Recovering the Orbital Signal of TOI-2049 b from Public Radial-Velocity Observations

Exoplanetary systems can be studied through the gravitational influence that orbiting planets exert on their host stars. One method of detecting this motion is radial-velocity spectroscopy, in which periodic Doppler shifts in stellar spectral lines reveal the reflex motion of the star. In this study, publicly available radial-velocity observations of the known exoplanet TOI-2049 b were independently analyzed to recover its orbital signal. A dataset containing 49 radial-velocity measurements was analyzed over an observational baseline of approximately 774 days. A period search over the range of 1–100 days identified a strongest candidate period of 5.303960 days. A subsequent weighted sinusoidal fit independently recovered a period of 5.303923±0.00215 days and a radial-velocity semi-amplitude of 132.17±15.59. Phase-folding the observations using the recovered period revealed a coherent periodic pattern. Residual analysis showed that the model reproduced the dominant periodic variation but did not account for all of the observed scatter, with a residual RMS of approximately 73.6 m/s and a reduced chi-square of approximately 2.15. The recovered period and semi-amplitude are consistent with the published characterization of TOI-2049 b. The study demonstrates that publicly available radial-velocity observations can be independently analyzed to recover the dominant orbital signal of a known exoplanet while also revealing the limitations of a simplified orbital model.