  Measuring the stellar rotation of one of the components in eclipsing binaries
(EBs) or planetary systems is a challenging task. The difficulty is mainly due
to the complexity of analyzing, in the same light curve, the signal from the
stellar rotation mixed with the transit signal of a stellar or sub-stellar
companion, like a brown dwarf or planet. There are many methods to correct the
long-term trend of the light curve. However, the correction often erases the
signal of the stellar rotation from spots crossing the visible stellar disk and
other weaker signals like planets. In this work, we present the DiffeRencial
flUx Method of cuTting Off biNariES (DRUM TONES) to identify the signal of the
binary transits and disentangle it from stellar rotation planet signals. We
present our technique with applications to EBs from CoRoT, Kepler, Kepler K2
and TESS missions. We also applied our method to simulated synthetic EB from
the PLATO mission. Our method shows good agreement in the determination of
stellar rotation periods for few observed targets from last space missions, as
well it is naturally useful for future European missions, such as PLAnetary
Transits and Oscillations of stars (PLATO).
