Active Galactic Nuclei This AGN textbook gives an overview on the current knowledge of the Active Galacitc Nuclei phenomenon. The spectral energy distribution will be discussed, pointing out what can be observed in different wavebands. The different physical models are presented together with formula important for the understanding of AGN physics. Furthermore, the authors discuss the AGN with respect to its environment, host galaxy, feedback in galaxies and in clusters of galaxies, variability, etc. and finally the cosmological evolution of the AGN phenomenon. This book includes phenomena based on new results in the X-Ray and gamma-ray domain from new telescopes such as Chandra, XMM-Newton, the Fermi Gamma-Ray Space Telescope, and the VHE regime not mentioned so far in AGN books. Those and other new developments as well as simulations of AGN merging events and formations, enabled through latest super-computing capabilities. From the contents: The observational picture of AGN Radiative processes The central engine AGN types and unification AGN through the electromagnetic spectrum AGN variability Environment Quasars and cosmology Formation, evolution and the ultimate fate of AGN What we do not know (yet)

Dieses Lehrbuch präsentiert die heutigen Erkenntnisse zum Phänomen der aktiven galaktischen Kerne (AGN), erläutert die Verteilung spektraler Energie sowie verschiedene physikalische Modelle und erörtert verschiedene physikalische Modelle.

1 Active Galactic Nuclei: A summary2 The observational picture of AGN2.1 From Welteninseln to AGN2.2 Broad lines, narrow lines, and the big-blue bump2.3 Jets and other outflows2.4 X-Ray Observations: Probing the innermost regions2.5 Up, up and away: from gamma-rays toward the TeV range3 The Central Engine3.1 The Black hole3.1.1 Approaching a black hole3.1.2 Evidence for black holes in AGN3.1.3 Schwarzschild metric3.1.4 Rotating black holes: the Kerr metric3.2 Accretion3.2.1 Accretion Basics: Bondi Accretion and the Eddington Limit3.2.2 Accretion and viscous dissipaation in a Thin Disk3.2.3 Accretion in Thick Disks3.2.4 Advection dominated accretion flows3.3 Absorption close to the black hole3.3.1 The Torus model3.3.2 Absorption in the disk3.3.3 Disk winds3.3.4 Alternative absorption models3.4 Narrow and Broad line regions3.5 Reverberation Mapping: Probing the Scale of the BLR3.5.1 Photo-Ionization Modeling3.6 AGN Jets: Emission, Dynamics and Morpologies3.6.1 Raising the jet3.6.2 Shocks and Knots3.6.3 Superluminal Motion4 AGN Types 94.1 Seyfert galaxies4.1.1 Narrow Line Seyfert Galaxies4.1.2 LINER4.1.3 ULIGs4.2 Radio Galaxies4.3 Quasars4.3.1 Radio Quiet Quasars4.3.2 Radio Loud Quasars: FSRQs, BL LACs and Blazars4.4 Unification of AGN4.4.1 Radio loud versus radio quiet4.4.2 Breaking the unification5 AGN through the electromagnetic spectrum5.1 Radio: resolving the central engine5.2 Infrared: Dust Near And Far5.3 Optical: where it all began5.4 UV: The Obscured Inner Disk5.5 X-rays: absorption, reflection, and Relativisticlly Alterd Line Progiles5.6 Gamma-rays: The Blazar Dominatated Sky5.7 VHE: the evolving domain5.8 The whole picture: the spectral energy distribution5.8.1 The synchrotron branch5.8.2 The inverse Compton branch5.8.3 Host galaxy contributions5.8.4 The disk component6 Environment6.1 Host galaxies of AGN6.2 The AGN starburst connection6.3 AGNs in clusters of galaxies7 Formation, evolution and the ultimate fate of AGN7.1 The first AGN: How Did They Form?7.2 AGN evolution7.2.1 The Number-Flux Relation7.2.2 The V/Vmax test7.2.3 Luminosity Function7.3 The late stages of an AGN?s life