  Plages are the magnetically active chromospheric structures prominently
visible in Ca $\scriptsize{{\textrm{II}}}$ K line (3933.67 \r{A}). A plage may
or may not be associated with a sunspot which is a magnetic structure visible
in the solar photosphere. In this study we explore this aspect of association
of plages with sunspots using the newly digitized Kodaikanal Ca
$\scriptsize{{\textrm{II}}}$ K plage data and the Greenwich sunspot area data.
Instead of using the plage index or fractional plage area and their comparison
with the sunspot number, we use, to our knowledge for the first time, the
individual plage areas and compared it with the sunspot area time series. Our
analysis shows that these two structures formed at two different layers are
highly correlated with each other on a time scale comparable to the solar
cycle. The area and the latitudinal distributions of plages are also similar to
that of the sunspots. Different area thresholdings on the `Butterfly diagram'
reveal that plages with area $\geq$4 arcmin$^2$ are mostly associated with a
sunspot in the photosphere. Apart from this, we found that the cyclic
properties change when different sized plages are considered separately. These
results may help us to better understand the generation and the evolution of
the magnetic structures in different layers of the solar atmosphere.
