标题： 通过经验模型揭示星系重子循环过程 显示英文标题

标题： Unveiling the galactic baryon cycle process by an empirical model

摘要： 我们提出一个经验模型来描述和限制星系演化过程中的重子循环过程。 该模型利用恒星质量-晕质量关系（SHMRs）在不同红移下的演化得出的恒星形成率，以及从NeutralUniverseMachine模型得出的冷气体含量，来约束模型星系中的气体吸积和气体外流再循环。 此外，通过详细模拟每个循环过程，特别是再循环过程，并利用在$z=0$处的气体相质量-金属丰度关系（MZR）作为约束，我们的模型建立了一个再循环比例与晕质量之间的关系。 发现从外流中再循环的气体比例是晕质量的函数，在晕质量为$\sim10^{10.4}M_{\rm \odot}$的星系中为$25\%$，在质量为$\sim 10^{12}M_{\rm \odot}$的晕中增加到$75\%$。 我们还发现来自FIRE-2模拟的质量载入因子与观测数据和我们的模型的约束很好地匹配。 此外，使用从流体动力学模拟中获得的星系际介质（CGM）的气体含量和金属丰度作为约束，我们的模型预测平均有$70\%$的宇宙重子吸积被吸积到晕中，且外流中未再循环的气体有$80\%$逃逸出星系，进入星系间介质（IGM）。 然而，我们注意到需要未来的观测数据来最终约束CGM和IGM之间的质量和金属交换。 显示英文摘要

摘要： We propose an empirical model to describe and constrain the baryon cycle process during galaxy evolution. This model utilizes the evolution of star formation rate, derived from the stellar mass-halo mass relations (SHMRs) across different redshifts, and the cold gas content, derived from the NeutralUniverseMachine model, to constrain gas accretion and recycle of gas outflow in the model galaxy. Additionally, through detailed modeling of each cycle process, particularly the recycling process, and utilizing the gas-phase mass-metallicity relation (MZR) at $z=0$ as a constraint, our model establishes a relation between the recycle fraction and halo mass. It is found that the fraction of gas recycled from the outflow is a function of halo mass, with a value of $25\%$ in galaxies with halo mass $\sim10^{10.4}M_{\rm \odot}$, increasing to $75\%$ in halos with mass $\sim 10^{12}M_{\rm \odot}$. We also find that the mass loading factor from the FIRE-2 simulation matches well with the constraints from both observational data and our model. Furthermore, using the gas content and metallicity of the circumgalactic medium (CGM) obtained from hydrodynamical simulations as constraints, our model predicts that on average $70\%$ of universal baryon accretion is accreted to the halo and $80\%$ of the non-recycled gas in the outflow has escaped from the galaxy, entering the intergalactic medium (IGM). However, we note that future observational data are needed to finally constrain the mass and metal exchange between the CGM and the IGM.