The AGORA High-resolution Galaxy Simulations Comparison Project. IV. Halo and Galaxy Mass Assembly in a Cosmological Zoom-in Simulation at z ≤ 2
(2024) In Astrophysical Journal 968(2).- 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... (More)
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.
(Less)
- author
- author collaboration
- organization
- publishing date
- 2024-06-01
- type
- Contribution to journal
- publication status
- published
- subject
- in
- Astrophysical Journal
- volume
- 968
- issue
- 2
- article number
- 125
- publisher
- American Astronomical Society
- external identifiers
-
- scopus:85196791875
- ISSN
- 0004-637X
- DOI
- 10.3847/1538-4357/ad43de
- language
- English
- LU publication?
- yes
- id
- 9b4eda27-7a8a-4b51-b9a1-555f0bea3f5f
- date added to LUP
- 2024-08-14 13:50:29
- date last changed
- 2024-08-14 13:51:30
@article{9b4eda27-7a8a-4b51-b9a1-555f0bea3f5f, abstract = {{<p>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.</p>}}, author = {{Roca-Fàbrega, Santi and Kim, Ji Hoon and Primack, Joel R. and Jung, Minyong and Genina, Anna and Hausammann, Loic and Kim, Hyeonyong and Lupi, Alessandro and Nagamine, Kentaro and Powell, Johnny W. and Revaz, Yves and Shimizu, Ikkoh and Strawn, Clayton and Velázquez, Héctor and Abel, Tom and Ceverino, Daniel and Dong, Bili and Quinn, Thomas R. and Shin, Eun Jin and Segovia-Otero, Alvaro and Agertz, Oscar and Barrow, Kirk S.S. and Cadiou, Corentin and Dekel, Avishai and Hummels, Cameron and Oh, Boon Kiat and Teyssier, Romain}}, issn = {{0004-637X}}, language = {{eng}}, month = {{06}}, number = {{2}}, publisher = {{American Astronomical Society}}, series = {{Astrophysical Journal}}, title = {{The AGORA High-resolution Galaxy Simulations Comparison Project. IV. Halo and Galaxy Mass Assembly in a Cosmological Zoom-in Simulation at z ≤ 2}}, url = {{http://dx.doi.org/10.3847/1538-4357/ad43de}}, doi = {{10.3847/1538-4357/ad43de}}, volume = {{968}}, year = {{2024}}, }