Measuring the bias factor with the weak lensing effect

Details Measuring the bias factor with the weak lensing effect Measuring the bias factor with the weak lensing effect

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aipc..336..335b&link_type=abstract

Dark matter. AIP Conference Proceedings, Volume 336, pp. 335-338 (1995).

Computer Science

1

Dark Matter, Quasars, Gravitational Lenses And Luminous Arcs, Superclusters, Large-Scale Structure Of The Universe

Scientific paper

The bias parameter b of galaxy formation relates the relative fluctuations in the galaxy number density to the relative fluctuations in the dark-matter density distribution. It lies at the heart of all interpretations of large-scale structure models, because they are compared to observations in terms of the spatial distribution of luminous matter they predict, and this can be inferred from the distribution of dark matter only by the assumption of some galaxy formation prescription, of which the biasing hypothesis is one example (Kaiser 1984, Dekel & Rees 1987). I propose here a method based on weak lensing which allows a measurement of the bias factor. This method requires galaxy counts down to 21st to 22nd magnitude, preferably in the red or near infrared in fields of 20'...30' radius centered on 50...100 high-redshift, bright QSOs. The result, a cross-correlation function between QSOs and galaxies, will be sensitive to the shape of the dark-matter perturbation spectrum on scales between 1 and 10 Mpc/h, where 100 h km/s/Mpc is the Hubble constant. The dependence of the so-derived b on the density parameter Ω0 is different from the dependence ~Ω0.60, hence the measurement proposed here can break the Ω0-b degeneracy in dynamical measurements of b.

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