  The rotational profile of the Sun is considered to be one of the key inputs
in a solar dynamo model. Hence, precise and long-term measurements of this
quantity is important for our understanding of solar magnetism and its
variability. In this study, we use the newly digitized, white light sunspot
data (1923 -- 2011) from Kodaikanal Solar Observatory (KoSO) to derive the
solar rotation profile. An automated correlation based sunspot tracking
algorithm is implemented to measure the rotation parameters, $A$, the
equatorial rotation rate and $B$, the latitudinal gradient. Our measurements of
$A=14.381\pm0.004$ and $B=-2.72\pm0.04$ compare well with previous studies. In
our analysis, we find that the bigger sunspots (with area $>$400~$\mu$Hem)
rotate slower than the smaller ones. At the same time, we do not find any
variation in the rotation rates between activity extremes, i.e solar maxima and
minima. Lastly, we employ our tracking algorithm on the Michelson Doppler
Imager (MDI) data and compare the MDI results with our KoSO values.
