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, . Redshifts. Gordon Richards. Drexel University. With thanks to. Michael Strauss, . Xiaohui. Fan, Don Schneider, and . Linhua. Jiang. Quasar Luminosity Function. Croom. et al. 2004. Space density of quasars as a function of . Yue . Shen. Carnegie Observatories. In collaboration with Brandon . Kelly (UCSB). M. otivation. T. he abundance (and clustering) of quasars are key to understand the evolution of quasars/SMBHs in the hierarchical structure formation paradigm . 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. Paul Hewett (. IoA. , Cambridge). James Allen (U. Sydney). Outline. Motivation: . quasar . clustering, . host-galaxy and local quasar environment, relation . to Ly. α. -absorbers and the inter-galactic medium, outflow properties of quasars themselves. http://www.pa.uky.edu. Only 10% of the class has completed the evaluations so far.. I will add 5 points on your final exam if you complete the evaluation.. Today’s model for the formation of the Milky Way and other galaxies. 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. Reionization. . Chris . Carilli (NRAO). LANL Cosmology School, July . 2011. . Review: constraints on IGM during . reionization. CMB large scale polarization. Gunn-Peterson effect. Quasar near zones: . 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.. Ashley . Pagnotta. (very old novae), . Ben Oppenheimer (. chemistry of hot Jupiter atmosphere). , . MS + Dave . Zurek. . (. Magellanic. dwarf novae). . Adric. . Reidel. (young . red. dwarfs). Jackie . 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 Charles L. Steinhardt. 1. , . Heng. . Hao. 2. , . Monica . Young. 3. , . Guido Risaliti. 4. , . Francesca . Civano. . Harvard-Smithsonian . Center. for Astrophysics. and. 1. IPMU, Univ. Tokyo; 2..