AI 中文总结
研究现代流体动力学模拟中星系形成模型的挑战，通过对比三个模拟与实测数据，发现不同反馈方案存在问题，当前反馈模型不完整，需重新审视次网格反馈方案，开发更自洽模型调节星系增长和晕气体热力学性质。
AI 中文摘要
在现代流体动力学模拟中，精确平衡宇宙时间内的气体储库、恒星形成和反馈，仍是星系形成模型的核心挑战。不同反馈方案在重现局部星系属性上效果各异，预测暗物质晕的热气体含量时差异显著。研究了Magneticum、IllustrisTNG和SIMBA这三个模拟，将其预测与MaNGA的空间分辨星系数据以及eROSITA和Sunyaev-Zel'dovich测量得到的热气体质量分数-晕质量关系的最新约束进行对比。重现观测到的fgas-Mh关系需要强大的活动星系核反馈，但这常导致模拟星系过度熄灭。Magneticum和SIMBA匹配了观测到的气体分数关系，但预测的熄灭星系过多。IllustrisTNG的活动星系核反馈较弱，恒星形成分数更现实，但在大质量星系群和贫星系团中系统地高估了热气体质量。这些矛盾表明当前反馈模型不完整，强调需要重新审视次网格反馈方案，开发更自洽的模型来同时调节星系增长和晕气体的热力学性质。
英文摘要
Accurately balancing gas reservoirs, star formation, and feedback across cosmic time remains a central challenge for galaxy formation models in modern hydrodynamical simulations. While different feedback prescriptions reproduce selected local galaxy properties with varying success, the most pronounced discrepancies emerge in predictions for the hot gas content of dark matter halos. We examine three state-of-the-art cosmological simulations: Magneticum, IllustrisTNG, and SIMBA, which struggle to simultaneously reproduce observed galaxy and halo gas properties in the local Universe. We confront their predictions with spatially resolved galaxy data from MaNGA and recent constraints on the hot gas mass fraction-halo mass (fgas-Mh) relation from eROSITA and Sunyaev-Zel'dovich (SZ) measurements. Reproducing the observed fgas-Mh relation requires strong active galactic nucleus (AGN) feedback. However, such feedback often leads to excessive quenching in simulated galaxy populations. Magneticum and SIMBA match the observed gas fraction relation but predict an overabundance of quenched galaxies. In contrast, IllustrisTNG implements weaker AGN feedback, yielding more realistic star-forming fractions but systematically overpredicting hot gas masses in massive groups and poor clusters. Overall, these tensions indicate current feedback models remain incomplete, not only in the total energy injected but also in the timing, location, and coupling of this energy to the surrounding gas. Our results therefore highlight the need to revisit subgrid feedback prescriptions and develop more self-consistent models capable of simultaneously regulating galaxy growth and the thermodynamic properties of halo gas. Motivated by this discrepancy, a companion study will explore whether the feedback strengths required to match halo gas constraints inevitably lead to overquenching and distorted galaxy demographics.
Comments14 pages, 11 figures + appendix. Modified abstract to match the arXiv guidelines. Accepted by A&A
