by extensive pulsar observations. RFI is typically near-field, and predominantly appears in more than 3 adjacent fan-beams, meaning that it can be reliably excised to reduce false positive rates when searching for transients. Using the adjacent fan-beam detections of FRB 160317, we have modeled the point of separation between the near-field or Fresnel region and the far-field or Fraunhofer region of the telescope. Assuming a point source at $10^{6}$ km, we compute the S/N for a tied-array beam (e.g. fan-beam 212) phased at an offset of 0.3 from the centre of the beam to ensure a two fan-beam detection. We compute the path length to each module, the phase of the signal along the array and perpendicular to the array, and add all these as a vector sum weighted by the module performance, to get the “boresight” S/N. We see that in Figure \[fig:fresnel\] at a distance of $\gtrsim 10^4$ km, we achieve a two fan-beam detection with S/N $\sim 13$ in the primary detection beam and S/N $\sim 5$ in the secondary detection beam, similar to the FRB being modeled. Detections of FRBs in 1 or 2 fan-beams only, thus allows us to identify them as sources more distant 