We present a variation of the recently updated Munich semi-analytical galaxy formation model, L-Galaxies, with a new gas stripping method. Extending earlier work, we directly measure the local environmental properties of galaxies to formulate a more accurate treatment of ram-pressure stripping for all galaxies. We fully recalibrate the modified L-Galaxies model using a Markov Chain Monte Carlo (MCMC) method with the stellar mass function and quenched fraction of galaxies as a function of stellar mass at 0 ≤ z ≤ 2 as constraints. Due to this recalibration, global galaxy population relations, including the stellar mass function, quenched fractions versus galaxy mass, and H i mass function are all largely unchanged and remain consistent with observations. By comparing to data on galaxy properties in different environments from the SDSS and HSC surveys, we demonstrate that our modified model improves the agreement with the quenched fractions and star formation rates of galaxies as a function of environment, stellar mass, and redshift. Overall, in the vicinity of haloes with total mass 1012 to $10^{15}\, \rm M_{\odot }$ at z = 0, our new model produces higher quenched fractions and stronger environmental dependencies, better recovering observed trends with halocentric distance up to several virial radii. By analysing the actual amount of gas stripped from galaxies in our model, we show that those in the vicinity of massive haloes lose a large fraction of their hot halo gas before they become satellites. We demonstrate that this affects galaxy quenching both within and beyond the halo boundary. This is likely to influence the correlations between galaxies up to tens of megaparsecs.

中文翻译：

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用 L-GALAXIES 形成星系：模拟星系演化的环境依赖性并与观测结果进行比较

我们提出了最近更新的慕尼黑半解析星系形成模型 L-Galaxies 的一种变体，它采用了一种新的气体剥离方法。扩展早期工作，我们直接测量星系的局部环境特性，以制定更准确的处理所有星系的冲压压力剥离。我们使用马尔可夫链蒙特卡罗 (MCMC) 方法完全重新校准修改后的 L 星系模型，其中恒星质量函数和星系的淬火分数作为 0 ≤ z ≤ 2 处恒星质量的函数作为约束条件。由于这种重新校准，全球星系种群关系，包括恒星质量函数、淬火分数与星系质量的关系以及 H i 质量函数都基本上没有变化，并且与观测结果保持一致。通过比较来自 SDSS 和 HSC 调查的不同环境中星系属性的数据，我们证明我们的修改后的模型改进了与星系的淬火分数和恒星形成率作为环境、恒星质量和红移函数的一致性。总体而言，在总质量为 1012 到 $10^{15}\, \rm M_{\odot }$ 在 z = 0 的晕圈附近，我们的新模型产生更高的淬火分数和更强的环境依赖性，更好地恢复观察到的以晕为中心的趋势距离可达几个维里半径。通过在我们的模型中分析从星系中剥离的实际气体量，我们表明，在大质量晕附近的那些在成为卫星之前会失去大部分的热晕气体。我们证明这会影响光晕边界内外的星系淬火。