Origin of the emission at centimeter wavelengths in the transitional disk surrounding T Chamaleontis

In this work we present an attempt to characterize the emission at centimeter wavelengths in T Chamaleontis, one of the most intriguing transitional protoplanetary disks of the southern hemisphere. Transitional disks are considered as the missing link between disks surrounding young stars and planetary systems. They are characterized by the presence of gaps in their radial dust distributions, which may be originated by photo-evaporative winds, close stellar companions, planets in formation, and grain growth, among other mechanisms. Emission at 0.7 cm and 1.7 cm can be produced by the contribution of different phenomena involving dust emission from large dust grains and free-free radiation from an ionized jet, ionized winds, accretion shocks near the central protostar, non-thermal synchrotron emission from the stellar chromosphere, or photoevaporative winds. Radio interferometers working at centimeter wavelengths offer the possibility for resolving the population of large dust grains on disks and provide insights on the origin of free-free emission. Using the Australia Telescope Compact Array (ATCA) observations we resolve the continuum emission at 0.7 cm and 1.7 cm surrounding T Chamaleontis, the first T Tauri star with observational evidences of planetary formation inside a disk gap. In this contribution we discuss on the possible nature of this emission at centimeter wavelengths.