  We measure the mass density profile of the lens galaxy in the Einstein ring
system 0047-2808 using our semi-linear inversion method developed in an earlier
paper. By introducing an adaptively gridded source plane, we are able to
eliminate the need for regularisation of the inversion. This removes the
problem of a poorly defined number of degrees of freedom, encountered by
inversion methods that employ regularisation, and so allows a proper
statistical comparison between models. We confirm the results of Wayth et al.
(2004), that the source is double, and that a power-law model gives a
significantly better fit that the singular isothermal ellipsoid model. We
measure a slope alpha=2.11+/-0.04. We find, further, that a dual-component
constant M/L baryonic + dark halo model gives a significantly better fit than
the power-law model, at the 99.7% confidence level. The inner logarithmic slope
of the dark halo profile is found to be 0.87^{+0.69}_{-0.61} (95% CL),
consistent with the predictions of CDM simulations of structure formation. We
determine an unevolved B-band mass to light ratio for the baryons (only) of
3.05^{+0.53}_{-0.90} h_65 M_sol/L_Bsol (95% CL). This is the first measurement
of the baryonic M/L of a single galaxy by purely gravitational lens methods.
The baryons account for 65^{+10}_{-18}% (95% CL) of the total projected mass,
or, assuming spherical symmetry, 84^{+12}_{-24}% (95% CL) of the total
three-dimensional mass within the mean radius of 1.16'' (7.5 h_65^{-1} kpc)
traced by the ring. Finally, at the level of >3sigma, we find that the halo
mass is rounder than the baryonic distribution and that the two components are
offset in orientation from one another.
