  We present new spatial models and distance estimates for globular clusters
(GC) and dwarf spheroidals (dSphs) orbiting our Galaxy based on RR Lyrae (RRab)
stars in the Pan-STARRS1 (PS1) 3$\pi$ survey. Using the PS1 sample of RRab
stars from Sesar et al. (2017) in 16 globular clusters and 5 dwarf galaxies, we
fit structural models in $(l,b,D)$ space; for 13 globular clusters and 6 dwarf
galaxies, we give only their mean heliocentric distance $D$. We verify the
accuracy of the period-luminosity (PL) relations used in Sesar et al. (2017) to
constrain the distance to those stars, and compare them to
period-luminosity-metallicity (PLZ) relations using metallicities from Carretta
et al. (2009). We compare our Sesar et al. (2017) distances to the
parallax-based \textit{Gaia} DR2 distance estimates from Bailer-Jones et al.
(2018), and find our distances to be consistent and considerably more precise.
