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The magnification effect of gravitational lensing is a powerful probe of thedistribution of matter in the universe, yet it is frequently overlooked due tothe fact that its signal to noise is smaller than that of lensing shear.Because its systematic errors are quite different from those of shear,magnification is nevertheless an important approach with which to study thedistribution of large scale structure. We present lensing mass profiles ofspectroscopic luminous red galaxies (LRGs) and galaxy clusters determinedthrough measurements of the weak lensing magnification of photometric LRGs intheir background. We measure the change in detected galaxy counts as well asthe increased average galaxy flux behind the lenses. In addition, we examinethe average change in source color due to extinction by dust in the lenses. Bysimultaneously fitting these three probes we constrain the mass profiles anddust-to-mass ratios of the lenses in six bins of lens richness. For eachrichness bin we fit an NFW halo mass, brightest cluster galaxy (BCG) mass,second halo term, and dust-to-mass ratio. The resulting mass-richness relationis consistent with previous analyses of the catalogs, and limits on thedust-to-mass ratio in the lenses are in agreement with expectations. We explorethe effects of including the (low signal-to-noise) flux magnification andreddening measurements in the analysis compared to using only the countsmagnification data; the additional probes significantly improve the agreementbetween our measured mass-richness relation and previous results.

Magnification of Photometric LRGs by Foreground LRGs and Clusters in SDSS