论文标题
恒星形成和化学富集
Star Formation and Chemical Enrichment in Protoclusters
论文作者
论文摘要
我们使用宇宙缩放的流体动力模拟检查了恒星形成和化学富集（PC）。我们发现所有PC中的总星形形成率（SFR）（$> 10^{14.4} \，h^{ - 1} $ m $ _ \ odot $）到达$> 10^4 \，\ Mathrm {m} _ \ odot \ odot \ odot \ odot \ odot \ mathrm {yr}^yr}^{yr}^{ - 1} $ z $ z $ z $ z $ z = 3 $ s = 3 $ quist and pc cob at pc cob at pc cob at pc and cob at pc cob at pc cob at pc。核心区域中的SFR约占PC中$ z \ gtrsim1 $的$ 30 \％$，这表明外部区域对揭示星系簇的演变的重要性。我们发现，PC的总SFR由$ 10^{10} \，\ le \，（\ Mathrm {M} _ \ star/m_ \ odot）\，\ le \，10^{11} $支配，而更多的大型星系在核心中占主导地位。对于化学丰度的演化，我们发现高密度区域具有较高的金属性和更快的演化。我们表明，由于IA型超新星的Fe富集，[O/Fe]与[Fe/H]的关系在$ z = 3.4 $中拒绝。我们没有发现质量 - 金属关系（MZR）或$ \ log $（n/o）与$ 12+\ log $（o/h）的环境影响。我们发现，在高红移宇宙（$ z> 1 $）中，星系簇中的化学富集速度更快。我们的工作将使未来的层析成像观测值受益，尤其是使用PC作为宇宙高密度区域加速结构形成和进化的独特探针。
We examine star formation and chemical enrichment in protoclusters (PCs) using cosmological zoom-in hydrodynamic simulations. We find that the total star formation rate (SFR) in all PC ($>10^{14.4}\,h^{-1}$M$_\odot$) reaches $>10^4\,\mathrm{M}_\odot \mathrm{yr}^{-1}$ at $z=3$, equivalent to the observed PCs. The SFR in the Core region accounts for about $30\%$ of the total star formation in the PC at $z\gtrsim1$, suggesting the importance of the outer regions to reveal the evolution of galaxy clusters. We find that the total SFR of PC is dominated by galaxies with $10^{10}\,\le\,(\mathrm{M}_\star/M_\odot)\,\le\,10^{11}$, while more massive galaxies dominate the SFR in the Core. For the chemical abundance evolution, we find that the higher-density region has a higher metallicity and faster evolution. We show that the [O/Fe] vs. [Fe/H] relation turns down in the Core at $z=3.4$ due to the enrichment of Fe by Type Ia supernovae. We find no environmental effects for the mass--metallicity relations (MZR) or $\log$(N/O) vs. $12+\log$(O/H) for galaxies. We find that the chemical enrichment in galaxy clusters proceeds faster in the high redshift Universe ($z>1$). Our work will benefit future tomographic observations, particularly using PCs as unique probes of accelerated structure formation and evolution in high-density regions of the universe.
