Same as Fig. 5, but with halo circular velocity profiles color-coded by concentration (top) and virial mass (bottom). Cetus and Tucana are shown as a triangle and a square, respectively. Top panel: the Local Group dwarf galaxies are color-coded according to their stellar mass; a probable correlation is visible between the circular velocity and the stellar mass. Bottom panel: the color-coded dots that follow the same color schema as the halo virial mass profiles are Local Group dwarf galaxies, for which virial masses were obtained from dynamical modeling (Read & Erkal 2019; Leaman et al. 2012).