每个星系的星际介质（ISM）和CGM中剩余的金属比例，并根据M BH-σ关系计算了每个SMBH的预期质量（Kormendy & Ho 2013）。每个SMBH与其预期质量的偏差ΔM BH通过σ与其宿主的电势进行比较。我们发现，吸积质量高于MBH-σ的SMBH在从ISM中去除金属方面比恒星形成星系中质量不足的SMBH更有效。总的来说，超大质量的SMBH抑制了宿主星系的星星形成，并更有效地将金属从ISM移动到CGM。然而，与其他模拟相比，我们几乎没有看到气体从CGM中排出。最后，我们预测，C iv柱密度在CGM的L* 星系是不太可能依赖于宿主星系SMBH质量。我们的研究结果表明，在低质量端的MBH-σ关系的散射可能表明如何有效的SMBH是在其宿主星系的局部质量重新分配。
The interaction between supermassive black hole (SMBH) feedback and the circumgalactic medium (CGM) continues to be an open question in galaxy evolution. In our study, we use smoothed particle hydrodynamics simulations to explore the impact of SMBH feedback on galactic metal retention and the motion of metals and gas into and through the CGM of L* galaxies. We examine 140 galaxies from the 25 Mpc cosmological volume Romulus25, with stellar masses between log(M */M ⊙) = 9.5–11.5. We measure the fraction of metals remaining in the interstellar medium (ISM) and CGM of each galaxy and calculate the expected mass of each SMBH based on the M BH–σ relation (Kormendy & Ho 2013). The deviation of each SMBH from its expected mass, ΔM BH, is compared to the potential of its host via σ. We find that SMBHs with accreted mass above M BH–σ are more effective at removing metals from the ISM than undermassive SMBHs in star-forming galaxies. Overall, overmassive SMBHs suppress the total star formation of their host galaxies and more effectively move metals from the ISM into the CGM. However, we see little to no evacuation of gas from the CGM out of their halos, in contrast with other simulations. Finally, we predict that C iv column densities in the CGM of L* galaxies are unlikely to depend on host galaxy SMBH mass. Our results show that the scatter in the low-mass end of the M BH–σ relation may indicate how effective an SMBH is in the local redistribution of mass in its host galaxy.