We undertook a surface photometry survey of 200 galaxies in the Virgo cluster ( complete to B < 14.0 mag ) carried out in the near-Infrared ( NIR ) H band .
Combining velocity dispersion measurements from the literature with new spectroscopic data for 11 galaxies we derive distances of 59 early type galaxies using the Fundamental Plane ( FP ) method .
The distance of another 75 late-type galaxies is determined using the Tully-Fisher ( TF ) method .
For this purpose we use the maximum rotational velocity , as derived from HI spectra from the literature , complemented with new H _ { \alpha } rotation curves of 8 highly HI deficient galaxies .
The zero-point of the FP and TF template relations are calibrated assuming the distance modulus of Virgo \mu _ { o } =31.0 , as determined with the Cepheids method .
Using these 134 distance determinations ( with individual uncertainties of 0.35 ( TF ) , 0.45 ( FP ) mag ) we find that the distance of cluster A , associated with M87 , is \mu _ { o } = 30.84 \pm 0.06 .
Cluster B , off-set to the south , is found at \mu _ { o } = 31.84 \pm 0.10 .
This subcluster is falling onto A at about 750 km~ { } s ^ { -1 } .
Clouds W and M are at twice the distance of A. Galaxies on the North-West and South-East of the main cluster A belong to two clouds composed almost exclusively of spiral galaxies with distances consistent with A , but with significantly different velocity distributions , suggesting that they are falling onto cluster A at approximately 770 km~ { } s ^ { -1 } from the far-side and at 200 km~ { } s ^ { -1 } from the near-side respectively .
The mass of Virgo inferred from the peculiar motions induced on its vicinity is consistent with the virial expectation .