Detection of exoplanets has been a fruitful task over the last decades only tarnished by the lack of confirmed exomoons. The observational bias related to the current methods of detecting exoplanets, as well as the strong dynamical effects that an exomoon of a close-in giant exoplanet undergoes, may be the cause of this absence of positive results. For these kind of systems, and according to newly models for tidal migration of exomoons that consider the evolution of planetary parameters such as its size, Love's number and tidal quality factor, the torque's interplay triggers the orbital evolution of the satellite until its semimajor-axis reaches a stationary value, nicknamed in advance as the \textit{tidal migration's braking point} (TMBP) of the system. The TMBP value mainly depends on a set of initial parameters as the moon and planet masses, distances and rotational rates. On the other hand, the detection of an exomoon is directly related to the moon's size, mass and moon-planet separation, which might be constrained by the satellital tidal biography. In this work we explored the set of initial orbital and physical parameter for a planet-moon system, to numerically asses the TMBP in order to obtain some constraints for exomoon detectability by diverse methods of namely, transits, radial velocity, TTV and TDV, with the instrumentation currently available.