Hot Jupiters are enigmatic planets, with their size and position unlike what we can compare to those in our Solar System. By studying them and learning more about their formation, the origins of our own Solar System can become more clear. HATS-24b is a hot Jupiter with a very short period and an inflated radius. These factors make it an important candidate for further study, to learn more about these kinds of planets. For this dissertation, both ground-based Prompt-8 and space-based TESS observations of HATS-24 b were used: to increase the precision of known parameters, to look for possible transit timing variations (TTVs) caused by a second planet, and to perform atmospheric retrieval. Parameters updated include an ephemeris of 2457948.709933 +- 7.3x10^-5 (BJD) and period of 1.34850230 +- 3.3x10^-7 days were found, among others. The precision, wavelength range, and quantity of the observations was not sufficient to get useful results from atmospheric retrieval. No significant TTVs were found, but limits were placed on the possible periods and masses of a second planet: a terrestrial-sized planet would need a period of at least 3 days, a Jupiter-sized planet would need a period of at least 4 days, and a brown dwarf would need to have a period of at least 13 days. This does not include the possibility of planets in orbital resonance. The lack of significant TTVs supports formation theories that predict low numbers of close planetary companions to hot Jupiters.