TY - JOUR
T1 - The agora high-resolution galaxy simulations comparison project. iii. cosmological zoom-in simulation of a milky way-mass halo
AU - Roca-Fàbrega, Santi
AU - Kim, Ji Hoon
AU - Hausammann, Loic
AU - Nagamine, Kentaro
AU - Lupi, Alessandro
AU - Powell, Johnny W.
AU - Shimizu, Ikkoh
AU - Ceverino, Daniel
AU - Primack, Joel R.
AU - Quinn, Thomas R.
AU - Revaz, Yves
AU - Velázquez, Héctor
AU - Abel, Tom
AU - Buehlmann, Michael
AU - Dekel, Avishai
AU - Dong, Bili
AU - Hahn, Oliver
AU - Hummels, Cameron
AU - Kim, Ki Won
AU - Smith, Britton D.
AU - Strawn, Clayton
AU - Teyssier, Romain
AU - Turk, Matthew J.
N1 - Funding Information:
We thank all of our colleagues who participate 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 thank Aldo Rodríguez-Puebla for sharing results from abundance matching semiempirical models, and Volker Springel for providing the original versions of GADGET-3 to be used in the AGORA Project. We also thank the anonymous referee for insightful comments and suggestions. This research used resources of the National Energy Research Scientific Computing Center, a user facility supported by the Office of Science of the U.S. Department of Energy under contract No. DE-AC02-05CH11231. S.R.-F. acknowledges support from a Spanish postdoctoral fellowship, under grant No. 2017-T2/TIC-5592. His work has been supported by the Madrid Government (Comunidad de Madrid–Spain) under the Multiannual Agreement with Complutense University in the line Program to Stimulate Research for Young Doctors in the context of V PRICIT (Regional Programme of Research and Technological Innovation). He also acknowledges financial support from the Spanish Ministry of Economy and Competitiveness under grant Nos. AYA2016-75808-R, AYA2017-90589-REDT, and S2018/ NMT-429, and from CAM-UCM under grant No. PR65/19-22462. 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 Institute of Supercomputing and Networking, Korea Institute of Science and Technology Information, with supercomputing resources, including technical support (grants KSC-2018-CRE-0052 and KSC-2019-CRE-0163). K.N. acknowledges support from MEXT/JSPS KAKENHI grant Nos. JP17H01111, 19H05810, and 20H00180, as well as travel support from Kavli IPMU, World Premier Research Center Initiative, where part of this work was conducted. A.L. acknowledges funding by the MIUR under the grant PRIN 2017-MB8AEZ. D.C. is a Ramon Cajal Researcher and is supported by Ministerio de Ciencia, Innova-ción y Universidades (FEDER) under research grant PGC2018-094975-C21. H.V. acknowledges support from PAPIIT of Universidad Nacional Autónoma de México (UNAM) under grant No. IN101918 and also from Centro Nacional de Supercomputo (CNS-IPICYT-CONACYT). The ART-I simulations were performed on the BRIGIT/EOLO cluster at Centro de Proceso de Datos, Universidad Complutense de Madrid, and on the STÓCATL supercomputer at Instituto de Astronomía de la UNAM. The RAMSES simulations were performed on the MIZTLI supercomputer at LANCAD, UNAM, within the research project LANCAD-UNAM-DGTIC-151 and on Labor-atorio Nacional de Supercómputo del Sureste, CONACYT. The CHANGA simulations were performed on the ATÓCATL supercomputer at Instituto de Astronomía de la UNAM, and on the Extreme Science and Engineering Discovery Environment (XSEDE) allocations TG-AST20020 and TG-MCA94P018. XSEDE is supported by the National Science Foundation grant ACI-1053575. The GADGET3-OSAKA simulations and analyses were performed on the XC50 systems at the Center for Computational Astrophysics of the National Astronomical Observatory of Japan, on OCTOPUS at the Cybermedia Center of Osaka University, and on Oakforest-PACS at the University of Tokyo as part of the HPCI System Research Project (hp190050 and hp200041). 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.
Publisher Copyright:
© 2021 Institute of Physics Publishing. All rights reserved.
