  NGC 5291, an early-type galaxy surrounded by a giant HI ring, is believed to
be formed from collision with another galaxy. Several star forming complexes
and tidal dwarf galaxies are distributed along the collisional ring which are
sites of star formation in environments where extreme dynamical effects are
involved. Dynamical effects can affect the star formation properties and the
spatial distribution of star forming complexes along the tidal features. To
study and quantify the star formation activity in the main body and in the ring
structure of the NGC 5291 system, we use high spatial resolution FUV and NUV
imaging observations from the Ultraviolet Imaging Telescope onboard AstroSat. A
total of 57 star-forming knots are identified to be part of this interacting
system out of which 12 are new detections (star forming complexes that lie
inside the HI contour) compared to the previous measurements from lower
resolution UV imaging. We estimate the attenuation in UV for each of the
resolved star-forming knots using the UV spectral slope $\beta$, derived from
the FUV-NUV colour. Using the extinction corrected UV fluxes, we derive the
star formation rate of the resolved star forming complexes. The extinction
corrected total star formation rate of this system is estimated as 1.75 $\pm$
0.04 $M_{\odot}/yr$. The comparison with dwarf galaxy populations (BCD, Sm and
dIm galaxies) in the nearby Universe shows that many of the knots in the NGC
5291 system have SFR values comparable to the SFR of BCD galaxies.
