  Basaltic asteroids (V-types) are believed to be fragments of large
differentiated bodies. The majority of them are found in the inner part of the
asteroid belt, and are current or past members of the Vesta family. Recently,
some V-type asteroids have been discovered far from the Vesta family supporting
the hypothesis of the presence of multiple basaltic asteroids in the early
solar system. The discovery of basaltic asteroids in the outer belt challenged
the models of the radial extent and the variability of the temperature
distribution in the early solar system. We aim to identify new basaltic V-type
asteroids using near-infrared colors of ~40000 asteroids observed by the
VHS-VISTA survey and compiled in the MOVIS-C catalogue. We also want to study
their near-infrared colors and to study the near-infrared color distribution of
the Vesta dynamical family. We performed a search in the MOVIS-C catalogue of
all the asteroids with (Y-J) and (J-Ks) in the range (Y-J) > 0.5 and (J-Ks) <
0.3, associated with V-type asteroids, and studied their color distribution. We
have also analyzed the near-infrared color distribution of 273 asteroid members
of the Vesta family and compared them with the albedo and visible colors from
WISE and SDSS data. We determined the fraction of V-type asteroids in the
family. We found 477 V-type candidates in MOVIS-C, 244 of them outside the
Vesta dynamical family. We identified 19 V-type asteroids beyond the 3:1 mean
motion resonance, 6 of them in the outer main belt, and 16 V-types in the inner
main belt with proper inclination i_p < 3.0deg, well below the inclination of
the Vesta family. We computed that ~85% of the members of the Vesta dynamical
family are V-type asteroids, and only 1-2% are primitive class asteroids and
unlikely members of the family. This work almost doubles the sample of basaltic
asteroid candidates in regions outside the Vesta family.
