spectral index are detailed in Section \[sec:disc\] followed by our conclusions in Section \[sec:conc\].

UTMOST specifications and survey properties {#sec:OA}
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The UTMOST consists of an East-West (E-W) aligned cylindrical paraboloid divided into two ‘arms’ (separated by a 15-m gap), each 11.6-m wide and 778-m long, with 7744 right circularly polarised ring antennas operating at 843 MHz on a line feed system at its focus. Groups of 22 consecutive ring antennas (these groups are termed ‘modules’) are phased to the physical centre of the module, forming 352 unique inputs (each with a beam $4.0^{\circ} \times 2.8^{\circ}$ FWHP) which are then beamformed (Bailes at al., submitted). We operate the telescope by tilting the arms North-South and steering the ring antennae East-West by differential rotation. UTMOST can access the sky South of $\delta=+18^{\circ}$ with the East-West steering limited to $\pm60^{\circ}$. The telescope’s field of view, sensitivity and high duty cycle make it a near ideal survey instrument for finding FRBs and other radio transients. Since late 2015, we have been using UTMOST to search for fast radio transients for an average of 18 hours a day, while simultaneously timing more than 300 pulsars weekly (Bailes et al., submitted, Jankowski et al., in 