We describe the serendipitous discovery of a radio point source in a 618 MHz image of the supernova remnant ( SNR ) G76.9+1.0 .
The SNR has a bipolar structure and the point source is located near a faint bridge of emission joining the two lobes of emission .
The point source was also detected in follow-up higher frequency ( 1170 MHz ) observations .
The spectral index for the point source obtained from the GMRT observations is \alpha = -2.1 ^ { -0.45 } _ { +0.36 } .
The steep spectrum , as well as the location of the point source near the centre of the SNR establish the fact that it is indeed the pulsar J2022+3842 associated with this SNR .
The weighted-mean radio position of this point source is \alpha = 20 ^ { h } 22 ^ { m } 21.69 ^ { s } \pm 0.11 ^ { s } , \delta = 38 \degr 42 \arcmin 14.8 % \arcsec \pm 1.7 \arcsec,J 2000 .
Consistent with this , subsequent analysis of archival Chandra X-ray data shows a point source coincident with the radio point source , as well as diffuse extended X-ray emission surrounding the unresolved source .
However , no pulsed emission was detected despite deep searches at both 610 MHz and 1160 MHz although pulsed emission has been seen at 2 GHz with the GBT .
It appears that the most likely reason for not detecting the pulsed signal at the GMRT is temporal broadening : for the estimated DM towards this SNR , the pulse broadening time could be as large as tens of milliseconds .
The diffuse X-ray emission is elongated along the same direction as the bipolar structure seen in the radio .
We interpret the radio lobes as having been formed from an equatorial wind .
Although direct detection of pulsed signal has not been possible , we show convincingly that sensitive , high-resolution , radio imaging at multiple frequencies is a useful method to search for pulsar candidates .