  Aims. This work considers the Virgo cluster of galaxies, focusing on its
structure, kinematics, and morphological landscape. Our principal aim is to
estimate the virial mass of the cluster. For this purpose, we present a sample
of 1537 galaxies with radial velocities $V_{LG} < 2600$~km~s$^{-1}$ situated
within a region of $\Delta{}SGL = 30^\circ$ and $\Delta{}SGB = 20^\circ$ around
M87. About half of the galaxies have distance estimates.
  Methods. We selected 398 galaxies with distances in a $(17\pm5)$~Mpc range.
Based on their 1D and 2D number-density profiles and their radial velocity
dispersions, we made an estimate for the virial mass of the Virgo cluster.
  Results. We identify the infall of galaxies towards the Virgo cluster core
along the Virgo Southern Extension filament. From a 1D profile of the cluster,
we obtain the virial mass estimate of $(6.3\pm0.9) \times 10^{14} M_\odot, $
which is in tight agreement with its mass estimate via the external infall
pattern of galaxies.
  Conclusions. We conclude that the Virgo cluster outskirts between the virial
radius and the zero-velocity radius do not contain significant amounts of dark
matter beyond the virial radius.
