PPT-Polarization & The AGN Torus

Chris Packham University of Texas at San Antonio Outline Polarization processes of importance to AGN Scattering Dichroism Synchrotron Sys and BLs MHD amp the torus Conclusions Caveats This review talk is being far from comprehensive and rather focuses on some topics that Ive enjoyed reading of late sorry to all those I offend by not featuring their great work. 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. . . . . 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. The value of . reionization. fraction derived from CMB polarization measurements has decreased steadily since WMAP2003 (WMAP2005, WMAP2007, WMAP2011, and Planck 2015). The final word from Planck is not out yet , and whenever it is out, it will surely not be “a 100-sigma measurement” of . 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 . Jeffrey Hatef. Mentor: Dr. Alan . Kogut. Inflation Theory: How is the Universe so big?. The universe appears too big, inflation is a possible answer.. COBE and WMAP. COBE beginning in 1989 and WMAP in 2001 have mapped the sky in the microwave range.. Class Activities: . Polarization (1). Class Activities: . Polarization (2). A stationary point charge +Q is near a block of polarization material (a linear dielectric). The net electrostatic force on the block due to the point charge is . . Achuta Kadambi. , . Vage. . Taamazyan. , . Boxin. Shi. , . and Ramesh Raskar. Camera Culture Group, MIT Media Lab . Contribution. Take-home message:. Verification. Solution. Compare with other depth enhancement techniques . Yaroslav. Derbenev. Center for Advanced Study of Accelerators. Jefferson Laboratory. EIC . Collaboiration. Meeting , January 10-12, 2010. Stony Brook, Long Island. Outline. Polarization of Ions (protons, deuterons, . . Paul McMillan. Lund/Oxford. Ringberg. Streams meeting, July 2015. Collaborators: James . Binney. , Jason Sanders. Modelling. streams (not orbits). Streams don’t follow orbits.. Streams exist because stars are put onto different orbits.. Wave 3 continue. Polarization. Polarization is a process of turning . unpolarized. light to polarized light. A light wave is an electromagnetic wave that travels through the vacuum of outer space. Light waves are produced by vibrating electric charges.. I. . Myserlis. E. . . Angelakis. (PhD advisor), L. . . Fuhrmann. , V. . Pavlidou. , A. Kraus, I. . Nestoras. , V. . Karamanavis. ,. . J.A. . Zensus, T. P. . Krichbaum. From the RoboPol team:. O.G. . Dispersion of light. Visible light = full spectrum . wavelengths range from 400 nm to 700 nm. Different wavelengths have ever so slightly different indices of refraction when passing through materials such as glass, plastic, or water (and probably others). Alexander . Polnarev. QMUL, School of Physics and Astronomy, London, UK. Tarusa. , 10 September 2015. Talk Overview:. Introduction: . Free electrons + Anisotropy = Polarization. The History of Polarization in Cosmology: .