  We present new measurements of scaling laws relating the luminosity of
galaxies to the amplitude and shape of their dark matter halos. Early imaging
and spectroscopic data from the Sloan Digital Sky Survey are used to make weak
lensing measurements of the surface mass density contrast Delta Sigma_+ around
classes of lens objects. This surface mass density contrast as a function of
radius is a measure of the galaxy-mass correlation function (GMCF). Because
spectroscopic redshifts are available for all lens objects, the mass and
distance scales are well constrained. The GMCF measured around ~31,000 lenses
is well fit by a power law of the form
  Delta Sigma_+ = (2.5+0.7-0.6) (R/1 Mpc)^{-0.8+-0.2} h M_sun pc^-2.
  We compare this GMCF to galaxy luminosity, type, and environment, and find
that it varies strongly with all three. We quantify these variations by
comparing the normalization of a fit to the inner 260 h^-1 kpc, M_260, to the
galaxy luminosity. While M_260 is not strongly related to luminosity in bluest
band u', there is a simple, linear relation between M_260 and luminosity in
redder bands (g', r', i', and z'). We test the universality of these
mass-to-light scalings by independently measuring them for spiral and
elliptical galaxies,and for galaxies in a variety of environments. We find
remarkable consistency in these determinations in the red bands, especially i'
and z'. This consistency across a wide range of systems suggests that the
measured scaling represents an excellent cosmic average, and that the
integrated star formation history of galaxies is strongly related to the dark
matter environments in which they form.
