The radial acceleration relation is a natural consequence of the
  baryonic Tully-Fisher relation
  Galaxies covering several orders of magnitude in stellar mass and a variety
of Hubble types have been shown to follow the "Radial Acceleration Relation"
(RAR), a relationship between $g_{\rm obs}$, the observed circular acceleration
of the galaxy, and $g_{\rm bar}$, the acceleration due to the total baryonic
mass of the galaxy. For accelerations above $10^{10}~{\rm m \, s}^{-2}$,
$g_{\rm obs}$ traces $g_{\rm bar}$, asymptoting to the 1:1 line. Below this
scale, there is a break in the relation such that $\rm g_{\rm obs} \sim g_{\rm
bar}^{1/2}$. We show that the RAR slope, scatter and the acceleration scale are
all natural consequences of the well-known baryonic Tully-Fisher relation
(BTFR). We further demonstrate that galaxies with a variety of baryonic and
dark matter (DM) profiles and a wide range of dark halo and galaxy properties
(well beyond those expected in CDM) lie on the RAR if we simply require that
their rotation curves satisfy the BTFR. We explore conditions needed to break
this degeneracy: sub-kpc resolved rotation curves inside of "cored"
DM-dominated profiles and/or outside $\gg 100\,$kpc could lie on BTFR but
deviate in the RAR, providing new constraints on DM.
