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Over the next decade, the astronomical community will be commissioningmultiple wide-field observatories well-suited for studying stellar halos inboth integrated light and resolved stars. In preparation for this, we use fivehigh-resolution cosmological simulations of Milky Way-like galaxies from theFiguring Out Gas & Galaxies in Enzo (FOGGIE) suite to explore the propertiesand components of stellar halos. At $z=0$, we find that the FOGGIE stellarhalos have masses, metallicity gradients, and surface brightness profiles thatare consistent with observations. In agreement with other simulations, theFOGGIE stellar halos receive 30-40% of their mass from stars that formed insitu. However, this population tends to be more centrally concentrated in theFOGGIE simulations and therefore does not contribute excess light or mass tothe outskirts of the halos. The rest of the stars in each stellar halo areaccreted from $\sim$10-50 other galaxies, with the majority of the accretedmass originating in 2-4 of these contributors. While the phase-mixed inner halo($r<$50 kpc) of each FOGGIE galaxy includes stars from a large number ofcontributors, the halo outskirts of three of the five galaxies are primarilymade up of stars from only a few contributors. We predict that upcomingwide-field observatories, like the Nancy Grace Roman Space Telescope, willprobe stellar halos around Milky Way-like galaxies out to $\sim$100 kpc inintegrated light and will be able to distinguish the debris of dwarf galaxieswith extended star formation histories from the underlying halo with resolvedcolor-magnitude diagrams.

Figuring Out Gas & Galaxies In Enzo (FOGGIE) VII: The (Dis)Assembly of Stellar Halos