  We present 4 new transit observations of the exoplanet WASP-28b observed
between August 2011 and October 2013. Employing another 11 transits available
in the literature we compute new ephemeris and redetermine the physical
parameters of the star and the exoplanet. Considering 3 yrs of observations, we
find no periodic TTVs or long-term variations of the inclination of the orbit,
i, or the depth of the transit, k, that could be attributable to the presence
of another planetary mass-body in the system. We also study the relations
between i and k with different factors that characterize the light-curves. The
fits suggest a possible weak correlation between k with the red noise factor,
\beta, and the photometric noise rate, PNR, and a weak anticorrelation between
i and PNR, although more points are needed to confirm these trends. Finally,
the kinematic study suggests that WASP-28 is a thin disk star.