PY - 2021/8/20
Y1 - 2021/8/20
N2 - We present a suite of high-resolution cosmological zoom-in simulations to z =4 of a 1012Me halo at z = 0, obtained using seven contemporary astrophysical simulation codes (ART-I, ENZO, RAMSES, CHANGA, GADGET-3, GEAR, and GIZMO) widely used in the numerical galaxy formation community. The physics prescriptions for gas cooling and heating and star formation are the same as the ones used in our previous Assembling Galaxies of Resolved Anatomy (AGORA) disk comparison but now account for the effects of cosmological processes such as the expansion of the universe, intergalactic gas inflow, and the cosmic ultraviolet background radiation emitted by massive stars and quasars. In this work, we introduce the most careful comparison yet of galaxy formation simulations run by different code groups, together with a series of four calibration steps each of which is designed to reduce the number of tunable simulation parameters adopted in the final run. In the first two steps, we methodically calibrate the gas physics, such as cooling and heating, in simulations without star formation. In the third step, we seek agreement on the total stellar mass produced with the common star formation prescription used in the AGORA disk comparison, in stellar-feedback-free simulations. In the last calibration step, we activate stellar feedback, where each code group is asked to set the feedback prescription to as close to the most widely used one in its code community as possible, while aiming for convergence in the stellar mass at z = 4 to the values predicted by semiempirical models. After all the participating code groups successfully complete the calibration steps, we achieve a suite of cosmological simulations with similar mass assembly histories down to z = 4. With numerical accuracy that resolves the internal structure of a target halo (≲100 physical pc at z = 4), we find that the codes overall agree well with one another, e.g., in gas and stellar properties, but also show differences, e.g., in circumgalactic medium (CGM) properties. We argue that, if adequately tested in accordance with our proposed calibration steps and common parameters, high-resolution cosmological zoom-in simulations can have robust and reproducible results. New code groups are invited to join and enrich this comparison by generating equivalent models or to test the code's compatibility on their own, by adopting the common initial conditions, the common easy-to-implement physics package, and the proposed calibration steps. Further analyses of the zoom-in simulations presented here will be presented in forthcoming reports from the AGORA Collaboration, including studies of the CGM, simulations by additional codes, and results at lower redshift.
AB - We present a suite of high-resolution cosmological zoom-in simulations to z =4 of a 1012Me halo at z = 0, obtained using seven contemporary astrophysical simulation codes (ART-I, ENZO, RAMSES, CHANGA, GADGET-3, GEAR, and GIZMO) widely used in the numerical galaxy formation community. The physics prescriptions for gas cooling and heating and star formation are the same as the ones used in our previous Assembling Galaxies of Resolved Anatomy (AGORA) disk comparison but now account for the effects of cosmological processes such as the expansion of the universe, intergalactic gas inflow, and the cosmic ultraviolet background radiation emitted by massive stars and quasars. In this work, we introduce the most careful comparison yet of galaxy formation simulations run by different code groups, together with a series of four calibration steps each of which is designed to reduce the number of tunable simulation parameters adopted in the final run. In the first two steps, we methodically calibrate the gas physics, such as cooling and heating, in simulations without star formation. In the third step, we seek agreement on the total stellar mass produced with the common star formation prescription used in the AGORA disk comparison, in stellar-feedback-free simulations. In the last calibration step, we activate stellar feedback, where each code group is asked to set the feedback prescription to as close to the most widely used one in its code community as possible, while aiming for convergence in the stellar mass at z = 4 to the values predicted by semiempirical models. After all the participating code groups successfully complete the calibration steps, we achieve a suite of cosmological simulations with similar mass assembly histories down to z = 4. With numerical accuracy that resolves the internal structure of a target halo (≲100 physical pc at z = 4), we find that the codes overall agree well with one another, e.g., in gas and stellar properties, but also show differences, e.g., in circumgalactic medium (CGM) properties. We argue that, if adequately tested in accordance with our proposed calibration steps and common parameters, high-resolution cosmological zoom-in simulations can have robust and reproducible results. New code groups are invited to join and enrich this comparison by generating equivalent models or to test the code's compatibility on their own, by adopting the common initial conditions, the common easy-to-implement physics package, and the proposed calibration steps. Further analyses of the zoom-in simulations presented here will be presented in forthcoming reports from the AGORA Collaboration, including studies of the CGM, simulations by additional codes, and results at lower redshift.
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U2 - 10.3847/1538-4357/ac088a
DO - 10.3847/1538-4357/ac088a
M3 - Article
AN - SCOPUS:85113961930
SN - 0004-637X
VL - 917
SP - 917
EP - 964
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -