Nature of X-rays from Gamma-ray Emitting Radio Galaxies

Most of the gamma-ray active galactic nuclei (AGNs) are associated with blazers with powerful jets aligned close to the line of sight. A few gamma-ray AGNs were discovered with misaligned jets, and some of them are very high energy (VHE) TeV sources. All of them are low-luminosity AGNs (LLANGs) hosted at the center of radio galaxies, generally associated with radiatively inefficient flows (RIAFs). It has been suggested that the high energy X-ray emission of these LLAGNs can come from accretion flows or from jets, but the nature of the X-rays is still uncertain. The gamma-ray to TeV emission mechanism is also not very well understood, but a popular model is the synchrotron self-Compton (SSC) emission. Using NuSTAR, Chandra, and Swift observations, we study a sample of gamma-ray emitting radio galaxies in order to understand the nature of their X-ray emission. We also discuss insights on the SSC models based on our X-ray observations. We report updates of our X-ray study and discuss recent models to understand these high energy emission processes.