Derivation of the cosmological density parameter Omega0 from large-scale flows.

Abstract

Methods for determining the cosmological density parameter 0 from large-scale flows are reviewed. Very consistent results using infrared astronomical satellite (IRAS) data have been obtained by different groups with completely independent methods. The two main methods involve either using maps of the galaxy distribution to predict the peculiar velocity of the Local Group or directly comparing the density field inferred from the IRAS galaxy distribution with the peculiar velocities inferred from optical distance methods. All methods based on IRAS data are consistent with Omega0 = 0.7 +/- 0.1, or if Omega0 = 1, with a bias parameter b = 1.2 +/- 0.1. Various problems associated with the method are discussed, including the issue of which waveband is optimum for such studies, bias, the universality of the luminosity function, and the convergence of the dipole. The lower values of 0 obtained in optical studies may indicate a higher degree of bias toward regions of high total matter-density for elliptical galaxies. A new study using the whole IRAS point source catalog to 0.6 jansky is described, which gives results consistent with other IRAS studies.