标题： 星系与暗物质晕的共同演化 显示英文标题

标题： The Co-Evolution Between Galaxies and Dark Matter Halos

摘要： 当前的宇宙学范式断言，暗物质晕通过层次结构形成和非线性局地（g）天体物理过程的结合，为星系的形成提供了引力支架。 这种密切关系，被称为星系-晕关联，表明暗物质晕的增长和组装影响了星系的属性。 虽然星系的恒星质量与它们的晕的质量有很强的相关性，但需要注意的是，星系-晕关联涵盖了更广泛的星系和晕属性分布。 这一分布可以通过天文观测数据和宇宙学$N$-体模拟来限制，这种方法被称为半经验建模。 通过在观测数据和宇宙结构形成模型的交叉点上运作，半经验建模从宇宙学的角度为星系形成和演化提供了有价值的见解。 在这篇进展报告中，我们利用一个新的sEM-经验模型EMPIRE，探索从矮星系到大椭圆星系的中心星系在整个宇宙时代中的恒星形成历史。 EMPIRE旨在约束连接星系和晕属性的多变量分布。 我们的研究结果揭示了中心大星系前身的不同增长阶段。 证据表明，冷流在更高的$z$时在维持恒星形成方面发挥了重要作用，而晕冲击加热在较低的$z$时变得更加突出。 最大恒星形成效率，SFE，在$z\lesssim1$的情况下发生在$M_{\rm vir \; shocks}$下方的一个因子$\sim1.5-2$。 此外，在更高的红移处， $z>1$，这个峰值有向更高质量靠拢的趋势， $M_{\rm vir}\sim 2\times 10^{12} M_{\odot}$。值得注意的是，在高于 $z\sim2$的红移处，SFE的峰值与冷气体流所表征的区域舒适地对齐。 显示英文摘要

摘要： The current cosmological paradigm asserts that dark matter halos provide the gravitational scaffolding for galaxy formation through a combination of hierarchical structure formation and non-linear local (g)astrophysical processes. This close relationship, known as the galaxy-halo connection, suggests that the growth and assembly of dark matter halos impact the properties of galaxies. While the stellar mass of galaxies correlates strongly with the mass of their halos, it is important to note that the galaxy-halo connection encompasses a broader distribution of galaxy and halo properties. This distribution can be constrained using data from astronomical observations and cosmological $N$-body simulations, a technique known as semi-empirical modeling. By operating at the intersection of observational data and the cosmological structure formation model, the semi-empirical modeling provides valuable insights into galaxy formation and evolution from a cosmological perspective. In this proceeding, we utilize a new sEM-emPIRical modEl, EMPIRE, to explore the star formation, SF, history of central galaxies across cosmic epochs, spanning from dwarfs to massive ellipticals. EMPIRE aims to constrain the multivariate distribution that links galaxy and halo properties. Our findings reveal distinct growth stages for progenitors of central massive galaxies. Evidence suggests that cold streams played a significant role in sustaining SF at higher $z$, while virial shock heating became more prominent at lower $z$. The maximum star formation efficiency, SFE, occurs at a factor of $\sim1.5-2$ below $M_{\rm vir \; shocks}$ for $z\lesssim1$. Furthermore, at higher redshifts, $z>1$, this peak tends towards higher masses, $M_{\rm vir}\sim 2\times 10^{12} M_{\odot}$. Notably, at redshifts higher than $z\sim2$, the peak of SFE aligns comfortably within the region characterized by cold streams.