We present the results of photometric observations carried out with four small telescopes of the asteroid 4 Vesta in the $B$, $R_{rm C}$, and $z$ bands at a minimum phase angle of 0.1 $timeform{D}$. The magnitudes, reduced to unit distance and zero phase angle, were $M_{B}(1, 1, 0) = 3.83 pm 0.01, M_{R_{rm C}}(1, 1, 0) = 2.67 pm 0.01$, and $M_{z}(1, 1, 0) = 3.03 pm 0.01$ mag. The absolute magnitude obtained from the IAU $H$--$G$ function is $sim$0.1 mag darker than the magnitude at a phase angle of 0$timeform{D}$ determined from the Shevchenko function and Hapke models with the coherent backscattering effect term. Our photometric measurements allowed us to derive geometric albedos of 0.35 in the $B$ band, 0.41 in the $R_{rm C}$ band, and 0.31 in the $z$ bands by using the Hapke model with the coherent backscattering effect term. Using the Hapke model, the porosity of the optically active regolith on Vesta was estimated to be $rho$ = 0.4--0.7, yielding the bluk density of 0.9--2.0 $times$ $10^3$ kg $mathrm{m^{-3}}$. It is evident that the opposition effect for Vesta makes a contribution to not only the shadow-hiding effect, but also the coherent backscattering effect that appears from ca. $1timeform{D}$. The amplitude of the coherent backscatter opposition effect for Vesta increases with a brightening of reflectance. By comparison with other solar system bodies, we suggest that multiple-scattering on an optically active scale may contribute to the amplitude of the coherent backscatter opposition effect ($B_{C0}$).
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