Cosmological streaming velocities and large-scale density maxima

Details Cosmological streaming velocities and large-scale density maxima Cosmological streaming velocities and large-scale density maxima

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.229..469p&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 229, Dec. 1, 1987, p. 469-483.

Astronomy and Astrophysics

Astronomy

7

Astronomical Models, Density Distribution, Flow Velocity, Galactic Evolution, Hubble Constant, Statistical Tests, Baryons, Cosmology, Galactic Clusters, Relic Radiation

Scientific paper

The statistical testing of models for galaxy formation are considered against the observed peculiar velocities on 10-100 Mpc scales (the Rubin-Ford effect). If observers are likely to be sited near maxima in the primordial field of density perturbations, then the observed filtered velocity field will be biased to low values by comparison with a point selected at random. This helps to explain how the peculiar velocities (relative to the microwave background) of the local supercluster and the Rubin-Ford shell can be so similar in magnitude. Using this assumption to predict peculiar velocities on two scales, models with large-scale damping (i.e., adiabatic perturbations) are tested. Allowed models have a damping length close to the Rubin-Ford scale and are mildly nonlinear. Both purely baryonic universes dominated by massive neutrinos can account for the observed velocities, provided Omega lies between 0.1 and 1. In particular, the canonical Omega = 1 massive neutrino model yields the required velocities quite naturally, while not violating the constraints on the anisotropy of the microwave background.

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