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[51.05] Galaxy Biasing and Mass-to-light Ratios from Weak Lensing in the SDSS

E.S. Sheldon (Center for Cosmological Physics, U. of Chicago), J. Frieman, D. Johnston (University of Chicago), T. Mckay (University of Michigan), SDSS Collaboration

Galaxy-galaxy lensing is a direct measure of the galaxy-mass cross correlation function w_gm. We use 75,000 lens galaxies with SDSS redshifts and 3 million source galaxies with photometric redshifts to measure w_gm on scales from 20 kpc to 10 Mpc. By comparing w_gm to the galaxy auto-correlation function, also measured from SDSS data, we constrain the bias between the galaxy distribution and the underlying mass distribution. This relationship is of fundamental importance to the understanding of galaxy formation. We also study w_gm as a function of galaxy luminosity and galaxy type, again comparing to similar studies carried out using the auto-correlation function. Finally, by comparing w_gm to the galaxy-luminosity correlation function, we constrain the bias between luminosity and mass, and the radial dependence of the mass-to-light ratio around galaxies.

Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/.

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Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.