Large-scale structure and galaxy motions in the Leo/Cancer
  constellations
  In the region of the sky limited by the coordinates RA$=7.0^h...12.0^h$,
Dec$=0^\circ...+20^\circ$ and extending from the Virgo Cluster to the South
Pole of the Local Supercluster, we consider the data on the galaxies with
radial velocities $V_{LG}\lesssim 2000$ km/s. For 290 among them, we determine
individual distances and peculiar velocities. In this region, known as the
local velocity anomaly zone, there are 23 groups and 20 pairs of galaxies for
which the estimates of virial/orbital masses are obtained. A nearby group
around NGC3379 = Leo I and NGC3627 as well as the Local Group show the motion
from the Local Void in the direction of Leo cloud with a characteristic
velocity of about 400 km/s. Another rich group of galaxies around NGC3607
reveals peculiar velocity of about -420 km/s in the frame of reference related
with the cosmic background radiation. A peculiar scattered association of dwarf
galaxies Gemini Flock at a distance of 8 Mpc has the radial velocity dispersion
of only 20 km/s and the size of approximately 0.7 Mpc. The virial mass estimate
for it is 300 times greater than the total stellar mass. The ratio of the sum
of virial masses of groups and pairs in the Leo/Can region to the sum of
stellar masses of the galaxies contained in them equals 26, which is equivalent
to the local average density $\Omega_{m(local)} = 0.074$, which is 3-4 times
smaller than the global average density of matter.
