PPT-SDSS Quasar Science

With thanks to the members of the Quasar Working Group particularly Don Schneider Xiaohui Fan Michael Strauss Pat Hall Dan Vanden Berk Sebastian Jester and Scott Anderson also Adam Myers. Constraining Dark Energy with intermediate-. redshift. probes. Hubert . Lampeitl. University Portsmouth, ICG. In collaboration with:. H.J. . Seo. , T. . Giannantonio. , C. Shapiro, R.C. Nichol, B. Bassett, W.J. Percival, T. Davis, . White Dwarfs . in . SDSS . . Estimating the Mean Mass of Normal . DAs . and . DBs . Kepler. Scot . Kleinman. , Atsuko Nitta. B. árbara. Castanheira, . Detlev. Koester. Marcos Diaz . H. a. H. b. Quasars. Quasars were . discovered by the . radio waves that they give off. Scientists at first had no idea what to these disruptions could possibly be. They still really don’t know.. Because of the initial ambiguity surrounding the Quasars they . Massive Black Holes. Stephen Fine. Outline. What is a quasar. How do we study quasar black holes. Why do we study quasar black holes. What are the current difficulties in studying black holes. How can we improve on the current situation. . Reionization. . . Chris . Carilli. (. M/N. RAO). Vatican Summer School June 2014. I. Introduction: Cosmic . Reionization. Concept . . Cool gas in z > 6 galaxies: quasar hosts. Constraints on evolution of neutral Intergalactic Medium (IGM). Status and future developments. Luigi Boschetti, David Roy, . Chris Justice, Steve Stehman and Louis Giglio. Current version is C5 . . first global run of the product. . run on purpose with conservative thresholds. Division of Particle and Astrophysical Science, Nagoya University, JAPAN. with. SKA-Japan high-. z. galaxy and cosmology WG. East-Asia SKA core member meeting, 29 May, 2012, ASIAA, Taipei, Taiwan. Fluctuation, Stars, and Galaxies: Light and Shadow of the Cosmic Structure Formation through H. Gordon Richards. Drexel University. With thanks to. Michael Strauss, . Yue. . Shen. (Princeton), Don Schneider, Nic Ross (Penn State), Adam . Myers (Illinois. ), Phil Hopkins (. Berkeley. ), . and a host of other people from the SDSS Collaboration. 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. . Division of Particle and Astrophysical Science, Nagoya University, JAPAN. with. SKA-Japan high-. z. galaxy and cosmology WG. East-Asian SKA WS, 30 . Nov. .-2 Dec., 2011, KASI, . Daejeon. , Korea. Formation and Evolution of Galaxies:. Mark Kidger. European Space Agency. European Space Astronomy Centre. Herschel Science Centre. What is a Quasar?. Quasar is a contraction of . Quasi-Stellar Object. .. They are objects that look like faint, blue stars, but are really incredibly distant.. Chandra. and the Inner Structure of AGNs. Warm Absorbers, X-ray Eclipses and . Broad Line Region Inflows, a unification. Martin Elvis. Harvard-Smithsonian Center for Astrophysics. Chandra. taught us about AGN structure. Ultra Metal - Poor (UMP ; [Fe/H] - 4 . 0 ) stars hold the key to the nucleosynthesis processes associated with first - generation stars in the Universe . However, only about two dozen UMP stars have b 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.