The use of the Tully–Fisher ( TF ) relation for the determination of H _ { \circ } relies on the availability of an adequate template TF relation and of reliable primary distances .
Here we use a TF template relation with the best available kinematical zero–point , obtained from a sample of 24 clusters of galaxies extending to cz \sim 9 , 000 km s ^ { -1 } , and the most recent set of Cepheid distances for galaxies fit for TF use .
The combination of these two ingredients yields H _ { \circ } = 69 \pm 5 km s ^ { -1 } Mpc ^ { -1 } .
The approach is significantly more accurate than the more common application with single cluster ( e.g .
Virgo , Coma ) samples .