In this work we extend the study on the mass distribution of the spiral galaxy NGC 5278, performing 1D and 2D (GALFIT) bulge-disk decomposition to determine which components constitute the baryonic mass in this galaxy. Our analysis does not detect any bulge, instead we find a bright source, probably related with the central AGN, and an exponential disk. We fix the stellar disk contribution to the rotation curve (RC) with broad band photometric observations and population synthesis models, to obtain the 2D mass distribution of the stellar disk. In particular, for NGC 5278, we find that the typical assumption of considering the mass-to-luminosity ratio (M/L) of the disk as constant along the galactocentric radius is not valid. We also extract a baryonic RC from the mass profile, to determine the inability of this baryonic RC (also taking into account ± 30% errors in the disk mass), to fit the entire RC. We perform the RC decomposition of NGC 5278 considering the determined baryonic RC and four types of dark matter (DM) halo: Hernquist, Burkert, Navarro, Frenk, & White and Einasto. Our results determine that Hernquist DM halo better models our observed RC in the case of disk mass Md = 5.6 × 10¹⁰ Mʘ and also with less 30% disk mass. In the case of more 30% disk mass the cored Einasto (n < 4) DM halo is the best fitting model.