density around 100 times higher than that found locally.

Further work with TTF was performed by @Francis04, who targeted Ly $\alpha$ emitters within 1 Mpc of the $z=2.159$ radio loud quasar PKS B0424-131 without making [*any*]{} detections. These authors selected this extremely luminous UV source with the expectation of finding Ly $\alpha$ fluorescent clouds in the vicinity of the quasar but these were not detected. With specific application to PKS B0424-131, @Bruns11 demonstrated that the most intrinsically UV-luminous quasars observed beyond $z=1$ suppress star formation in low-mass haloes ($M_{\rm vir} \lesssim 10^{12}$ M$_\odot$) within a megaparsec of the quasar. The intense UV radiation field is expected to photo-evaporate HI clouds which presumably accounts for the lack of detections. We return to this point in our conclusion (§ \[sec:conclusion\]).

The present work continues to push TTF to higher redshifts, searching three quasar fields at redshifts up to $z \sim 4.5$. The objects selected include examples of both radio-loud and radio-quiet quasars, and their environments are compared. Section \[sec:obs\] of this paper describes the observations, including target selection, instrumental characteristics and a note on data reduction. Section \[sec:sim\] describes simulations performed to examine statistical properties and completeness of our sample. Section \[sec:id\] 