PPT-AGN Monitoring Workshop

MPIFR 1415 March 2011 Reduction and first results of FGAMMA data I Nestoras on behalf of the FGAMMA team General information Coordinated observations at Effelsberg and PV Typical 48h per session for Effelsberg 12h for PV. Fred Davies. ASTR 278. 2/23/12. Contents. Eddington Ratio. What does it mean?. How do we measure it?. Contents. Eddington Ratio. What does it mean?. How do we measure it?. Two regimes of measurement. 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. JWST Workshop. – . STScI. Baltimore. June 8, 2011. Mid-Infrared Observation of High . Redshift. Galaxy Evolution. Most star formation activity occurs behind dust . Chary & Pope . 2011. Bouwens. 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. Ioana. . Duţ. an. Advisors: Peter Biermann & Alan Roy. Phinney, 1994. Large-scale mechanisms: . . bar potentials. & galaxy interactions. . THEORY: . Gaseous orbits in a weak bar potential: . with VLBI at . Parkes. Stas Shabala. University of Tasmania. Why study AGN. . AGN physics. Brightest objects in the Universe, yet we don’t know:. Composition. Accretion / outflow connection. Details of interaction with environment. 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 . Nikos Fanidakis. and. C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. . Frenk. 9. th. Hellenic Astronomical Conference, Athens, Greece September 20-24, 2009. 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. RE J1034+396. Matthew Middleton. Spectral and timing similarities of AGN and . BHB. A simple scaling.... Index of -1.35 from analytical method (Vaughan et al. 2005) and large scale simulations (Middleton & Done 2010). Chris Packham. University of Texas at San Antonio. Outline. Polarization processes of importance to AGN. Scattering. Dichroism. Synchrotron. Sy’s. and BLs. MHD & the torus. Conclusions. Caveats: This review talk is being far from comprehensive, and rather focuses on some topics that I’ve enjoyed reading of late – sorry to all those I offend by not featuring their great work. 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. . D. . Barret. , IRAP FR. J.W. den Herder, SRON NL. L. . Piro. , INAF/IAPS IT. E. . Pointecouteau. , IRAP FR. The . Athena/X-IFU . X-ray view of Hot and. . Energetic . Universe: probing the. . Black .