Local gravity and large-scale structure

Details Local gravity and large-scale structure Local gravity and large-scale structure

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...349..408j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 349, Feb. 1, 1990, p. 408-414. Research supported by NASA, NSF, and MPI, an

Astronomy and Astrophysics

Astronomy

58

Galactic Structure, Gravitation Theory, Relic Radiation, Space Density, Astronomical Models, Dark Matter, Infrared Sources (Astronomy)

Scientific paper

The magnitude and direction of the observed dipole anisotropy of the galaxy distribution can in principle constrain the amount of large-scale power present in the spectrum of primordial density fluctuations. This paper confronts the data, provided by a recent redshift survey of galaxies detected by the IRAS satellite, with the predictions of two cosmological models with very different levels of large-scale power: the biased Cold Dark Matter dominated model (CDM) and a baryon-dominated model (BDM) with isocurvature initial conditions. Model predictions are investigated for the Local Group peculiar velocity, v(R), induced by mass inhomogeneities distributed out to a given radius, R, for R less than about 10,000 km/s. Several convergence measures for v(R) are developed, which can become powerful cosmological tests when deep enough samples become available. For the present data sets, the CDM and BDM predictions are indistinguishable at the 2 sigma level and both are consistent with observations. A promising discriminant between cosmological models is the misalignment angle between v(R) and the apex of the dipole anisotropy of the microwave background.

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