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We compare and contrast the stellar structures of isolated Local Group dwarfgalaxies, as traced by their oldest stellar populations, with the satellitedwarf galaxies of the Milky Way and M31. All Local Group dwarfs with Mv < -6and surface brightness < 26.5 mags. per square arcsec. are considered, takingadvantage of measurements from surveys that use similar observations andanalysis techniques. For the isolated dwarfs, we use the results from SolitaryLocal (Solo) Dwarf Galaxy Survey. We begin by confirming that the structuraland dynamical properties of the two satellite populations are not obviouslystatistically different from each other, but we note that there many moresatellites around M31 than around the Milky Way down to equivalent magnitudeand surface brightness limits. We find that dwarfs in close proximity to amassive galaxy generally show more scatter in their Kormendy relations thanthose in isolation. Specifically, isolated Local Group dwarf galaxies show atighter trend of half-light radius versus magnitude than the satellitepopulations, and similar effects are also seen for related parameters. Thereappears to be a transition in the structural and dynamical properties of thedwarf galaxy population around ~400 kpc from the Milky Way and M31, such thatthe smallest, faintest, most circular dwarf galaxies are found closer than thisseparation. We discuss the impact of selection effects on our analysis, and weargue that our results point to the significance of tidal interactions on thepopulation of systems within approximately 400 kpc from the MW and M31.

Solo dwarfs IV: Comparing and contrasting satellite and isolated dwarf galaxies in the Local Group