Dianoga星系团与星系群的模拟：重子成分的性质
Dianoga simulations of galaxy clusters and groups: Properties of the baryonic components
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中文总结 AI 辅助
本文通过Dianoga宇宙学模拟套件，结合OpenGadget3代码，研究AGN反馈与恒星形成对星系团等重子成分性质的影响，揭示AGN能量注入与亚分辨率星际介质模型界面细节的重要性。
中文摘要 AI 辅助
我们推出了Dianoga星系团与星系群宇宙学模拟套件，专门用于研究活动星系核（AGN）反馈和恒星形成实施的影响。使用OpenGadget3代码，我们对28个以大质量星系团为中心的区域以及一个宇宙学盒子进行了模拟，生成了包含293个质量M₂₀₀>1.5×10¹³M⊙的晕的样本。参考实施中AGN反馈的参数仅通过匹配本地超大质量黑洞（SMBH）质量与宿主星系恒星质量的关系进行了最小程度的校准。我们将模拟结果与观测到的星系恒星质量函数（GSMF）、星系团与星系群中的恒星质量分数、 brightest cluster galaxy（BCG）质量、星系际介质（ICM）/星系间介质（IGM）性质及其热力学性质轮廓的标度关系进行了比较。在附录中，我们展示了修改参考反馈模型的六种替代配置下结果的变化情况。我们的参考模型预测的GSMF总体与观测一致，尽管在高值端存在高估；大质量星系团的BCG恒星质量和质量分数高于观测值，而星系群的则更接近观测值；预测的ICM/IGM性质总体与观测一致，模拟星系团的核心区域熵和温度轮廓的“冷核”程度略低于观测值。与其他AGN反馈实施的比较表明，包含亚分辨率星际介质热蒸发的模型成功使BCG质量和恒星质量分数更接近观测值，并提高了模拟星系团的冷核程度。我们的结果表明，AGN能量注入与亚分辨率星际介质模型之间的界面细节至少与总反馈效率本身同样关键。
英文摘要
We introduce the Dianoga set of cosmological simulations of galaxy clusters and groups, specifically aimed at studying the impact of the implementation of AGN feedback and star formation. Using the OpenGadget3 code, we carry out simulations of 28 regions centred on massive galaxy clusters, and of a cosmological box. This generates a sample of 293 halos with M_{200}> 1.5 x 10^{13} M_{\odot}. Parameters of AGN feedback in the reference implementation were minimally calibrated exclusively to match the local relation between SMBH masses and stellar masses of host galaxies. Simulations are compared to observed galaxy stellar mass function (GSMF), stellar mass fraction in clusters and groups, BCG masses, scaling relations between ICM/IGM properties and profiles of their thermodynamical properties. In the appendix, we show how results vary as we modify the reference feedback model in six alternative configurations. Our reference model predicts a GSMF in general agreement with observations, albeit overestimated in the high end. BCG stellar masses and mass fractions are higher than observed in massive clusters, while being closer to observations for groups. Predicted properties of the ICM/IGM are in general agreement with observations, with the core regions of simulated clusters having entropy and temperature profiles that are slightly less "cool-cored" than observed. A comparison with other implementations of AGN feedback highlights that models including thermal evaporation of the sub-resolution interstellar medium succeed to bring BCG masses and stellar mass fractions closer to observation, and to increase the cool-coreness of simulated clusters. Our results demonstrate that the details of the interface between AGN energy injection and the sub-resolution interstellar medium model are at least as critical as the total feedback efficiency itself.
