The Astrophysical Journal (Jan 2024)
The AGORA High-resolution Galaxy Simulations Comparison Project. IV. Halo and Galaxy Mass Assembly in a Cosmological Zoom-in Simulation at z ≤ 2
- Santi Roca-Fàbrega,
- Ji-hoon Kim,
- Joel R. Primack,
- Minyong Jung,
- Anna Genina,
- Loic Hausammann,
- Hyeonyong Kim,
- Alessandro Lupi,
- Kentaro Nagamine,
- Johnny W. Powell,
- Yves Revaz,
- Ikkoh Shimizu,
- Clayton Strawn,
- Héctor Velázquez,
- Tom Abel,
- Daniel Ceverino,
- Bili Dong,
- Thomas R. Quinn,
- Eun-jin Shin,
- Alvaro Segovia-Otero,
- Oscar Agertz,
- Kirk S. S. Barrow,
- Corentin Cadiou,
- Avishai Dekel,
- Cameron Hummels,
- Boon Kiat Oh,
- Romain Teyssier,
- The AGORA Collaboration
Affiliations
- Santi Roca-Fàbrega
- ORCiD
- Lund Observatory, Division of Astrophysics, Department of Physics, Lund University , SE-221 00 Lund, Sweden ; [email protected]; Departamento de Física de la Tierra y Astrofísica, Facultad de Ciencias Físicas , Plaza Ciencias, 1, 28040 Madrid, Spain
- Ji-hoon Kim
- ORCiD
- Seoul National University Astronomy Research Center , Seoul 08826, Republic of Korea ; [email protected]; Center for Theoretical Physics, Department of Physics and Astronomy, Seoul National University , Seoul 08826, Republic of Korea ; [email protected]
- Joel R. Primack
- ORCiD
- Department of Physics, University of California at Santa Cruz , Santa Cruz, CA 95064, USA ; [email protected]
- Minyong Jung
- ORCiD
- Center for Theoretical Physics, Department of Physics and Astronomy, Seoul National University , Seoul 08826, Republic of Korea ; [email protected]
- Anna Genina
- ORCiD
- Max-Planck-Institut für Astrophysik , Karl-Schwarzschild-Str. 1, D-85748, Garching, Germany
- Loic Hausammann
- ORCiD
- Institute of Physics , Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne (EPFL), CH-1015 Lausanne, Switzerland; TS High Performance Computing, Eidgenössische Technische Hochschule Zürich (ETHZ) , 8092 Zürich, Switzerland
- Hyeonyong Kim
- ORCiD
- Center for Theoretical Physics, Department of Physics and Astronomy, Seoul National University , Seoul 08826, Republic of Korea ; [email protected]; Department of Aerospace Engineering, Seoul National University , Seoul 08826, Republic of Korea
- Alessandro Lupi
- ORCiD
- DiSAT, Università degli Studi dell’Insubria , via Valleggio 11, I-22100 Como, Italy; Dipartimento di Fisica “G. Occhialini,” Università degli Studi di Milano-Bicocca , I-20126 Milano, Italy
- Kentaro Nagamine
- ORCiD
- Department of Earth and Space Science, Graduate School of Science, Osaka University , Toyonaka, Osaka, 560-0043, Japan; Kavli IPMU (WPI), University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba, 277-8583, Japan; Department of Physics & Astronomy, University of Nevada Las Vegas , Las Vegas, NV 89154, USA
- Johnny W. Powell
- ORCiD
- Department of Physics, Reed College , Portland, OR 97202, USA
- Yves Revaz
- ORCiD
- Institute of Physics , Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne (EPFL), CH-1015 Lausanne, Switzerland
- Ikkoh Shimizu
- Shikoku Gakuin University , 3-2-1 Bunkyocho, Zentsuji, Kagawa, 765-8505, Japan
- Clayton Strawn
- ORCiD
- Department of Physics, University of California at Santa Cruz , Santa Cruz, CA 95064, USA ; [email protected]
- Héctor Velázquez
- Instituto de Astronomía, Universidad Nacional Autónoma de México , A.P. 70-264, 04510, Mexico, D.F., Mexico
- Tom Abel
- ORCiD
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University , Stanford, CA 94305, USA; Department of Physics, Stanford University , Stanford, CA 94305, USA; SLAC National Accelerator Laboratory , Menlo Park, CA 94025, USA
- Daniel Ceverino
- ORCiD
- Universidad Autónoma de Madrid, Ciudad Universitaria de Cantoblanco , E-28049 Madrid, Spain; CIAFF, Facultad de Ciencias, Universidad Autónoma de Madrid , E-28049 Madrid, Spain
- Bili Dong
- Department of Physics, Center for Astrophysics and Space Sciences, University of California at San Diego , La Jolla, CA 92093, USA
- Thomas R. Quinn
- ORCiD
- Department of Astronomy, University of Washington , Seattle, WA 98195, USA
- Eun-jin Shin
- ORCiD
- Center for Theoretical Physics, Department of Physics and Astronomy, Seoul National University , Seoul 08826, Republic of Korea ; [email protected]
- Alvaro Segovia-Otero
- ORCiD
- Lund Observatory, Division of Astrophysics, Department of Physics, Lund University , SE-221 00 Lund, Sweden ; [email protected]
- Oscar Agertz
- ORCiD
- Lund Observatory, Division of Astrophysics, Department of Physics, Lund University , SE-221 00 Lund, Sweden ; [email protected]
- Kirk S. S. Barrow
- ORCiD
- Department of Astronomy, University of Illinois at Urbana-Champaign , Urbana, IL 61801, USA
- Corentin Cadiou
- ORCiD
- Lund Observatory, Division of Astrophysics, Department of Physics, Lund University , SE-221 00 Lund, Sweden ; [email protected]
- Avishai Dekel
- ORCiD
- Center for Astrophysics and Planetary Science, Racah Institute of Physics, The Hebrew University , Jerusalem 91904, Israel
- Cameron Hummels
- ORCiD
- TAPIR, California Institute of Technology , Pasadena, CA 91125, USA
- Boon Kiat Oh
- ORCiD
- Center for Theoretical Physics, Department of Physics and Astronomy, Seoul National University , Seoul 08826, Republic of Korea ; [email protected]; Department of Physics, University of Connecticut , U-3046, Storrs, CT 06269, USA
- Romain Teyssier
- ORCiD
- Department of Astrophysical Sciences, Princeton University , Princeton, NJ 08544, USA
- The AGORA Collaboration
- DOI
- https://doi.org/10.3847/1538-4357/ad43de
- Journal volume & issue
-
Vol. 968,
no. 2
p. 125
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 ∼ 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.
Keywords
