  In $2016-17$, the Galactic transient black hole candidate GRS 1716-249
exhibited an outburst event after a long period of quiescence of almost 23
years. The source remained in the outbursting phase for $\sim 9$ months. We
study the spectral and temporal properties of the source during this outburst
using archival data from four astronomy satellites, namely MAXI, Swift, NuSTAR
and AstroSat. Initial spectral analysis is done using combined disk black body
and power-law models. For a better understanding of the accretion flow
properties, we studied spectra with the physical two component advective flow
(TCAF) model. Accretion flow parameters are extracted directly from the
spectral fits with the TCAF model. Low frequency quasi-periodic oscillations
are also observed in the Swift/XRT and AstroSat/LAXPC data. From the nature of
the variation of the spectral and temporal properties, we find the source
remains in hard state during the entire outburst. It never had a transition to
other states which makes this event a `failed' outburst. An absence of the
softer spectral states is consistent with the class of short orbital period
objects, where the source belongs to. From the spectral fit, we also estimate
the probable mass of GRS~1716-249 to be in the range of $4.50-5.93 M_\odot$ or
$5.02^{+0.91}_{-0.52} M_\odot$.
