PPT-Radio and X-ray emission in radio-quiet quasars

Katrien C Steenbrugge Katherine M Blundell and Zdenka Kuncic Instituto de Astronom ía UCN Department of Physics University of Oxford School of Physics University of Sydney. :. Active Galactic Nuclei: powerful energy sources in . “nuclei” . (. central ~1 pc) . of some galaxies. Main types. : . Seyferts. , radio galaxies and quasars. Other variants we’ll skip.. Power source: accretion of matter onto a supermassive black . R. N. Manchester. CSIRO Astronomy and Space Science Australia . Telescope National Facility. , Sydney. Summary. Pulse profiles – doubles and . interpulses. High . Edot. pulsars – radio and high-energy emission. S. ources associated with. Broad Absorption Line . Q. uasars. Takayuki HAYASHI (. Univ. of . Tokyo, NAOJ). A member of AGN WG in SKA-. jp. A. DOI . (ISAS/JAXA), . H. . NAGAI . (NAOJ). G. . Bruni. Laura Chomiuk. Jansky. Fellow, Michigan State University. Supernova Types: I vs. II. Type I:. No Hydrogen. Thermonuclear WD explosions (. Ia. ) . and. . Core collapse of massive stars stripped of H envelopes (. Most of the power of galaxies come from the stars. Almost all nearby galaxies. Some galaxies have very bright sources right at the center. Can be as bright as a galaxy!. Or even much brighter. Called . Sources. 1. Sources of high-energy particles. We now have clear observational diagnostics for particle acceleration. synchrotron radiation (radio, sometimes X-ray). inverse Compton scattering (X-ray, . Anisotropic Radiative Feedback of . Active Galactic Nuclei. Shuang-Nan Zhang. ,. Yuan Liu. ,. Jin Zhang. . Institute of High Energy Physics. and. National Astronomical Observatories of China. Chinese Academy of Sciences. Will Potter. Junior Research Fellow, . University of Oxford. Outline. An extended relativistic fluid jet emission model based on observations of M87.. Fitting radio observations to constrain the structure and dynamics of jets.. ASKAP. Marcin Glowacki. Supervisors: Elaine Sadler & James Allison. Reddened Quasars. Hopkins et al. (2006). 2. Reddened Quasars. Hopkins et al. (2006). 3. Reddened Quasars. Hopkins et al. (2006). Surface accuracy not so important, so easy to make large one.. angular resolution . . . wavelength. mirror diameter. D larger than optical case, but wavelength . much. larger (cm's to m's), e.g. for wavelength = 1 cm, diameter = 100 m, resolution = 20".. Material for this talk: A.M.S. Richards, T.W.B.Muxlow, N.J.Jackson (JBCA Manchester); . R.A.Laing (ESO Garching); I. Marti-Vidal (OSO, Onsala); R. Perley (NRAO Socorro) and Wikipedia. Summary. Radio astronomy – key aspects. Exoplanets. Jake D. Turner. University of Virginia. astrojaketurner@gmail.com. Exoplanet Magnetic Fields . Motivation. Interior . structure . Star. -planet Interactions. Habitability. Jake . Turner (. Magnetar. Joseph . Gelfand. . (NYUAD / CCPP) . Scott Ransom (NRAO), . Chryssa. . Kouveliotou. (GWU),. . Mallory S.E. Roberts (NYUAD), Hind Al Ali (NYUAD), Yoni . Granot. 2015 December 17. 1. 28th Texas Symposium on Relativistic Astrophysics. Amy Kimball. NRAO Charlottesville (. NAASC. ). Why is quasar “feedback” important for galaxy formation. . (and what are the two feedback modes)?. How to identify candidate “most extreme feedback” objects.