RT Journal Article
T1 The AGORA high-resolution galaxy simulations comparison project  VII. Satellite quenching in zoom-in simulation of a milky way-mass halo
A1 Rodríguez Cardoso, Ramón
A1 Roca Fàbrega, Santi
A1 Jung, Minyong
A1 Nguyễn, Thịnh H.
A1 Kim, Ji-hoon
A1 Primack, Joel
A1 Agertz, Oscar
A1 Barrow, Kirk S. S.
A1 Gallego Maestro, Jesús
A1 Nagamine, Kentaro
A1 Powell, Johnny W.
A1 Revaz, Yves
A1 Velázquez, Hector
A1 Genina, Anna
A1 Kim, Hyeonyong
A1 Lupi, Alessandro
A1 Abel, Tom
A1 Cen, Renyue
A1 Ceverino, Daniel
A1 Dekel, Avishai
A1 Oh, Boon Kiat
A1 Quinn, Thomas R.
AB Context. Satellite galaxies experience multiple physical processes when interacting with their host halos, often leading to the quenching of star formation. In the Local Group, satellite quenching has been shown to be highly efficient, affecting nearly all satellites except the most massive ones. While recent surveys study Milky Way-analogs to assess how representative our Local Group is, the dominant physical mechanisms behind satellite quenching in Milky Way-mass halos remain under debate.Aims. We analyze satellite quenching within the same Milky Way-mass halo simulated using various widely used astrophysical codes, each using different hydrodynamic methods and implementing different supernovae feedback recipes. The goal is to determine whether quenched fractions, quenching timescales, and the dominant quenching mechanisms are consistent across codes or if they show sensitivity to the specific hydrodynamic method and supernovae feedback physics employed.Methods. We used a subset of high-resolution cosmological zoom-in simulations of a Milky Way-mass halo from the multiple-code AGORA CosmoRun suite. Our analysis focuses on comparing satellite quenching across the different models and against observational data. We also analyzed the dominant mechanisms driving satellite quenching in each model.Results. We find that the quenched fraction is consistent with the latest SAGA Survey results within its 1σ host-to-host scatter across all the models. Regarding quenching timescales, all the models reproduce the trend observed in the ELVES survey, Local Group observations, and previous simulations: The less massive the satellite, the shorter its quenching timescale. All of our models converge on the dominant quenching mechanisms: Strangulation halts cold gas accretion in all satellites, while ram pressure stripping is the predominant mechanism for gas removal, and it is particularly effective in satellites with M*<108 M⊙. Nevertheless, the efficiency of the stripping mechanisms differs among the codes, showing a strong sensitivity to the different supernovae feedback implementations and/or hydrodynamic methods employed.
PB EDP Sciences
SN 0004-6361
YR 2025
FD 2025-06
LK https://hdl.handle.net/20.500.14352/130578
UL https://hdl.handle.net/20.500.14352/130578
LA eng
NO Rodríguez-Cardoso, R., Roca-Fàbrega, S., Jung, M., Nguyễn, T. H., Kim, J. H., Primack, J., ... & Quinn, T. R. (2025). The AGORA High-Resolution Galaxy Simulations Comparison Project-VII. Satellite quenching in zoom-in simulation of a Milky Way-mass halo. Astronomy & Astrophysics, 698, A303.
NO ©The Authors 2025.DE-AC02-05CH11231;2022M3K3A1093827;2023R1A2C1003244;KSC-2021-CRE-0442;KSC-2022-CRE-0355 ;KSC-2024-CRE-0232;20H00180;22K21349;24H00002;24H00241;
NO United States Department of Energy
NO European Commission
NO Ministerio de Ciencia e Innovación (España)
NO Agencia Estatal de Investigación (España)
NO Comunidad de Madrid
NO National Research Foundation of Korea
NO Korea Institute of Science and Technology Information
NO Center for Computational Astrophysics, National Astronomical Observatory of Japan
NO Osaka University
NO Japan Society for the Promotion of Science
NO University of Tokyo
DS Docta Complutense
RD 22 mar 2026