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In this work we extend the study on the mass distribution of the spiralgalaxy NGC 5278, performing 1D and 2D bulge-disk decomposition to determinewhich components constitute the baryonic mass in this galaxy. Our analysis doesnot detect any bulge, instead we find a bright source, probably related withthe central AGN, and an exponential disk. We fix the stellar disk contributionto the rotation curve (RC) with broad band photometric observations andpopulation synthesis models, to obtain 2D mass distribution of the stellardisk. In the particular case of NGC 5278, we find that the typical assumptionof considering the mass-to-luminosity ratio (M/L) of the disk as constant alongthe galactocentric radius is not valid. We also extract a baryonic RC from themass profile, to determine the inability of this baryonic RC and also of thebaryonic RC with more and less 30% disk mass (in order to consider the diskmass errors) to fit the entire RC. We perform the RC decomposition of NGC 5278considering the baryonic RC and four types of dark matter halos: Hernquist;Burkert; Einasto and Navarro, Frenk & White. Our results show that Hernquisthalo 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 thecase of 30% more disk mass the cored Einasto (n < 4) halo is the best fittingmodel.

Disk Mass-to-Light ratio distribution from stellar population synthesis: Application to rotation curve decomposition of NGC 5278 (KPG 390A)