The stellar populations of high-redshift dwarf galaxies

TL;DR

This study uses high-resolution simulations to explore the stellar populations of dwarf galaxy satellites around a high-redshift Lyman Break Galaxy, revealing diverse star formation histories and potential JWST observability.

Contribution

It provides new insights into the formation and evolution of dwarf satellites at high redshift, highlighting the link between stellar mass and star formation history.

Findings

High-mass dwarfs have prolonged, merger-rich star formation histories.

Lower-mass dwarfs experience short, merger-free star formation episodes.

All satellites show spherical morphology with older, metal-poor stars centrally located.

Abstract

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.