We present the results obtained from imaging observations , and search for radio pulsations towards the magnetar SGR J1935+2154 made using the Giant Metrewave Radio Telescope , and the Ooty Radio Telescope .
We present the high resolution radio image of the supernova remnant ( SNR ) G57.2+0.8 , which is positionally associated with SGR J1935+2154 .
We did not detect significant periodic radio pulsations from the magnetar , with 8 \sigma upper limits on its flux density of 0.4 , and 0.2 mJy at 326.5 , and 610 MHz , respectively , for an assumed duty cycle of 10 % .
The corresponding 6 \sigma upper limits at the two frequencies for any burst emission with an assumed width of 10 ms are 0.5 Jy , and 63 mJy , respectively .
No continuum radio point source was detected at the position of SGR J1935+2154 with a 3 \sigma upper limit of 1.2 mJy .
We also did not detect significant diffuse radio emission in a radius of 70 arc seconds in coincidence with the diffuse X-ray emission reported recently , with a 3 \sigma upper limit of 4.5 mJy .
Using the archival HI spectra , we estimate the distance of SNR G57.2+0.8 to be 11.7 \pm 2.8 kpc .
Based on measured HI column density ( N _ { H } ) along this line of sight , we argue that the magnetar could be physically associated with SNR G57.2+0.8 .
Based on present data , we can not rule out either a pulsar wind nebula or a dust scattering halo origin for the diffuse X-ray emission seen around the magnetar .