PrefaceContents1. The High Energy Window1.1 Some fundamental concepts2. Emission processes in Active Galactic Nuclei [Bambi, Grandi, Torresi, ...]2.1 Thermal processes: 2.1.1 Optically thick and geometrically thin disk2.1.2 Hot corona: x-ray production by Thermal Comptonization2.1.3 X-ray reprocessing: iron line and Compton hump2.1.4 ADAF2.2 Non thermal Processes2.1 Synchrotron radiation2.2 Inverse Compton2.3 SSC2.4 Hadronic cascade3. AGN as a high energy laboratory [Grandi, Torresi, ...]3.1 AGN: why do we study them?3.2 Spectral energy Distribution3.2.1 Radio quiet AGN3.2.1.1 Accretion disk and soft excess3.2.1.2 Iron line and reflection3.2.1.3 Warm absorber and winds3.2.2 Radio Loud AGN3.2.2.1 Core3.2.2.2 Jets on kpc scales3.2.2.3 Radio lobes3.3 Classification of AGN3.3.1 Optical classification3.3.2 Radio classification3.3.3 Doppler Boosting3.4 Radio Quiet - Radio Loud AGN3.4.1 Radio Loudness3.4.2 Tomography of an AGN3.5 Unification of accreting black holes through all mass scales4. How to detect X-rays and gamma-rays from space: optics and detectors [Bulgarelli, Fioretti]4.1 Matter and radiation interaction4.1.1 Photoelectric effect4.1.2 Compton effect4.1.3 Pair production4.2 Fundamental Concepts4.2.1 Quantum efficiency4.2.2 Effective Area4.2.3 Energy redistribution4.2.4 Sensitivity4.2.5 Spatial Resolution4.2.6 Angular Resolution4.3 Detectors4.3.1 Scintillator (including scintillators for gamma-ray astronomy)4.3.2 Microchannel Plate4.3.3 CdTe4.3.4 CZT4.3.5 CCD4.3.6 Spark chambers4.3.7 Silicon strip detectors4.3.8 Calorimeters4.4 Mirror and focussing of photons4.4.1 Collimated System4.4.2 Focussing System4.5 Monte Carlo Simulations of X-ray and Gamma-ray Telescope4.5.1 Toolkits and frameworks4.5.2 Space radiation environment4.5.3 Spacecraft and payload mass modeling4.5.4 Analysis pipeline for the residual background evaluation5 Past, present, and future X-ray and gamma-ray missions [Bulgarelli, Guainazzi, Pollock, ...]5.1 The discovery of astrophysical X-ray sources5.2 The initial surveys5.3 The first observatories5.3.1 Explorer-115.3.2 OSO-35.3.3 SAS-25.3.4 COS-B5.3.5 Einstein5.3.6 EXOSAT5.3.7 CGRO (A general introduction here to provide the big view: moredetails in 5.8.2 and 5.9.2)5.4 Imaging proportional counters5.4.1 The ROSAT PSPC5.4.2 The ROSAT All Sky Survey (RASS)5.4.3 The broad-band perspective5.4.3.1 BeppoSAX5.4.3.2 Astrosat5.4.3.3 HXMT5.4.4 High-resolution timing5.5 X-ray CCD astrophysics5.5.1 Spectroscopic imaging of thermal plasmas5.5.1.2 SNRs5.5.1.3 Galaxies5.5.1.4 Galaxy clusters5.5.2 Surveys and the XRB5.5.3 Serendipitous source catalogs5.5.3.1 The Chandra Source Catalog5.5.3.2 The XMM-Newton EPIC Source Catalog5.5.3.3 The XMM-Newton Slew Catalog5.5.3.4 The Swift XRT catalogs5.6 The path towards hard X-ray focusing5.6.1 The BeppoSAX/PDS5.6.2 Suzaku5.6.3 NuSTAR: the focusing revolution5.7 High-resolution spectroscopy5.7.1 Gratings versus calorimeters5.7.2 Diagnostics of inte
About the Author:

Cosimo Bambi is Xie Xide Junior Chair Professor at the Department of Physics at Fudan University (China). He received his Ph.D. from Ferrara University (Italy) in 2007 and was a postdoc at Wayne State University (Michigan), IPMU at The University of Tokyo (Japan), and at LMU Munich (Germany). He moved to Fudan University at the end of 2012 under the Thousand Young Talents Program. His research interests cover several areas in gravity, cosmology, and high-energy astrophysics. He has published more than 100 papers on refereed journals as first or corresponding author, has over 3,500 citations, and his h-index is 36. He has authored three books, and edited one volume (in ASSL) with Springer.