Top:thermal energy required for an H atom to escape a planetary potential as a function of planet density. The size of each data point reflects the density of the planet. For example, for Earth, T_min = 5035 K, whereas the denser planets have much higher tempratures, above 10 000 K. Bottom: BB temperature vs. distance from Sgr A* of the 28 EPs, purely due to heating from the active (inserted subplot: older EPs) and the quiescent (main plot: younger EPs) states of Sgr A*.