2006ApJ...651...61H

With close pairs of quasars at different redshifts, a background quasar sight line can be used to study a foreground quasar's environment in absorption. We search 149 moderate-resolution background quasar spectra from Gemini, Keck, the MMT, and the SDSS to survey Lyman limit systems (LLSs) and damped Lyα systems (DLAs) in the vicinity of 1.8<z<4.0 luminous foreground quasars. A sample of 27 new quasar-absorber pairs is uncovered with column densities 10^17.2/cm2<N_HI_<10^20.9/cm2 and transverse (proper) distances of 22 h^–1 kpc<R<1.7 h^–1 Mpc from the foreground quasars. If they emit isotropically, the implied ionizing photon fluxes are a factor of ∼5-8000 times larger than the ambient extragalactic UV background over this range of distances. The observed probability of intercepting an absorber is very high for small separations: six out of eight projected sight lines with transverse separations R<150 h^–1 kpc have an absorber coincident with the foreground quasar, of which four have N_HI_>10¹⁹/cm2. The covering factor of N_HI_>10¹⁹/cm2 absorbers is thus ∼50% (4/8) on these small scales, whereas ≲2% would have been expected at random. There are many cosmological applications of these new sight lines: they provide laboratories for studying fluorescent Lyα recombination radiation from LLSs; they constrain the environments, emission geometry, and radiative histories of quasars; and they shed light on the physical nature of LLSs and DLAs.