X-rays from the Corona and Disc of AGN Andy Fabian Institute of Astronomy University of Cambridge 3C273 N = 0, 1020, 1022, 1024 cm−2 H 0 1 − 0 1 ) 1 1 − 1 V − 0 e 1 k 1 − s 2 − m Opt UV X−ray c s n o t o 2 h 1 P − 0 ( 1 2 V e k 3 1 − 0 10−4 10−3 0.01 0.1 1 10 100 1000 1 Energy (keV) N = 0, 1020, 1022, 1024 cm−2 H 0 1 − 0 1 ) 1 1 − 1 V − 0 DISK e 1 k 1 − s 2 − m Opt UV X−ray c s n o t o 2 h 1 P − 0 CORONA ( 1 2 V e k 3 1 − 0 10−4 10−3 0.01 0.1 1 10 100 1000 1 Energy (keV) N = 0, 1020, 1022, 1024 cm−2 H 0 1 − 0 1 Effect of Galactic absorption ) 1 1 − 1 V − 0 e 1 k 1 − s 2 − m Opt UV X−ray c s n o t o 2 h 1 P − 0 ( 1 2 V e k 3 1 − 0 10−4 10−3 0.01 0.1 1 10 100 1000 1 Energy (keV) To observer Direct Power-law Corona Accretion disc (Quasi-blackbody emission in optical and UV for AGN) Corona is compact Rapid variability in AGN MCG-6-30-15