In the present paper we derive the density distribution of dark matter ( DM ) in a well-observed nearby disc galaxy , the Andromeda galaxy .
From photometrical and chemical evolution models constructed in the first part of the study ( 63 , hereafter Paper I ) we can calculate the mass distribution of visible components ( the bulge , the disc , the stellar halo , the outer diffuse stellar halo ) .
In the dynamical model we calculate stellar rotation velocities along the major axis and velocity dispersions along the major , minor and intermediate axes of the galaxy assuming triaxial velocity dispersion ellipsoid .
Comparing the calculated values with the collected observational data , we find the amount of DM , which must be added to reach an agreement with the observed rotation and dispersion data .

We conclude that within the uncertainties , the DM distributions by Moore , Burkert , Navarro , Frenk & White ( NFW ) and the Einasto fit with observations nearly at all distances .
The NFW and Einasto density distributions give the best fit with observations .

The total mass of M 31 with the NFW DM distribution is 1.19 \cdot 10 ^ { 12 } \mathrm { M _ { \sun } } , the ratio of the DM mass to the visible mass is 10.0 .
For the Einasto DM distribution , these values are 1.28 \cdot 10 ^ { 12 } \mathrm { M _ { \sun } } and 10.8 .
The ratio of the DM mass to the visible mass inside the Holmberg radius is 1.75 for the NFW and the Einasto distributions .
For different cuspy DM distributions , the virial mass is in a range ( 6.9–7.9 ) \cdot 10 ^ { 11 } \mathrm { M _ { \sun } } and the virial radius is \sim 150 \mathrm { kpc } .
The DM mean densities inside 10 pc for cusped models are 33 and 16 \mathrm { M _ { \sun } pc ^ { -3 } } for the NFW and the Einasto profiles , respectively .
For the cored Burkert profile , this value is 0.06 \mathrm { M _ { \sun } pc ^ { -3 } } .