  In this work we extend the study on the mass distribution of the spiral
galaxy NGC 5278, performing 1D and 2D 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 2D mass distribution of the stellar
disk. In the particular case of 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 and also of the
baryonic RC with more and less 30% disk mass (in order to consider the disk
mass errors) to fit the entire RC. We perform the RC decomposition of NGC 5278
considering the baryonic RC and four types of dark matter halos: Hernquist;
Burkert; Einasto and Navarro, Frenk & White. Our results show that Hernquist
halo models better our observed RC in the case of determined disk mass
($M_d=5.6\times 10^{10}$ solar masses) and also with 30% less disk mass. In the
case of 30% more disk mass the cored Einasto (n < 4) halo is the best fitting
model.
