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We use recent very extended HI kinematics (out to 48 kpc) along with previousH$\alpha$ kinematics of the spiral galaxy NGC 3198 in order to derive itsdistribution of dark matter (DM). First, we used a chi-square method to modelthe rotation curve (RC) of this galaxy in terms of different profiles of its DMdistribution: the universal rotation curve (URC) mass model (stellar disk $+$Burkert halo $+$ gaseous disk), the NFW mass model (stellar disk $+$ NFW halo$+$ gaseous disk) and the baryon $\Lambda$CDM mass model (stellar disk $+$ NFWhalo modified by baryonic physics $+$ gaseous disk). Second, to derive the DMhalo density distribution, we applied a new method that does not require aglobal and often uncertain mass modelling. While according to the standardmethod, both URC and NFW mass models can account for the RC, the new methodinstead leads to a density profile that is sharply disagrees with the dark halodensity distribution predicted within the Lambda cold dark matter($\Lambda$CDM) scenario. We find that the effects of baryonic physics modifythe original $\Lambda$CDM halo densities in such a way that the resultingprofile is more compatible with the DM density of NGC 3198 derived using ournew method. However, at large distances, r $\sim$ 25 kpc, also this modifiedbaryon $\Lambda$CDM halo profile appears to create a tension with the derivedDM halo density.

The Dark Matter Distribution in the Spiral $NGC~3198$ out to 0.22 $R_{vir}$