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We present the results of modeling 5, 8 and 15 GHz maps of the gravitationallens MG1131+0456 using the LensClean algorithm. Two models for the massdistribution in the lens were fit: a de Vaucouleurs model and a model with thetwo-dimensional potential phi = b^{2-alpha}(r^2+s^2)^{alpha/2}/2alpha, both inan external shear field. The best fit de Vaucouleurs model has an effectiveradius of R_e = 0.83+-0.13 arcseconds, larger than that measured at opticalwavelengths. The best fit ``alpha model'' has alpha=0.6+-0.2 and a core radiusof s = 0.19 +- 0.07 arcseconds. An isothermal model (alpha=1) is inconsistentwith the data. The best alpha model fits the 8 GHz map significantly betterthan the best de Vaucouleurs model. Although it is difficult to distinguishvisually the original image and the reconstructions, none of the models isstatistically consistent with the data. We believe the primary problem is thatan external shear is an inadequate model for the angular structure of the lensgalaxy. The finite core radius in the models is required by the structure ofthe extended ring, so we confirm that the central component in the 8 GHz map isa central, lensed image of the source rather than the lens galaxy. The modellens positions, the position angle of the shear, and the mass interior to thering are determined very precisely by the lens models. The time delay betweenthe compact components is predicted with an uncertainty we estimate to be atmost +- 9%; the formal uncertainty is +- 4%.Comment: 47 pages. There are 2 Postscript files in the package

The Mass Distribution of the Lens Galaxy in MG 1131+0456