We present a multi-epoch time-resolved high-resolution optical spectroscopy study of the short-period (P(orb) = 11.2 hr) eclipsing M0V+M5V RS CVn binary V405 Andromeda. By means of indirect imaging techniques, namely Doppler imaging, we study the surface activity features of the M0V component of the system. A modified version of a Doppler imaging code, which takes into account the tidal distortion of the surface of the star, is applied to the multi-epoch data set in order to provide indirect images of the stellar surface. The multi-epoch surface brightness distributions show a low intensity "belt" of spots at latitudes +/- 40 degrees and a noticeable absence of high latitude features or polar spots on the primary star of V405 Andromeda. They also reveal slow evolution of the spot distribution over similar to 4 yr. An entropy landscape procedure is used in order to find the set of binary parameters that lead to the smoothest surface brightness distributions. As a result, we find M(1) = 0.51 +/- 0.03M(circle dot), M(2) = 0.21 +/- 0.01M(circle dot), R(1) = 0.71 +/- 0.01 R(circle dot), and an inclination i = 65 degrees +/- 1 degrees. The resulting systemic velocity is distinct for different epochs, raising the possibility of the existence of a third body in the system.