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We thank all of our colleagues participating in the AGORA Project for their collaborative spirit, which has allowed the AGORA Collaboration to remain strong as a platform to foster and launch multiple science-oriented comparison efforts. We also thank Volker Springel for providing the original versions of Gadget-3 to be used in the AGORA Project. We thank the UCSC Foundation Board Opportunity Fund for supporting the AGORA Project papers as well as the AGORA annual meetings. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under contract No. DE-AC02-05CH11231 using NERSC award HEP-ERCAP0024062. S.R.-F. and O.A. acknowledge support from the Knut and Alice Wallenberg Foundation, the Swedish Research Council (grant 2019-04659), and the Swedish National Space Agency (SNSA Dnr 2023-00164). S.R.-F. also acknowledges financial support from the Spanish Ministry of Science and Innovation through projects PID2020-114581GB-C22, PID2022-138896NB-C55, and PID2021-123417ob-i00. J.K. acknowledges support from the Samsung Science and Technology Foundation under project No. SSTF-BA1802-04. His work was also supported by the National Research Foundation of Korea (NRF) grant funded by the Korean government (MSIT; Nos. 2022M3K3A1093827 and 2023R1A2C1003244). His work was also supported by the National Institute of Supercomputing and Network/Korea Institute of Science and Technology Information with supercomputing resources including technical support, grants KSC-2020-CRE-0219, KSC-2021-CRE-0442, and KSC-2022-CRE-0355. A.G. would like to thank Ruediger Pakmor, Volker Springel, Matthew Smith, and Benjamin Keller for help with Arepo and Grackle. Art-I simulations were performed on the Brigit/Eolo cluster at the Centro de Proceso de Datos, Universidad Complutense de Madrid, and on the Atocatl supercomputer at the Instituto de Astronomia de la UNAM. Ramses simulations were performed on the Miztli supercomputer at the LANACAD, Universidad Nacional Autonoma de Mexico, within the research project LANCAD-UNAM-DGTIC-151 and on the Laboratorio Nacional de Supercmputo del Sureste-Conacyt. Changa simulations were performed on the Atocatl supercomputer at the Instituto de Astronomia de la UNAM. Gadget3-Osaka simulations and analyses were performed on the XC50 systems at the Center for Computational Astrophysics (CfCA) of the National Astronomical Observatory of Japan (NAOJ), Octopus at the Cybermedia Center, Osaka University, and Oakforest-PACS at the University of Tokyo as part of the HPCI system Research Project (hp190050, hp200041). Arepo simulations were performed on the High-Performance Computing resources of the Freya cluster at the Max Planck Computing and Data Facility (MPCDF, https://www.mpcdf.mpg.de) in Garching operated by the Max Planck Society (MPG). The publicly available Enzo and yt codes used in this work are the products of collaborative efforts by many independent scientists from numerous institutions around the world. Their commitment to open science has helped make this work possible.

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The AGORA High-resolution Galaxy Simulations Comparison Project. IV. Halo and Galaxy Mass Assembly in a Cosmological Zoom-in Simulation at z ≤ 2

Publicated to:ASTROPHYSICAL JOURNAL. 968 (2): 125- - 2024-06-01 968(2), DOI: 10.3847/1538-4357/ad43de

Authors: Roca-Fabrega, Santi; Kim, Ji-hoon; Primack, Joel R; Jung, Minyong; Genina, Anna; Hausammann, Loic; Kim, Hyeonyong; Lupi, Alessandro; Nagamine, Kentaro; Powell, Johnny W; Revaz, Yves; Shimizu, Ikkoh; Strawn, Clayton; Velazquez, Hector; Abel, Tom; Ceverino, Daniel; Dong, Bili; Quinn, Thomas R; Shin, Eun-jin; Segovia-Otero, Alvaro; Agertz, Oscar; Barrow, Kirk S S; Cadiou, Corentin; Dekel, Avishai; Hummels, Cameron; Oh, Boon Kiat; Teyssier, Romain

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Abstract

In this fourth paper from the AGORA Collaboration, we study the evolution down to redshift z = 2 and below of a set of cosmological zoom-in simulations of a Milky Way mass galaxy by eight of the leading hydrodynamic simulation codes. We also compare this CosmoRun suite of simulations with dark matter-only simulations by the same eight codes. We analyze general properties of the halo and galaxy at z = 4 and 3, and before the last major merger, focusing on the formation of well-defined rotationally supported disks, the mass-metallicity relation, the specific star formation rate, the gas metallicity gradients, and the nonaxisymmetric structures in the stellar disks. Codes generally converge well to the stellar-to-halo mass ratios predicted by semianalytic models at z similar to 2. We see that almost all the hydro codes develop rotationally supported structures at low redshifts. Most agree within 0.5 dex with the observed mass-metallicity relation at high and intermediate redshifts, and reproduce the gas metallicity gradients obtained from analytical models and low-redshift observations. We confirm that the intercode differences in the halo assembly history reported in the first paper of the collaboration also exist in CosmoRun, making the code-to-code comparison more difficult. We show that such differences are mainly due to variations in code-dependent parameters that control the time stepping strategy of the gravity solver. We find that variations in the early stellar feedback can also result in differences in the timing of the low-redshift mergers. All the simulation data down to z = 2 and the auxiliary data will be made publicly available.

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