the sky (left) and velocity distribution (right) in Fig. \[fig:distribution\]. When calculating the projection on the sky, we have normalised the total visible area on the sky in each distance bin. We also plot the distribution of all objects detected by [SExtractor]{} in the field for comparison.

Based on these figures, there is little evidence of projected clustering in the low-$z$ fields. However, there is a notably higher density of objects within 1 Mpc (projected) of BR B0019-1522. This is consistent with what one might expect from an examination of Fig. \[fig:elgcandidates\]: note the large number of objects to the east of the quasar in Fig. 3(c). It is also in-line with the scale lengths observed in clusters around other AGN [@Venemans02; @Bremer02; @Barr04].

There is no suggestion of clustering in velocity space in Fig. \[fig:distribution\]. In part, this may be due to the low number of detections in the low-$z$ fields. In the field of BR B0019-1522, we note that all candidates were observed as bluer than the quasar itself; this is noteworthy, but not implausible given the wavelength range probed (6650–6740 Å, with the quasar at 6722 Å). Although the bluest velocity bins show a lower number of 