PPT-A Unified AGN Structure: From X-ray Absorbers

to the Blazar Sequence and the MeV Blazars DK Keigo Fukumura Chris Shrader Ehud Behar Ioannis Contopoulos Stella Boula Apostolos Mastichiadis The WellKnown AGN Cartoon A sum of disjointed components that map the zeroth order AGN phenomenology. The Xray absorbing gas is often called a warm absorber because UV observations show that it is accompanied by very weak or no signi64257cant absorption at the H I Lyman limit 912 A The gas must be substantially ionized much more H II than H I and he They support the machine and iron out the bumps without need for regular servicing However even though damper units are not serviceable there are occasions when it is necessary to dismantle the units You may decide to fit covers different from stand 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. 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. porous absorber resonance absorber (Helmholtz absorber) mail: wolfgang.kropp@chalmers.se Porous absorber In contrary to the wave propagation in structures, for gases the influence of shear forces ca 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. 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. 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. Jae Woong Yoon. , . Kyu. Jin Lee, . Manoj. . Niraula. , Mohammad . Shyiq. . Amin. ,. and Robert Magnusson. Dept. of Electrical Engineering, University of Texas – Arlington, TX 76019, United States. . Sushil Sharma. for the ME Group. Outline. Raytracing. Background. SR raytracing. Frontend raytracing. SR High-Power Absorbers. Crotch absorbers. Damping wiggler (DW) absorbers. Frontend High-Power Components. Jelle Kaastra. Jerry . Kriss. , Massimo . Cappi. , . Missagh. . Mehdipour. , Pierre-Olivier . Petrucci. , . Katrien. . Steenbrugge. , Nahum . Arav. , Ehud Behar, . Stefano . Bianchi, . Rozenn. . Boissay. Denis . Martynov. University of Birmingham. Overview. Input power of 500 W. Parametric instabilities. Angular instabilities. Uniform absorption. Point defects. 500 W laser. Currently we have 75 W with a solid state laser.