QSO clustering -- III. Clustering in the Large Bright Quasar Survey and evolution of the QSO correlation function

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Abstract
We present results of a clustering analysis for the Large Bright Quasar Survey (LBQS), and combine these with results obtained from other QSO surveys including the Durham/AAT UVX sample (Paper I). We find a weak signal in the LBQS at small scales, At intermediate scales (8–50 h−1 Mpc) we have tested the QSO correlation function (at the average redshift of 1.27) against linear cold dark matter (CDM) predictions normalized to the cosmic microwave background (CMB) results of COBE. For standard CDM (Ω0 = l, Г = 0.5) we find the best-fitting QSO bias to be bqρ(z = 0) = l.40−0.43+0.28 Thus there appears to be a narrow range around bqρ∼2, consistent with both the biased evolution and comparisons to COBE-normalized power spectra, which allows the Ω0 = 1, CDM model to survive. An interesting test of the Ω0 = 1 model should therefore be possible in a larger data set. We also test ACDM, finding a similar bias, bqρ(z = 0) = 1.20 −0.18.+0.13 At large scales we find little evidence in the LBQS for the anticorrelation beween 40 and 100 h−1 Mpc seen in the Durham/AAT survey. In the combined sample we find no significant signal on any scale larger than 50 h−l Mpc. Since from simulations we estimate that above 100 h−1 Mpc our errors are at the ± 0.025 level, these QSO clustering observations represent the most accurate upper limit on the amplitude of large-scale structure from redshift survey data.

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