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 \pm 0.057 R _ { J } , mass of 2.26 \pm 0.17 M _ { J } , and density of 1.03 \pm 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 , T _ { c } = ( 2457948.709321 \pm 0.000039 ) + E ( 1.3484978 \pm 0.0000009 ) .
We have applied the differential analysis using a solar spectrum to recalculate the stellar surface parameters of HATS-24 , where we obtained T _ { eff } = 6125 \pm 94 K , \log { g } = 4.370 \pm 0.045 cm s ˆ { -2 } , and [ Fe/H ] = -0.229 \pm 0.058 dex .
This allowed us to estimate an equilibrium temperature for HATS-24b of T _ { eq } = 2166 \pm 53 K. The mass and radius of HATS-24b are consistent with the theoretical model of a pure helium-hydrogen planet at 1 Gy .