星系团的DIANOGA模拟：表征原星系团中的恒星形成
The DIANOGA simulations of galaxy clusters: characterizing star formation in proto-clusters
摘要：
我们研究了恒星形成率（SFR）在宇宙学流体动力学模拟的星系（原）团的红移范围$0<z<4$，比较他们最近的观测研究，我们还研究了不同的参数的恒星形成模型对星系的性质，如SFR，恒星形成效率，气体分数的影响。我们分析了一组放大宇宙流体动力学模拟集中在12个集群。模拟进行了GADGET-3 TreePM/SPH代码，其中包括各种次网格模型来处理未解决的重子物理，包括AGN反馈。模拟没有再现原星系团核心内观察到的高SFR值，其中SFR值在$z\sim2$和$z\sim 4$均被因子$\gtrsim 4$低估。差异的出现是因为模拟无法再现观察到的星暴种群，并且在$z\sim 2$处恶化，因为模拟低估了恒星形成星系的主要序列的标准化（即，恒星质量和SFR之间的相关性）的系数为$\sim 3$。由于主序列的低标准化似乎是由低估的气体分数驱动的，目前还不清楚数值模拟是否由于预测的气体分数过低或恒星形成效率过低而错过了星暴星系。我们的结果是稳定的，对不同的恒星形成亚网格模型的几个参数，并不依赖于AGN反馈的细节。
英文摘要：
We studied the star formation rate (SFR) in cosmological hydrodynamical simulations of galaxy (proto-)clusters in the redshift range $0<z<4$, comparing them to recent observational studies; we also investigated the effect of varying the parameters of the star formation model on galaxy properties such as SFR, star-formation efficiency, and gas fraction. We analyze a set of zoom-in cosmological hydrodynamical simulations centred on twelve clusters. The simulations are carried out with the GADGET-3 TreePM/SPH code which includes various subgrid models to treat unresolved baryonic physics, including AGN feedback. Simulations do not reproduce the high values of SFR observed within protoclusters cores, where the values of SFR are underpredicted by a factor $\gtrsim 4$ both at $z\sim2$ and $z\sim 4$. The difference arises as simulations are unable to reproduce the observed starburst population and is worsened at $z\sim 2$ because simulations underpredict the normalization of the main sequence of star forming galaxies (i.e., the correlation between stellar mass and SFR) by a factor of $\sim 3$. As the low normalization of the main sequence seems to be driven by an underestimated gas fraction, it remains unclear whether numerical simulations miss starburst galaxies due to a too low predicted gas fractions or too low star formation efficiencies. Our results are stable against varying several parameters of the star formation subgrid model and do not depend on the details of the AGN feedback.
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