PPT-AGN evolution:

a panchromatic view Andrea Merloni MPE Merloni FERO 8 September 2016 Introduction What FERO is about Detailed physical modelling of the inner region of AGN A few bright sources lots of photons extensive observational campaigns. Formation and cosmic evolution of massive black holes. Andrea Merloni. MPE, Garching. Syllabus. Monday:. Observational evidence of Supermassive Black Holes. AGN surveys. Tuesday: . The evolution of SMBH mass function and spin distributions. Tori. : . Theory & Observations. Moshe . Elitzur. . University of Kentucky . Unified Scheme for AGN. M. . ~ 10. 6 . – 10. 10. M. . R. s. ~ 10. 11 . – 10. 15 . cm. T. oroidal. Smolcic. . ea. ). Compilation based on different star formation estimators (UV, IR, radio, Hα..). Large scatter: Dust obscuration is major problem. Hopkins & . Beacom. (2006) compilation. redshift. は階層的銀河形成論で説明. できるか？. Motohiro. 　. Enoki. Tomoaki Ishiyama (Tsukuba Univ.). Masakazu A. R. Kobayashi (Ehime Univ.). Masahiro . Nagashima. . (Nagasaki Univ. .). §1. Introduction. Harry Ferguson (STScI). Feedback. Behroozi. + 2011. Halo quenching. Quasar mode AGN. Radio Mode AGN. (. SNe. ). SNe. Satellites: Ram pressure, tides, shocks…. UV back-ground. AGN feedback in . SAMs. Capetti. , . R. Baldi, B. Balmaverde, S. Buttiglione. AGN 10 - Roma 10/09/2012. WHY AN AGN CENSUS?. A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, . E.G.. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION . Tiziana Venturi. . tventuri@ira.inaf.it. Active Galactic Nuclei 9 Ferrara, 27.05.2010. Radio VLBI . as. the . most. . direct. way . to. Violette Impellizzeri (NRAO). Alan Roy (. MPIfR. ), Christian Henkel (. MPIfR. ). The unified scheme of AGN. Diversity of AGN classes explained by a single unified scheme :. The nuclear activity is powered by a . Andrei LobanovMPIfR, Bonn AGN/RG ScienceAGN/RG Science AGN/RG drivers for LOFAR and SKA: astrophysical masers, nuclear regions of AGN, physics of relativistic and mildly relativistic outflows, kinetic Electra . Panagoulia. Institute of Astronomy, Cambridge, UK. W. ith: Andy Fabian. Jeremy Sanders. Julie . Hlavacek-Larrondo. X-ray View of Galaxy Ecosystems . 11. th. July 2014. Hee. -Won Lee. Department of Physics and Astronomy. Sejong. University. 2015. 1. 27. Content. Introduction. Scattering . and Unification of AGN. Scattered Ly . alpha. Balmer. Wings. Discussion. Active Galactic Nuclei. VG. So we want a color magnitude diagram for AGN so that by looking at the color of an AGN we can get its luminosity. But AGN have no fusion, why would we expect a color-magnitude relation?. The gas that accretes onto the black hole is still hot and so must follow the Blackbody Radiation law. . The. . XMM ultra-deep survey in the CDFS. . Andrea Comastri . INAF-Osservatorio Astronomico Bologna ITALY. P. Ranalli (UniBO), R. Gilli (INAF-BO), C. Vignali (UniBO),. K. Iwasawa (ICC-Barcelona), I. Georgantopoulos (INAF-BO), N. Cappelluti (INAF-BO), E. Rovilos (INAF-BO), X. Barcons (IFCA), F.J. Carrera (IFCA), S. Falocco (IFCA), M. Brusa (MPE), H. Brunner (MPE), I. Balestra (MPE), A. Merloni (MPE), A. Finoguenov (MPE), F. Civano (CfA), F. Fiore (INAF-Roma), F. Nicastro (INAF-Roma), S. Puccetti (ASI), V. Mainieri (ESO), P. Rosati (ESO), P. Tozzi (INAF-TS), N. Brandt (PSU), J. Silverman (IPMU). XRB. and . AGN. . Accretion . Processes. Anca. . Constantin. James Madison Univ.. W/. Paul . Green(SAO. ) . Tom . Aldcroft. (SAO. ). HongYan. . Zhou(USTChina. ). Daryl Haggard (. UWashington. ).