PPT-The survey for new AGN candidates

Author : cheryl-pisano | Published Date : 2016-08-01

within the field of Fermi unassociated gammaray sources Yamaguchi U niv Yoshitaka FUJINAGA K Ninuma A Kimura K Fujisawa K Akutagawa K Sugiyama K Motogi Yamaguchi

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The survey for new AGN candidates: Transcript

within the field of Fermi unassociated gammaray sources Yamaguchi U niv Yoshitaka FUJINAGA K Ninuma A Kimura K Fujisawa K Akutagawa K Sugiyama K Motogi Yamaguchi Univ . . Statistics. : . 1.8 . Ms. ½. . sq. .deg. . @. 160 . ksec. 1761 . sources. Dec. ’06-June ’07. Catalog. : . Elvis . et. al., . 2009, ApJS 184, 158. Martin Elvis, Francesca . Civano. , . Aldcroft. 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. . . . . MIR imaging & . s. pectroscopy. ISM dust model & PAH. . vectorized. Monte Carlo model . SED of a clumpy AGN torus. Frank . Heymann. (PhD), Martin Haas, . Endrik. . Kr. 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. and . Galaxy Evolution. Meg Urry. Yale University. ~All galaxies host supermassive black holes. The . formation. and . evolution. of . galaxies. is closely tied to. the . growth. of . black holes. 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. 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. 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. 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. Tiziana Venturi. . tventuri@ira.inaf.it. Active Galactic Nuclei 9 Ferrara, 27.05.2010. Radio VLBI . as. the . most. . direct. way . to. . GIOVANNOLI. Laboratoire. . d’Astrophysique. de Marseille, FRANCE. Advisor : Veronique BUAT. C. ollaborators. : Denis . Burgarella. , Stefan Noll. Spectral . energy. distribution . modeling. . 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. .

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