No assembly required: mergers are mostly irrelevant for the growth of low-mass dwarf galaxies

We investigate the merger histories of isolated dwarf galaxies based on a suite of 15 high-resolution cosmological zoom-in simulations, all with masses of |Mₕₐₗₒ ≈ 10¹⁰\, M| (and M|_ ~ 10⁵-10⁷\, M|⁠) at |z|= 0, from the Feedback in Realistic Environments project. The stellar populations of these dwarf galaxies at |z|= 0 are formed essentially entirely ‘in situ’: over 90|\,per\,cent| of the stellar mass is formed in the main progenitor in all but two cases, and all 15 of the galaxies have |> 70 \,per\,cent| of their stellar mass formed in situ. Virtually all galaxy mergers occur prior to |z|∼ 3, meaning that accreted stellar populations are ancient. On average, our simulated dwarfs undergo five galaxy mergers in their lifetimes, with typical pre-merger galaxy mass ratios that are less than 1:10. This merger frequency is generally comparable to what has been found in dissipationless simulations when coupled with abundance matching. Two of the simulated dwarfs have a luminous satellite companion at |z|= 0. These ultra-faint dwarfs lie at or below current detectability thresholds but are intriguing targets for next-generation facilities. The small contribution of accreted stars makes it extremely difficult to discern the effects of mergers in the vast majority of dwarfs either photometrically or using resolved-star colour–magnitude diagrams (CMDs). The important implication for near-field cosmology is that star formation histories (SFHs) of comparably massive galaxies derived from resolved CMDs should trace the build-up of stellar mass in one main system across cosmic time as opposed to reflecting the contributions of many individual SFHs of merged dwarfs.