  A correlation between the surface density of foreground galaxies tracing the
Large Scale Structure and the position of distant galaxies and quasars is
expected from the magnification bias effect (Canizares 1981). We show that this
foreground--background correlation function w_{fb} can be used as a
straightforward and almost model-free method to measure the cosmological ratio
Omega/b. For samples with appropriate redshift distributions, w_{fb} is
proportional to Omega<delta g>, where delta and g are respectively the
foreground dark matter and galaxy surface density fluctuations. Therefore,
Omega/b is proportional to the ratio w_{fb}/w, where w is equivalent to <gg>,
the foreground galaxy angular two-point correlation function, b is the biasing
factor, and the proportionality factor is independent of the dark matter power
spectrum. Simple estimations show that the application of this method to the
galaxy and quasar samples generated by the upcoming Sloan Sky Digital Survey
will achieve a highly accurate and well resolved measurement of the ratio
Omega/b.
