PDF-AGN and Radio Galaxy Studies AGN and Radio Galaxy Studies with LOFAR a

Andrei LobanovMPIfR Bonn AGNRG ScienceAGNRG Science AGNRG drivers for LOFAR and SKA astrophysical masers nuclear regions of AGN physics of relativistic and mildly relativistic outflows kinetic. Anatomy of Extragalactic . R. adio Sources. Miley. Symposium May, 2013, Chris Carilli NRAO. ‘Radio Galaxies as beacons to early, massive galaxy formation’. Anatomy at low redshift. High luminosity (FRII, L. :. 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 . David Roberts, Jake Cohen, & Jing Lu. Brandeis University. Lakshmi . Saripalli. & Ravi . Subrahmanyan. Raman Research Institute. 1. Radio Galaxies. X-Shaped Radio Galaxies. Cheung’s Sample. 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. Manuel Aravena, Jeff Wagg, . Padelis. Papadopoulos, . Ilana. . Feain. Outline. Introduction: the ULIRG to QSO evolutionary scenario. A high-resolution search for molecular gas in optically bright . 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 . w. eb . Ryan Shannon, . ICRAR-Curtin/. ATNF (. Vikram. Ravi, Swinburne . Pulsar . Group). Outline. Fast radio bursts (. FRBs) . Exciting times!. FRB 131104 . The . (improbable/real-time) . discovery of an FRB to the Carina dwarf spheroidal. Heino Falcke . Radboud University, Nijmegen. ASTRON, . Dwingeloo. What we (don’t) know about UHECRs . We know:. their energies (up to 10. 20. eV).. their overall energy spectrum. We don’t know:. The SETI Project. Lesson 6: Where to Survey. Questions? Please contact Carolyn Donelan @ carolyn.donelan@richlandone.org.. The GAVRT SETI Project. The GAVRT SETI Project will search most of the stars in our galaxy, in all the frequencies the telescope (named DSS-28) can reach (in 200 MHz increments).. Extragalactic radio . s. ources and their importance for astronomy. Leiden 10-13 June 2013. Ron Ekers. CSIRO, . Australia. George Miley. The largest, the furthest, the most powerful, and to some of us the most fascinating objects known in the Universe are to be found among the radio sources associated with some elliptical galaxies and QSO’s. In recent years it has become apparent that they are also objects of considerable beauty.. The Hubble Deep Field. 10 day exposure –field located in the Big Dipper. Edwin Hubble. Edwin . Hubble. Hubble’s Galaxy Classification . Spiral Galaxies. galaxies like the Milky Way with arcing structures lying in a plane and emanating from the nuclear bulge. Exoplanets. Jake D. Turner. University of Virginia. astrojaketurner@gmail.com. Exoplanet Magnetic Fields . Motivation. Interior . structure . Star. -planet Interactions. Habitability. Jake . Turner (. Are Nebulae within or outside of our galaxy??. Nebula comes from a Greek word meaning Cloud. April 1920, National Academy of Sciences , Washington, DC. Harlow Shapley (had determined size of Milky Way Galaxy) pushed that nebulae were relatively close by objects.. 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.