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[16.15] Galaxy Mass to Light Ratios and \Omega_M from Weak Lensing in the SDSS

E. Sheldon (Mich.), J. Frieman, D. Johnston (Chicago), T. Mckay, J. Racusin (Mich.), A. Stebbins (Fermilab), SDSS Collaboration

We present measurements of galaxy mass to light ratios and a preliminary measurement of \Omega_M using weak lensing measurements in SDSS data. Using weak shear we measure the Galaxy-Mass Correlation Function (GMCF) to 2 h^-1 Mpc around galaxies with SDSS redshifts. The amplitude of the GMCF within 260 h^-1 kpc is converted to a mass M₂₆₀. We find that the relationship between M₂₆₀ and light in the redder SDSS bandpasses is consistent with linear, meaning galaxies in the probed luminosity range all have the same mass to light ratio when measured in red bandpasses. The Galaxy-Luminosity function (GLCF) within 2 Mpc is also measured using SDSS data. We find that the shape of the GLCF and GMCF are consistent on 2 Mpc scales, implying a convergence of the mass to light ratio on these scales. This mass to light ratio is combined with the luminosity density measured in the same bandpasses to infer \Omega_M.

The Sloan Digital Sky Survey (SDSS) is a joint project of The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Princeton University, the United States Naval Observatory, and the University of Washington. Apache Point Observatory, site of the SDSS telescopes, is operated by the Astrophysical Research Consortium (ARC).

The author(s) of this abstract have provided an email address for comments about the abstract: esheldon@umich.edu

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