"Fossil galaxy groups" are identified as bright elliptical galaxies surrounded by a population of faint dwarf galaxies and an extended, hot X-ray halo. The strong relation between the optical luminosity of the dominant galaxy, and the X-ray luminosity which is attributed to the former group environment, is indirect evidence of their formation history. They are believed to be the merger remnant of a galaxy group whose members have succumb to dynamical friction and coalesced to form a single, massive elliptical galaxy. As with clusters and normal galaxy groups, the extended X-ray halo is hotter than expected for a given X-ray luminosity. Observations and simulations of clusters suggest that active galactic nuclei (AGN) are responsible for the elevated temperatures in such systems. In recent times, it is believed that AGN are triggered by merger events between galaxies, however fossil groups have likely not undergone a major merger in over a gigayear. We present the first systematic study of fossil galaxy groups at radio wavelengths in order measure the AGN frequency in these systems. These observations reveal the radio properties of the dominant elliptical galaxy after the majority of its mass has been assembled, and indirectly probe the degree to which a radio AGN are long-lived or can be sustained by processes other than major mergers.