  Exoplanet discoveries have motivated numerous efforts to find unseen
populations of exomoons, yet they have been unsuccessful. A plausible
explanation is that most discovered planets are located on close-in orbits,
which would make their moons prone to tidal evolution and orbital detachment.
In recent models of tidally-driven migration of exomoons, evolving planets
might prevent what was considered their most plausible fate (i.e. colliding
against their host planet), favouring scenarios where moons are pushed away and
reach what we define as the "satellite tidal orbital parking" distance
($a_\mathrm{stop}$), which is often within the critical limit for unstable
orbits and depends mainly on the system's initial conditions: mass-ratio,
semi-major axes, and rotational rates. By using semi-analytical calculations
and numerical simulations, we calculate $a_\mathrm{stop}$ for different initial
system parameters and constrain the transit detectability of exomoons around
close-in planets. We found that systems with $M_\mathrm{m}/M_\mathrm{p} \geq
10^{-4}$, which are less likely to form, are also stable and detectable with
present facilities (e.g. Kepler and TESS) through their direct and secondary
effects in planet+moon transit, as they are massive, oversized, and migrate
slowly. In contrast, systems with lower moon-to-planet mass ratios are
"ephemeral" and hardly detectable. Moreover, any detection, confirmation, and
full characterisation would require both the short cadence capabilities of TESS
and high photometric sensitivity of ground-based observatories. Finally,
despite the shortage of discovered long-period planets in currently available
databases, the tidal migration model adopted in this work supports the idea
that they are more likely to host the first detectable exomoon.
