Kinematics of the local Universe - X. H-0 from the inverse B-band Tully-Fisher relation using diameter and magnitude limited samples

We derive the value of H-0 using the inverse diameter and magnitude B-band Tully-Fisher relations and the large all-sky sample KLUN (5171 spiral galax ies). Our kinematical model was that of Peebles centered at Virgo. Our cali brator sample consisted of 15 field galaxies with cepheid distance moduli m easured mostly with HST. A straightforward application of the inverse relat ion yielded H-0 approximate to 80 km s(-1) Mpc(-1) for the diameter relatio n and H-0 approximate to 70 km s(-1) Mpc(-1) for the magnitude relation. H- 0 from diameters is about 50 percent and from magnitudes about 30 percent l arger than the corresponding direct estimates (cf. Theureau et al. 1997b). This discrepancy could not be resolved in terms of a selection effect in lo g V-max nor by the dependence of the zero-point on the Hubble type. We showed that a new, calibrator selection bias (Teerikorpi et al. 1999), i s present. By using samples of signicificant size (n=2142 for diameters and N=1713 for magnitudes) we found for a homogeneous distribution of galaxies (alpha = 0): - H-0 = 52(-4)(+5) km s(-1) Mpc(-1) for the inverse diameter B-band Tully-F isher relation, and - H-0 = 53(-5)(+6) km s(-1) Mpc(-1) for the inverse magnitude]B-band Tully- Fisher relation. Also H-0's from a fractal distribution of galaxies (decreasing radial numbe r density gradient alpha = 0.8) agree with the direct predictions. This is the first time when the inverse Tully-Fisher relation clearly lends credenc e to small values of the Hubble constant H-0 and to long cosmological dista nce scale consistently supported by Sandage et al. (1995).