Clustering Analyses of 300,000 Photometrically Classified Quasars. II. The Excess on Very Small Scales

Abstract

We study quasar clustering on small scales, modeling clustering amplitudes using halo-driven dark matter descriptions. From 91 pairs on scales <35 h -1 kpc, we detect only a slight excess in quasar clustering over our best-fit large-scale model. Integrated across all redshifts, the implied quasar bias is b Q = 4.21 ± 0.98 ( b Q = 3.93 ± 0.71) at ~18 h -1 kpc (~28 h -1 kpc). Our best-fit (real space) power index is ~-2 [i.e., ξ( r ) ##IMG## [http://ej.iop.org/icons/Entities/vprop.gif] {vprop} r -2 ], implying steeper halo profiles than currently found in simulations. Alternatively, quasar binaries with separation <35 h -1 kpc may trace merging galaxies, with typical dynamical merger times t d ~ (610 ± 260) m -1/2 h -1 Myr, for quasars of host halo mass m × 10 12 h -1 M ☉ . We find that UV-excess quasars at ~28 h -1 kpc cluster >5 times higher at z > 2 than at z < 2, at the 2.0 σ level. However, as the space density of quasars declines as z increases, an excess of quasar binaries (over expectation) at z > 2 could be consistent with reduced merger rates at z > 2 for the galaxies forming UV-excess quasars. Comparing our clustering at ~28 h -1 kpc to a ξ( r ) = ( r /4.8 h -1 Mpc) -1.53 power law, we find an upper limit on any excess of a factor of 4.3 ± 1.3, which, noting some caveats, differs from large excesses recently measured for binary quasars, at 2.2 σ. We speculate that binary quasar surveys that are biased to z > 2 may find inflated clustering excesses when compared to models fit at z < 2. We provide details of 111 photometrically classified quasar pairs with separations <0.1'. Spectroscopy of these pairs could significantly constrain quasar dynamics in merging galaxies.