The Frequency Modulation (FM) Method, first proposed by Shibahashi et al. (2012) and expanded upon in 2015, provides a way to detect binary motion in pulsating stars using only photometric data. Orbit..
The Frequency Modulation (FM) Method, first proposed by Shibahashi et al. (2012) and expanded upon in 2015, provides a way to detect binary motion in pulsating stars using only photometric data. Orbital motion produces frequency shifts that appear as multiplets in the Fourier transform of the light curve, with spacing equal to the orbital frequency from the central peak. The relative amplitudes and phases of these peaks can be used to derive orbital parameters—offering a purely photometric alternative to spectroscopic radial velocity (RV) measurements. This project applies the FM method to confirm potential subdwarf B (sdB) companions that have been suggested by the Observed–Calculated (O-C) timing method, to compare the two methods using long-baseline, high-precision data from TESS, Kepler, and similar missions.
