Hot-Jupiters are the outcome of giant-planet's migration. If their regular moons survive these processes, the angular moment exchange between the star, the planet and the moon could drive the satellite towards an unbounded state, becoming a new planetary embryo of the system (a \textit{ploonet}). In spite of the diverse branches of fates of these ejected objects and their intrinsic chaotic dynamic behavior, our numerical simulations have shown that a set of these ploonets survive for long timescales in quasi-coorbital configurations to their host planets. If we also suppose that ejected moons are volatile-rich bodies, the stellar radiation at close-in distances trigger an intense sublimation and erosion processes of their surfaces and atmospheres respectively, during both planetocentric migration and siderocentric evolution if they orbits remain closer. Observations of the aforementioned systems should exhibit some recognizable footprint: firstly a noisy major transit (concerning to the host planet) and a minor transit (due to the ploonet) with a similar orbital period, and secondly, a huge vapor trail as the outcome of the photo-evaporation processes that could explain the unusually extended circumplanetary and circumstellar disks already proposed in newly observational works. In this work we combine numerical simulations and semi-analytical estimations to, initially, asses the orbital evolution and fate of a ploonet and, subsequently, to estimate its surface and atmospheric erosion and their size evolution, to finally discuss about the main features that these systems would exhibits in transit detections.