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Extended, old, and round stellar halos appear to be ubiquitous aroundhigh-mass dwarf galaxies ($10^{8.5}<M_\star/M_\odot<10^{9.6}$) in the observeduniverse. However, it is unlikely that these dwarfs have undergone a sufficientnumber of minor mergers to form stellar halos that are composed ofpredominantly accreted stars. Here, we demonstrate that FIRE-2 (Feedback inRealistic Environments) cosmological zoom-in simulations are capable ofproducing dwarf galaxies with realistic structure, including both a thick diskand round stellar halo. Crucially, these stellar halos are formed in-situ,largely via the outward migration of disk stars. However, there also exists alarge population of "non-disky" dwarfs in FIRE-2 that lack a well-defineddisk/halo and do not resemble the observed dwarf population. These non-diskydwarfs tend to be either more gas poor or to have burstier recent starformation histories than the disky dwarfs, suggesting that star formationfeedback may be preventing disk formation. Both classes of dwarfs underscorethe power of a galaxy's intrinsic shape -- which is a direct quantification ofthe distribution of the galaxy's stellar content -- to interrogate the feedbackimplementation in simulated galaxies.

The In-situ Origins of Dwarf Stellar Outskirts in FIRE-2