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Just as the PSF magnitudes are optimal measures of the fluxes of
stars, the optimal measure of the flux of a galaxy would use a matched galaxy
model. With this in mind, the code fits two models to the
two-dimensional image of each object in each band:|
1. a pure deVaucouleurs profile, and
2. a pure exponential profile.
The best-fit model in the r-band is fit to the other four bands; the results are stored as the model magnitudes. Details, including a very important warning, can be found here.