  The photometric monitoring of planetary transits is an important method for
the characterization of exoplanets. Transiting exoplanets allow measurements of
the planetary radius and mass, providing information on the physical structure
of the planet. Therefore, the parameters obtained with the transit method
become fundamental for a comparative study of exoplanets in different planetary
systems. In this work, we present the results obtained from observations of a
transit event of the exoplanet HATS-24b using the new SPARC4 CCD mounted on the
1.6 m telescope of the Pico dos Dias Observatory (OPD). We have used Bayesian
statistical inference to determine the physical parameters of this exoplanet,
where we obtained a radius of 1.395+-0.057 RJup, mass of 2.26+-0.17 MJup, and
density of 1.03+-0.15 g/cm^3. We have combined our measurements of the central
time of transit and orbital period with values from the literature to obtain an
improved ephemeris for the transits of HATS-24b, Tc=(2457948.709321+-0.000039)
+ E (1.3484978+-0.0000009). We have applied the differential analysis using a
solar spectrum to recalculate the stellar surface parameters of HATS-24, where
we obtained Teff=6125+-94 K, log(g)=4.370+-0.045 cm/s^2, and
[Fe/H]=-0.229+-0.058 dex. This allowed us to estimate an equilibrium
temperature for HATS-24b of Teq=2166+-53 K. The mass and radius of HATS-24b are
consistent with the theoretical model of a pure helium-hydrogen planet at 1 Gy.
