Using The Baryonic Tully-Fisher Relation to Measure $H_o$
  We explore the use of the baryonic Tully-Fisher relation (bTFR) as a new
distance indicator. Advances in near-IR imaging and stellar population models,
plus precise rotation curves, have reduced the scatter in the bTFR such that
distance is the dominant source of uncertainty. Using 50 galaxies with accurate
distances from Cepheids or tip magnitude of the red giant branch, we calibrate
the bTFR on a scale independent of $H_o$. We then apply this calibrated bTFR to
95 independent galaxies from the SPARC sample, using CosmicFlows-3 velocities,
to deduce the local value of $H_o$. We find $H_o$ = 75.1 +/- 2.3 (stat) +/- 1.5
(sys) km s$^{-1}$ Mpc$^{-1}$.
