GOGREEN: A critical assessment of environmental trends in cosmological hydrodynamical simulations at z ≈ 1
GOGREEN: A critical assessment of environmental trends in cosmological hydrodynamical simulations at z ≈ 1
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GOGREEN：对 z 至 1 处宇宙流体动力学模拟环境趋势的严格评估
DOI：
10.1093/mnras/stac3438
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发表时间：
2022
影响因子：
4.8
通讯作者：
Cerulo, Pierluigi
中科院分区：
文献类型：
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作者：
Kukstas, Egidijus;Balogh, Michael L.;McCarthy, Ian G.;Bahé, Yannick M.;De Lucia, Gabriella;Jablonka, Pascale;Vulcani, Benedetta;Baxter, Devontae C.;Biviano, Andrea;Cerulo, Pierluigi
最近的观测表明，星系在Z∼1的环境猝灭与局部宇宙的环境猝灭有本质上的不同。然而，这些差异的物理根源尚未阐明。此外，虽然观测到的环境趋势和宇宙流体动力学模拟的预测之间的低红移比较现在是例行公事，但到目前为止，在较高红移的情况下进行比较的相对较少。在这里，我们面对三个最先进的模拟套件(巴哈马+MACSIS，EAGLE+Hydrangea，IllustrisTNG)，分别使用来自COSMOS/UltraVISTA和GoGreen调查的最先进的现场和星团环境观测，ATZ∼1，以评估模拟的真实性，并深入了解环境猝灭的演变。我们表明，虽然这些模拟通常复制了野外静止和恒星形成星系的恒星含量和恒星质量函数，但所有的模拟都难以捕捉到星团环境中观察到的卫星猝灭，因为它们在猝灭低质量卫星方面过于有效。此外，其中两个套件不能充分熄灭星系团中质量最高的星系，这可能是来自活动星系核的反馈不足的结果。尽管在分辨率、反馈实现和流体力学解算器上存在很大的差异，但在所有的模拟中都存在低恒星质量(M⊙)的差异的原因尚不清楚。下一代模拟将推动更高的分辨率，并包括对寒冷的星际介质进行显式建模，这可能有助于我们揭示低质量张力。
Recent observations have shown that the environmental quenching of galaxies atz∼ 1 is qualitatively different to that in the local Universe. However, the physical origin of these differences has not yet been elucidated. In addition, while low-redshift comparisons between observed environmental trends and the predictions of cosmological hydrodynamical simulations are now routine, there have been relatively few comparisons at higher redshifts to date. Here we confront three state-of-the-art suites of simulations (BAHAMAS+MACSIS, EAGLE+Hydrangea, IllustrisTNG) with state-of-the-art observations of the field and cluster environments from the COSMOS/UltraVISTA and GOGREEN surveys, respectively, atz∼ 1 to assess the realism of the simulations and gain insight into the evolution of environmental quenching. We show that while the simulations generally reproduce the stellar content and the stellar mass functions of quiescent and star-forming galaxies in the field, all the simulations struggle to capture the observed quenching of satellites in the cluster environment, in that they are overly efficient at quenching low-mass satellites. Furthermore, two of the suites do not sufficiently quench the highest mass galaxies in clusters, perhaps a result of insufficient feedback from AGN. The origin of the discrepancy at low stellar masses (M⊙), which is present in all the simulations in spite of large differences in resolution, feedback implementations, and hydrodynamical solvers, is unclear. The next generation of simulations, which will push to significantly higher resolution and also include explicit modelling of the cold interstellar medium, may help us to shed light on the low-mass tension.