IRAS versus POTENT density fields on large scales:: Biasing parameter and Ω

The galaxy density field as extracted from the IRAS 1.2 Jy redshift survey is compared to the mass-density field as reconstructed by the POTENT method from the Mark III catalog of peculiar velocities. The reconstruction is done with Gaussian smoothing of radius 12 h(-1) Mpc, and the comparison is carried out within volumes of effective radii 31-46 h(-1) Mpc, containing approximate to 10-26 independent samples. Random and systematic errors are estimated from multiple realizations of mock catalogs drawn from a simulation that mimics the observed density held in the local universe. The relationship between the two density fields is found to be consistent with gravitational instability theory in the mildly nonlinear regime and a linear biasing relation between galaxies and mass. We measure beta(1) = Omega(0.6)/b(I) = 0.89 +/- 0.12 within a volume of effective radius 40 h(-1) Mpc, where b(I) is the IRAS galaxy biasing parameter at 12 h(-1) Mpc. This result is only weakly dependent on the comparison volume, suggesting that cosmic scatter is no greater than +/-0.1. These data are thus consistent with Omega = 1 and b(I) similar or equal to 1. If b(I) > 0.75, as theoretical models of biasing indicate, then Omega > 0.33 at 95% confidence. A comparison with other estimates of beta(I), if not dominated by unaccounted-for systematic errors, may provide hints for scale dependence in the biasing relation for IRAS galaxies.