Kukstas, EgidijusBalogh, MichaelMcCarthy, I. G.Bahe, YannickDe Lucia, GJablonka, PascaleVulcani, BenedettaBaxter, Devontae CBiviano, AndreaCerulo, PierluigiLidman, Christopher2025-04-022025-04-020035-8711https://hdl.handle.net/1885/733746157Recent observations have shown that the environmental quenching of galaxies at z ∼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, at z ∼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* ≲ 1010 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.We thank the native Hawaiians for the use of Maunakea, as observations from Gemini, CFHT, and Subaru were all used as part of our survey. The authors thank David Barnes and Scott Kay for sharing their MACSIS simulation data with us. MB gratefully acknowledges support from the NSERC Discovery Grant program. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 769130). YMB gratefully acknowledges funding from the Netherlands Organization for Scientific Research (NWO) through Veni grant number 639.041.751. GW gratefully acknowledges support from the National Science Foundation through grant AST-1517863, and from HST program numbers GO-15294 and GO-16300. Support for program numbers GO-15294 and GO-16300 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. RD gratefully acknowledges support by the ANID BASAL projects ACE210002 and FB210003. GR gratefully acknowledges support from NSF AST-1517815, HST program numbers GO-15294 and AR-14310, and NASA ADAP award 80NSSC19K0592. MCC acknowledges support from NSF grants AST-1518257 and AST-1815475. This work used the DiRAC@Durham facility managed by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility. The equipment was funded by BEIS capital funding via STFC capital grants ST/P002293/1, ST/R002371/1, and ST/S002502/1, Durham University and STFC operations grant ST/R000832/1. DiRAC is part of the National e-Infrastructure. IPC acknowledge the financial support from the Spanish Ministry of Science and Innovation and the European Union - NextGenerationEU through the Recovery and Resilience Facility project ICTS-MRR-2021-03-CEFCA. DCB thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant 1829740, the Brinson Foundation, and the Moore Foundation; participation in the program has greatly benefited this work. FS acknowledges support by a CNES fellowship.application/pdfen-AU©2022 The authorshttp://creativecommons.org/licenses/by/4.0/hydrodynamicsgalaxies: evolutiongalaxies: groups: generalgalaxies: interactions202310.1093/mnras/stac34382023-12-17Creative Commons Attribution licence