A Search For the Possible Planetary Companions of Hot Jupiters

Regarding the origin of Hot Jupiters, a topic that remains mysterious forcontemporary astronomers, current theories primarily diverge into two distinct hypotheses. The first posits disk-driven migration theory, while the second advocates for high-eccentricity migration theory. The former hypothesis suggests that Hot Jupiters are frequently accompanied by additional planetarycompanions, whereas the latter implies that systems with such configurations are comparatively rare. In this analysis, we meticulously examine four systems:TOI-1259, TOI-1130, TOI-2337, and XO-7, utilizing data collected by the Transiting Exoplanets Survey Satellite (TESS) over recent years. Each of these systems harbors at least oneHot Jupiter orbiting its host star (with some systems containing two stars). Our principal objective is to detect potential smaller planets with larger orbits, or planetary companions, by processing the raw data employing computational methods and Python programming. We retrieve data from TESS and select sectors with an exposure time of 120 seconds, subsequently coalescing them into a unified light curve. Subsequent to eliminating inferior data quality and isolating the transit dips attributable to the known Hot Jupiters, we exclude these dips to obtain a light curve unaffected by the presence of gas giants. Utilizing the Box-Least-Squares technique, we identify the period with the highest likelihood and seek a distinct peak within a relatively flat baseline in the graphical representation. Ultimately, we fold the light curve according to the calculated period, scanning for a conspicuous dip that would indicate the presence of an additional planet. By predicting whether these systems have planetary companions,we can measure the probability and obtain a guess that the high-eccentricity migration theory may be more likely.