  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.
