Kavli Affiliate: Tom Abel
| First 5 Authors: R. Rodríguez-Cardoso, S. Roca-Fàbrega, Minyong Jung, Thinh Huu Nguyen, Ji-hoon Kim
| Summary:
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 (LG), satellite quenching has been shown to be
highly efficient, affecting nearly all satellites except the most massive ones.
While recent surveys are studying Milky Way (MW) analogs to assess how
representative our LG is, the dominant physical mechanisms behind satellite
quenching in MW-mass halos remain under debate. Aims: We analyze satellite
quenching within the same MW-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 (SNe) feedback physics employed. Methods: We
use a subset of high-resolution cosmological zoom-in simulations of a MW-mass
halo from the multiple-code AGORA CosmoRun suite. Results: We find that the
quenched fraction is consistent with the latest SAGA survey results within its
1$sigma$ host-to-host scatter across all the models. Regarding quenching
timescales, all the models reproduce the trend observed in the ELVES survey, LG
observations, and previous simulations: the less massive the satellite, the
shorter its quenching timescale. All our models converge on the dominant
quenching mechanisms: strangulation halts cold gas accretion and ram pressure
stripping is the predominant mechanism for gas removal, particularly effective
in satellites with $M_* < 10^8, M_odot$. Nevertheless, the efficiency of the
stripping mechanisms differs among the codes, showing a strong sensitivity to
the different SNe feedback implementations and/or hydrodynamic methods
employed.
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