  The Baryonic Tully-Fisher Relation (BTFR) links baryonic mass of rotationally
supported galaxies to their flat disk velocities. A popular form of the BTFR
linked to MOND is based on an empirically determined characteristic
acceleration, a0 that serves as the constant of proportionality. In this work,
we propose an alternative, parametric form of the BTFR employing individual
galactic properties from the SPARC galaxy database. Based on this data we find
that a precise mass-velocity correlation is possible taking into account
galactic disk radius and two dynamical related properties; mass discrepancy and
disk surface density. We find no need to invoke a characteristic acceleration
constant although its ansatz can be extracted and compared to several recent
analyses also arguing against the MOND interpretation of a0. This improved BTFR
finding has ramifications for the Radial Acceleration Relation (RAR) as well.
Rather than a universal relation that describes the dynamics of all
rotationally-supported galaxies, we find the RAR consists of a statistically
distributed family of curves, reflecting the unique properties attributed to
individual galaxies.
