We present the results of photometric observations carried out with four small telescopes of the asteroid 4 Vesta in the B, R C , and z ′ bands at a minimum phase angle of 0.1 • . The magnitudes, reduced to unit distance and zero phase angle, were M B (1,1,0) = 3.83 ± 0.01,M R C (1,1,0) = 2.67 ± 0.01, and M z ′ (1,1,0) = 3.03 ± 0.01 mag. The absolute magnitude obtained from the IAU H-G function is ∼0.1 mag darker than the magnitude at a phase angle of 0 • 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 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 ρ = 0.4-0.7, yielding the bluk density of 0.9-2.0 × 10 3 kg 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 1 appears from ca. 1 • . 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 ).