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Various models of modified gravity invoke ``screening'' mechanisms that aresensitive to the value of the local gravitational potential. This could haveobservable consequences for galaxies. These consequences might be seen bycomparing two proxies for galaxy mass -- their luminosity and their internalkinematics -- as a function of local galaxy density. Motivated by thisprospect, we have compared the observed properties of luminous red galaxies(LRGs) inside and outside of voids in the cosmic large scale structure. We usedarchival measurements of line widths, luminosities, redshifts, colors, andpositions of galaxies in conjunction with recent void catalogs to constructcomparison LRG samples inside and outside of voids. We fitted these two samplesto the well-established fundamental plane of elliptical galaxies to constrainany differences between the inferred value of the Newtonian gravitationalconstant G for the two samples. We obtained a null result, with an upper limiton any fractional difference in G within and outside of cosmological voids tobe $\alpha =\delta$$ G/G \sim$ 40\%. This upper bound is dominated by thesmall-number statistics of our N $\sim $ 100 within-void LRG sample. With thecaveat that environmental effects could influence various parameters such asstar formation, we estimate that a 1\% statistical limit on $\alpha$ could beattained with data from 10${^5}$ elliptical galaxies within voids. This iswithin the reach of future photometric and spectroscopic surveys, both of whichare required to pursue this method.

Using Elliptical Galaxy Kinematics to Compare of the Strength of Gravity in Cosmological Regions of Differing Gravitational Potential -- A First Look