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 \pm 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 M _ { d } = 5.6 \times 10 ^ { 10 } M _ { \odot } 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 .