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We present MWFitting, a method to fit the stellar components of the Galaxy bycomparing Hess Diagrams (HDs) from TRILEGAL models to real data. We applyMWFitting to photometric data from the first three years of the Dark EnergySurvey (DES). After removing regions containing known resolved stellar systemssuch as globular clusters, dwarf galaxies, nearby galaxies, the LargeMagellanic Cloud and the Sagittarius Stream, our main sample spans a total areaof $\sim$2,300 deg$^2$ distributed across the DES footprint. We further explorea smaller subset ($\sim$ 1,300 deg$^2$) that excludes all regions with knownstellar streams and stellar overdensities. Validation tests on synthetic datapossessing similar properties to the DES data show that the method is able torecover input parameters with a precision better than 3\%. Based on thebest-fit models, we create simulated stellar catalogues covering the whole DESfootprint down to $g = 24$ magnitude. Comparisons of data and simulationsprovide evidence for a break in the power law index describing the stellardensity of the Milky Way (MW) halo. Several previously discovered stellarover-densities are recovered in the residual stellar density map, showing thereliability of MWFitting in determining the Galactic components. Simulationsmade with the best-fitting parameters are a promising way to predict MW starcounts for surveys such as LSST and Euclid.

Modelling the Milky Way. I -- Method and first results fitting the thick disk and halo with DES-Y3 data