We present galaxy-galaxy lensing measurements over scales 0.025 to 10 h ^ { -1 } 
Mpc in the Sloan Digital Sky Survey .
Using a flux-limited sample of 127,001 lens galaxies with spectroscopic redshifts and mean luminosity \langle L \rangle \sim 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 \pm 0.06 and r _ { 0 } = ( 5.4 \pm 0.7 ) ( 0.27 / \Omega _ { m } ) ^ { 1 / \gamma } h ^ { -1 } Mpc .
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 h ^ { -1 } Mpc , with mean \langle b / r \rangle = ( 1.3 \pm 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 \langle b / r \rangle _ { Vlim } = ( 2.0 \pm 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 \sim 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 .