determined. This locus is then integrated to estimate the total volume over which the line might be observed at this redshift. This procedure is then repeated along the full length of the curves shown in Fig. \[fig:sfgs\]. In this way, the total number of interlopers which might be observed is estimated. The results are shown in Table \[tab:interlopers\].

It is clear that the estaimted number of interlopers is negligible in the case of the two lower-redshift fields. However, it is possible that as many as five of the candidate ELGs in the BR B0019-1522 field are, in fact, low redshift interlopers. This could only be confirmed by further observations.

Properties of candidate ELGs {#sec:properties}
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In this section, we consider the distribution of candidate ELGs around the quasars to determine whether the quasar lies in an identifiable overdensity relative to the field.

The small number of candidates around the lower-$z$ quasars renders a meaningful statistical analysis of the individual fields unreliable. In an attempt to mitigate this, and given the apparent similarity of the fields, they are both considered as one unit in this section.

![image](fig5)

The distribution of ELG candidates around the quasar is shown in both projection on 