We have measured the bias of QSOs as a function of QSO luminosity at xed redshift (z < 1) by cross-correlating them with luminous red galaxies (LRGs) in the same spatial volume, hence breaking the degeneracy between QSO luminosity and redshift. We use three QSO samples from 2SLAQ, 2QZ and Sloan Digital Sky Survey (SDSS) covering a QSO absolute magnitude range, -24.5 <MbJ < -21.5, and cross-correlate them with 2SLAQ (z ≈ 0.5) and AAOmega (z ≈ 0.7) photometric and spectroscopic LRGs in the same redshift ranges. The spectroscopic QSO samples, in the spectroscopic LRG areas, contain up to 700 QSOs and in photometric LRG areas up to 7000 QSOs. The 2D and 3D cross-clustering measurements are generally in good agreement. Our (2SLAQ) QSO-LRG clustering amplitude (r0 = 6.98 ± 0.6 h-1 Mpc) as measured from the semiprojected cross-correlation function appears similar to the (2SLAQ) LRG-LRG autocorrelation amplitude (r0 = 7.45 ± 0.35 h-1 Mpc) and both are higher than the (2QZ + 2SLAQ) QSO-QSO amplitude (r0 ≈ 5.0 h-1 Mpc). Our measurements show remarkably little QSO-LRG cross-clustering dependence on QSO luminosity. This result is unexpected on the basis of simple high-peak biasing models, where more luminous QSOs are assumed to occupy rarer and so more clustered high-mass peaks. Assuming a standard ΛCDM model and values for bLRG measured from LRG autocorrelation analyses, from the spectroscopic samples at z ≈ 0.55 we nd bQ = 2.3 ± 0.5 at MbJ ≈-24 and bQ = 1.6 ± 0.3 at MbJ ≈-22. Averaging over all the spectroscopic and photometric samples, we nd an average value of bQ = 1.8 ± 0.1 at z ≈ 0.6 and MbJ ≈-23. The implied dark matter halo mass inhabited by QSOs is ≈ 1013 h-1 M⊙, again approximately independent of QSO luminosity. We have also made a z-space distortion analysis of the QSO-LRG cross-clustering at z ≈ 0.55. The velocity dispersion tted to QSO-LRG cross-correlation, ξ (σ, π), at ±600 km s-1 is close to that expected given the larger QSO redshift errors. The dynamical infall result for the combined 2SLAQ, 2QZ and SDSS QSO sample gives βQ = 0.23 ± 0.15 which implies bQ = 3.2 ± 2.1, assuming the standard cosmological model. Although noisier, this latter value is consistent with the value of bQ = 1.9 ± 0.2 obtained from the amplitude of the cross-correlation function in the same redshift range.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science