  The supernovae of Type Ibc are rare and the detailed characteristics of these
explosions have been studied only for a few events. Unlike Type II SNe, the
progenitors of Type Ibc have never been detected in pre-explosion images. So,
to understand the nature of their progenitors and the characteristics of the
explosions, investigation of proximate events are necessary. Here we present
the results of multi-wavelength observations of Type Ib SN 2007uy in the nearby
($\sim$ 29.5 Mpc) galaxy NGC 2770. Analysis of the photometric observations
revealed this explosion as an energetic event with peak absolute R band
magnitude $-18.5\pm0.16$, which is about one mag brighter than the mean value
($-17.6\pm0.6$) derived for well observed Type Ibc events. The SN is highly
extinguished, E(B-V) = 0.63$\pm$0.15 mag, mainly due to foreground material
present in the host galaxy. From optical light curve modeling we determine that
about 0.3 M$_{\odot}$ radioactive $^{56}$Ni is produced and roughly 4.4
M$_{\odot}$ material is ejected during this explosion with liberated energy
$\sim 15\times10^{51}$ erg, indicating the event to be an energetic one.
Through optical spectroscopy, we have noticed a clear aspheric evolution of
several line forming regions, but no dependency of asymmetry is seen on the
distribution of $^{56}$Ni inside the ejecta. The SN shock interaction with the
circumburst material is clearly noticeable in radio follow-up, presenting a
Synchrotron Self Absorption (SSA) dominated light curve with a contribution of
Free Free Absorption (FFA) during the early phases. Assuming a WR star, with
wind velocity $\ga 10^3 {\rm km s}^{-1}$, as a progenitor, we derive a lower
limit to the mass loss rate inferred from the radio data as $\dot{M} \ga
2.4\times10^{-5}$ M$_{\odot}$, yr$^{-1}$, which is consistent with the results
obtained for other Type Ibc SNe bright at radio frequencies.
