and $682\pm7$ pc cm$^{-3}$ respectively. The data are uncalibrated as the bandpass of the system varies as a function of meridian angle, and the flux densities are in arbitrary units. Note the different time range on the abscissa for FRB 160410.[]{data-label="fig:frbs1"}](Fig1c){width="50.00000%"}

Most published FRBs have been detected with single dish antennas, with relatively poor angular resolution, and we are unable to indisputably rule out a near-field or atmospheric origin for the one-off events until now. The FRB detections made with the multi-beam receiver at the Parkes radio telescope however, are likely to originate at $\gtrsim 20$ km [@Vedantham]. Also FRB 150418 has been proposed to be associated with a galaxy at $z \sim 0.5$. However this association has been called into question by [@Williams] and [@Vedantham], and other models like giant pulses from extragalactic pulsars which could account for the excess DM in the local environment, have been proposed [@Connor]. Better localisation during discovery in the radio requires an interferometric detection.

![The three panels display the total power pulse profiles for one polarisation in three adjacent fan-beams. FRBs 160317 and 160410 were also detected as sub-threshold events in neighbouring fan-beams (in addition to the high S/Ns in the primary detection 