  We present galaxy-galaxy lensing measurements over scales 0.025 to 10 Mpc/h
in the Sloan Digital Sky Survey. Using a flux-limited sample of 127,001 lens
galaxies with spectroscopic redshifts and mean luminosity <L> = L_* and
9,020,388 source galaxies with photometric redshifts, we invert the lensing
signal to obtain the galaxy-mass correlation function xi_{gm}. We find xi_{gm}
is consistent with a power-law, xi_{gm} = (r/r_0)^{-gamma}, with best-fit
parameters gamma = 1.79 +/- 0.06 and r_0 = (5.4+/-0.7)(0.27/Omega_m)^{1/gamma}
Mpc/h. At fixed separation, the ratio xi_{gg}/xi_{gm} = b/r where b is the bias
and r is the correlation coefficient. Comparing to the galaxy auto-correlation
function for a similarly selected sample of SDSS galaxies, we find that b/r is
approximately scale independent over scales 0.2-6.7 Mpc/h, with mean <b/r> =
(1.3+/-0.2)(Omega_m/0.27). We also find no scale dependence in b/r for a volume
limited sample of luminous galaxies (-23.0 < M_r < -21.5). The mean b/r for
this sample is <b/r>_{Vlim} = (2.0+/-0.7)(Omega_m/0.27). We split the lens
galaxy sample into subsets based on luminosity, color, spectral type, and
velocity dispersion, and see clear trends of the lensing signal with each of
these parameters. The amplitude and logarithmic slope of xi_{gm} increases with
galaxy luminosity. For high luminosities (L ~5 L_*), xi_{gm} deviates
significantly from a power law. These trends with luminosity also appear in the
subsample of red galaxies, which are more strongly clustered than blue
galaxies.
