an astrophysical origin.\
An important attribute of any astrophysical population is the integral source counts, or the log$N$-log$F$ curve, which is the number of sources expected to have an observed fluence, ${\mathcal{F}_{\rm obs}}$, above a certain threshold. We model the log$N$-log$F$ curve as a power law with index $\alpha$: $$\label{eqn:lnls}
\mathcal{N}(>{\mathcal{F}_{\rm obs}}) \propto {\mathcal{F}_{\rm obs}}^{-\alpha}.$$ where $\alpha=1.5$ for a non-evolving population in Euclidean space. We show that for far-field events, the fraction of events detected in multiple focal-plane feeds on a given telescope is mostly determined by the index, $\alpha$. In particular, source counts with flatter slopes (values of $\alpha$ closer to zero) yield a relative abundance of brighter events which results in an increased propensity for multiple-beam detections. The principal motivation for this paper is a surprising large fraction (2 out of 16) of multiple-beam FRB detections with the Parkes multi-beam receiver. We use simulated far-field beam models of the Parkes multibeam receiver and the observed multiple-beam detection rates to constrain the value of $\alpha$ (Section \[sec:alpha\_mbs\]). While doing so, we fully account for possible detections of bright events beyond the nominal beam Full Width at Half Maximum (FWHM), and also ensure that our results are robust to survey 