In this work , we present a spectral and temporal analysis of Swift /XRT and NuSTAR observations of GRS 1716–249 during its recent 2016–2017 outburst . This low mass X-ray binary underwent an extraordinary outburst after a long quiescence of 23 years , since its last major outburst in 1993 . The source was observed over two different epochs during 2017 April , 07 and 10 . The best fit joint spectral fitting in the energy range 0.5 - 79.0 keV indicates that the spectrum is best described by relatively cold , weak disk blackbody emission , dominant thermal Comptonization emission , and a relativistically broadened fluorescent iron K \alpha emission line . We observed a clear indication of a Compton hump around 30 keV . We also detected an excess feature of \sim 1.3 keV . Assuming a lamp-post geometry of the corona , we constrained the inner disk radius for both observations to 11.92 ^ { +8.62 } _ { -11.92 } R _ { ISCO } ( i.e. , an upper limit ) and 10.39 ^ { +9.51 } _ { -3.02 } R _ { ISCO } ( where R _ { ISCO } \equiv radius of the innermost stable circular orbit ) for the first epoch ( E1 ) and second epoch ( E2 ) , respectively . A significant ( \sim 5 \sigma ) type - C quasi-periodic oscillation ( QPO ) at 1.20 \pm 0.04 Hz is detected for the first time for GRS 1716–249 , which drifts to 1.55 \pm 0.04 Hz ( \sim 6 \sigma ) at the end of the second observation . The derived spectral and temporal properties show a positive correlation between the QPO frequency and the photon index .