Precessing jet model for the supernova remnant G109.1-1.0.

The authors propose that the central X-ray pulsar in G109.1-1.0, designated 1E 2259+586, ejects two oppositely directed precessing jets or beams, which give rise to the observed radio structure. The radio emission is interpreted as synchrotron emission from electrons accelerated at the interface of the jets with the walls of the SNR. Thus the observed intersecting arcs of radio emission represent the trace of the precessing jets on the supernova remnant walls. The precession axis is inclined at 37 degrees to the line of sight and the precession cone half angle is 55 degrees. The observed large scale X-ray jet in G109.1-1.0 is found to coincide in position with the precession axis as was found for the X-ray jets from SS433.