They estimated that the bursts had an energy similar to the brightest giant pulses from the Crab pulsar,[8][15] which had never been seen from a magnetar.

[22] To further secure the association of FRB 200428 with the remnant, the Five-hundred-meter Aperture Spherical Telescope (FAST) reported the detection of a much weaker radio burst,[23] which was localized to within a maximal margin of error of a few arcminutes of the position of the remnant with a dispersion measure consistent with those reported by STARE2 and CHIME.

[24] The Very Large Array (VLA) followed the remnant 1–2 days after FRB 200428 and did not find any pulsed radio emission or an afterglow.

[25][26] The Deep Space Network (DSN) observed the remnant 1.5 to 3.5 days after the FRB and did not find evidence of periodic emission.

[40][41][42][43][44][45][46] The repeated X-ray bursts are easily explained by collisions of fragments caused by the partial tidal disruption of a planet orbiting the star.