projection effects away from the meridian.

![image](Fig4a.pdf){width="47.00000%"}![image](Fig4b.pdf){width="47.00000%"} ![image](Fig4c.pdf){width="47.00000%"}

\[sec:pipeline\]

In November 2015, we commenced our third FRB survey “V3.0”. It ran for a total of 159.0 days on sky (between 01-11-2015 and 30-11-2016), at $\upepsilon \approx 0.14$ of the final target telescope sensitivity. Our fluence limit of the survey, that is the fluence of the narrowest detectable pulse $\cal{F}_\mathrm{lim}$ can be parametrized as,

$$\label{eq:lim_flue}
{\cal{F}_\mathrm{lim}} \approx 11 \Bigg(\frac{W}{\mathrm{ms}}\Bigg)^{1/2}\,  \mathrm{Jy \, ms}$$

where, 11 Jy is the UTMOST flux limit for $\mathrm{S/N}=10$, $G=3.0$ K Jy$^{-1}$, $\Delta\nu=16$ MHz, $W=1$ ms, $N_\mathrm{p}=1$ and $T_\mathrm{sys}=400$ K. It should be noted that this is not the same as the fluence completeness limit $\cal{F}_\mathrm{complete}$. Between $\cal{F}_\mathrm{lim}$ and $\cal{F}_\mathrm{complete}$ we are incomplete and not all FRBs with fluences in this range are detectable. This incompleteness region corresponds to the pink shaded region in Figure \[fig:fluence\]. The two previous surveys (V1.0 and V2.0) reported in [@Caleb] yielded no FRB events. Relative to V3.0, V1.0 ran for 19.5 days at lower sensitivity ($\upepsilon = 0.07$), while V2.0 operated for 9.4 days at the same sensitivity ($\upepsilon =
0.14$). FRB survey V3.0 consists primarily of pointings taken commensally during pulsar timing observations. In this mode, the time series data from 