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 \pm 2.3 ( stat ) \pm 1.5 ( sys ) km s ^ { -1 } Mpc ^ { -1 } .