given by Equation \[eqn:eventrate\].\
Clearly, $\alpha=1$ is the dividing line between the FOV and sensitivity domains: $\alpha>1$ yields a paucity of bright events and larger, more sensitive telescopes win. Brighter events are relatively plentiful for $\alpha<1$ which favors smaller dishes with larger fields of view. If we conservatively assume that $\alpha=1.0$ and that the maximum cut-off fluence is 500 Jy ms (see Fig. \[fig:eventrate\]), then the optimal dish diameter is $d\sim 6$ m— a value at which the $\alpha=1$ line begins to saturate. Smaller dishes may be insensitive to a large number of events, and significantly larger dishes will have excluded large numbers of events due to their narrow fields of view. For the most likely range of $0.66<\alpha<0.96$, we find that dish diameters of between 1m and 6m are preferred, and that the detection rate could be well over 10 events per month. Hence, we conclude that given the constraints on $\alpha$ presented here, a modest array ($N_{\rm ant}\sim 10$) of small dishes of about $d\sim 6$ m will detect at least $\gtrsim 1$ FRB per month. Future FRB surveys may take advantage of this fact and design for a system that detects events using the incoherent sum of 