The stellar populations of high-redshift dwarf galaxies
  We use high-resolution ($\approx 10$ pc), zoom-in simulations of a typical
(stellar mass $M_\star\simeq10^{10}M_\odot$) Lyman Break Galaxy (LBG) at
$z\simeq 6$ to investigate the stellar populations of its six dwarf galaxy
satellites, whose stellar [gas] masses are in the range $\log (M_\star/M_\odot)
\simeq 6-9$ [$\log (M_{gas}/M_\odot) \simeq4.3-7.75$]. The properties and
evolution of satellites show no dependence on the distance from the central
massive LBG ($< 11.5$ kpc). Instead, their star formation and chemical
enrichment histories are tightly connected their stellar (and sub-halo) mass.
High-mass dwarf galaxies ($\rm M_\star \gtrsim 5\times 10^8 M_\odot$)
experience a long history of star formation, characterised by many merger
events. Lower-mass systems go through a series of short star formation
episodes, with no signs of mergers; their star formation activity starts
relatively late ($z\approx 7$), and it is rapidly quenched by internal stellar
feedback. In spite of the different evolutionary patterns, all satellites show
a spherical morphology, with ancient and more metal-poor stars located towards
the inner regions. All six dwarf satellites experienced high star formation
rate ($\rm >5\,M_\odot yr ^{-1}$) bursts, which can be detected by JWST while
targeting high-$z$ LBGs.
