The central component has been observed to have a flat radio spectrum with substantial polarization, which is characteristic of a pulsar or plerion wind nebula.

[2] X-ray observations with the ASCA and Chandra observatories also show the composite nature of Kesteven 75, its morphology being very similar to that of radio frequencies.

Based on the high velocity of the ejecta and the low density implied by the initially estimated distance (much greater than currently accepted), it has been suggested that Kesteven 75 comes from a type Ib/c supernova explosion.

[6] However, subsequent studies have proposed that Kesteven 75 is probably the result of a more common type IIP supernova, where the plerion expands into an asymmetric nickel bubble.

Its inferred magnetic field (Bs = 4.9 × 1013 G) is the largest among this type of objects, and is probably responsible for the activity intervals discovered, suggesting a transition to a magnetar state.