Presentation #116.37 in the session Stellar/Compact Objects.
When pulsar wind expands into the surrounding material left by the early expansion of SNR it is shocked and forms a magnetic bubble called a “pulsar wind nebula (PWN)”. The Dragonfly PWN (G75.2+0.1) is powered by a young pulsar J2021+3651 and is clearly resolved with a double tori structure and a polar jet in X-rays. Our new radio data taken with the Very Large Array (VLA) at 6 GHz reveals a radio PWN two times larger than its X-ray counterpart and a spectrum softer than typical PWNe. Its polarization map shows a highly ordered and complex magnetic field structure suggesting a toroidal field distorted by the pulsar’s motion. Although our VLA L-band (1.5 GHz) image and the archival X-ray data have revealed a bow-shock structure on large scale, which suggests a supersonically moving pulsar, the ram pressure does not destroy the torus and jet. It indicates that this young PWN is likely a rare case moving trans-sonically. Our newly approved Chandra observation will measure the pulsar’s velocity to prove this and to confirm its association with the TeV source located in the tail of the bow shock