  Observations suggest that the dark matter and stars in early-type galaxies
`conspire' to produce a surprisingly simple distribution of total mass,
$\rho(r)\propto\rho^{-\gamma}$, with $\gamma\approx2$. We measure the
distribution of mass in 48 early-type galaxies that gravitationally lens a
resolved background source. By fitting the source light in every pixel of
images from the Hubble Space Telescope, we find a mean
$\langle\gamma\rangle=2.075_{-0.024}^{+0.023}$ with intrinsic scatter between
galaxies of $\sigma_\gamma=0.172^{+0.022}_{-0.032}$ for the overall sample.
This is consistent with, and has similar precision to traditional techniques
that employ spectroscopic observations to supplement lensing with mass
estimates from stellar dynamics. Comparing measurements of $\gamma$ for
individual lenses using both techniques, we find a statistically insignificant
correlation of $-0.150^{+0.223}_{-0.217}$ between the two, indicating a lack of
statistical power or deviations from a power-law density in certain lenses. At
fixed surface mass density, we measure a redshift dependence,
$\partial\langle\gamma\rangle/\partial z=0.345^{+0.322}_{-0.296}$, that is
consistent with traditional techniques for the same sample of SLACS and GALLERY
lenses. Interestingly, the consistency breaks down when we measure the
dependence of $\gamma$ on the surface mass density of a lens galaxy. We argue
that this is tentative evidence for an inflection point in the total-mass
density profile at a few times the galaxy effective radius -- breaking the
conspiracy.
