Tracing stars in Milky Way satellites with A-SLOTH
Li-Hsin Chen, Mattis Magg, Tilman Hartwig, Simon C. O. Glover,, Alexander P. Ji, and Ralf S. Klessen

TL;DR
This paper uses a new semi-analytic model, A-SLOTH, to study the stellar mass-to-halo mass relation in Milky Way-like systems, revealing a plateau in ultra-faint regimes and the impact of early conditions on satellite galaxy formation.
Contribution
The paper introduces a novel model that tracks star formation and feedback in ultra-faint dwarf galaxies, improving understanding of their stellar properties and formation history.
Findings
Identification of a plateau in the stellar mass-to-halo mass relation.
The number of ultra-faint satellites increases rapidly below a certain stellar mass.
High-redshift baryon-dark matter streaming velocity influences satellite galaxy abundance.
Abstract
We study the stellar mass-to-halo mass relation at in 30 Milky Way-like systems down to the ultra-faint () regime using the semi-analytic model A-SLOTH. A new model allows us to follow star formation and the stochastic stellar feedback from individually sampled Pop II stars. Our fiducial model produces consistent results with the stellar mass-to-halo mass relation derived from abundance matching and the observed cumulative stellar mass function above the observational completeness. We find a plateau in the stellar mass-to-halo mass relation in the ultra-faint regime. The stellar mass of this plateau tells us how many stars formed before supernovae occur and regulate further star formation, which is determined by the Pop~II star formation efficiency. We also find that the number of luminous satellites increases rapidly as decreases until $M_* \approx 10^4…
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