A Survey for Large Separation Lensed FIRST Quasars, II. Magnification Bias and Redshift Distribution

Details A Survey for Large Separation Lensed FIRST Quasars, II. Magnification Bias and Redshift Distribution A Survey for Large Separation Lensed FIRST Quasars, II. Magnification Bias and Redshift Distribution

2002-10-22

arxiv.org/abs/astro-ph/0210487v1

Mon.Not.Roy.Astron.Soc. 337 (2002) 1163

Astronomy and Astrophysics

Astrophysics

6 pages, 3 figures, accepted to MNRAS

Scientific paper

10.1046/j.1365-8711.2002.05974.x

The statistics of large-separation gravitational lensing are a powerful tool to probe mass distributions on the scale of galaxy clusters. In this paper we refine the analysis of our survey for large-separation (>5'') lensed FIRST quasars (Ofek et al. 2001) by estimating the magnification bias and the source redshift distribution. Finding no large separation lens among 8000 likely quasars in that sample, implies an upper bound on the lensed fraction of 3.7 x 10^-4 at 95% CL. From a published deep 1.4 GHz radio survey of the Hubble Deep Field, and corresponding optical searches for faint quasars, we calculate a lower limit to the `double flux magnification bias' affecting our radio-optically selected sample, of B>1.1. From the four-colour information in the SDSS Early Data Release, we calculate the photometric redshift distribution of a sample of FIRST quasar candidates and compare it with the redshift distribution from the FIRST Bright Quasar Survey. We find that the median redshift of the quasars in our sample is about 1.4. With these new results, we find that for all plausible cosmologies, the absence of lensed quasars in our survey is consistent with a model based on an empirical, non-evolving, cluster mass function, where clusters are represented by singular isothermal spheres. On the other hand, comparison of our results to the lensing predictions of published N-body-ray-tracing simulations (Wambsganss et al. 1995, 1998) rejects the COBE normalised \Omega_{0}=1 CDM model at 99.9% confidence.

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