  We present the results obtained from detailed timing and spectral studies of
the Be/X-ray binary pulsar KS 1947+300 during its 2013 giant outburst. We used
data from Suzaku observations of the pulsar at two epochs i.e. on 2013 October
22 (close to the peak of the outburst) and 2013 November 22. X-ray pulsations
at $\sim$18.81 s were clearly detected in the light curves obtained from both
observations. Pulse periods estimated during the outburst showed that the
pulsar was spinning up. The pulse profile was found to be single-peaked up to
$\sim$10 keV beyond which a sharp peak followed by a dip-like feature appeared
at hard X-rays. The dip-like feature has been observed up to $\sim$70 keV. The
1-110 keV broad-band spectroscopy of both observations revealed that the
best-fit model comprised of a partially absorbed Negative and Positive power
law with EXponential cutoff (NPEX) continuum model along with a blackbody
component for the soft X-ray excess and two Gaussian functions at 6.4 and 6.7
keV for emission lines. Both the lines were identified as emission from neutral
and He-like iron atom. To fit the spectra, we included the previously reported
cyclotron absorption line at 12.2 keV. From the spin-up rate, the magnetic
field of the pulsar was estimated to be $\sim$1.2$\times$10$^{12}$ G and found
to be comparable to that obtained from the detection of the cyclotron
absorption feature. Pulse-phase resolved spectroscopy revealed the pulsating
nature of the soft X-ray excess component in phase with the continuum flux.
This confirms that the accretion column and/or accretion stream are the most
probable regions of pulsar's soft X-ray excess emission. The presence of the
pulsating soft X-ray excess in phase with continuum emission may be the
possible reason for not observing the dip at soft X-rays.
