PPT-Determining broad-band spectra of radio galaxies with the EVLA

Jeremy Harwood YERAC 2011 Background Image courtesy of NASACXCCfARKraft et al MPIfRESOAPEXA Weiss et al ESOWFI What are radio galaxies Type of active galaxy Fanaroff and Riley class I. Both of these occur around 3300 cm. -1. , but they look different.. Alcohol O-H. , broad with rounded tip.. Primary amine . (RNH. 2. ), broad with two sharp spikes.. Secondary amine . (R. 2. NH), broad with one sharp spike.. 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. Anja. von . der. Linden et al., 2007, MNRAS, 379, 867. On the prevalence of radio-loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows. P. N. Best et al., 2007, MNRAS, 379, 894. None Narrow Narrow Broad Broad Broad Narrow Broad Narrow None Narrow Narrow BroadNone Broad None Narrow Broad None Broad None Broad NarrowNoneNarrowNarrow Narrow Broad Narrow NarrowBroad Narrow Broad Paul . Nulsen. (. CfA. ), Christine Jones (. CfA. ), . William Forman (. CfA. ), Eugene . Churazov. (MPA),. Laurence David (. CfA. ), Brian McNamara (Waterloo),. Steven Murray (. CfA. ) . AGN Outbursts in Giant . :. 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 . Lawrence Rudnick, University of Minnesota. Deep+wideband+polarization. ~30. m. Jy,800sq . deg. 700-1800. More science using subsamples. This is single project from large survey. Feasible with JVLA only: NVSS level investment. Richard . Prestage. (Marian . W. . Pospieszalski, Steve White, Steve Durand). Noise Temperature Summary of Cryogenic HEMTs. ALMA Workshop, March 21-22, 2011 . 2. M. min. Prediction (1991) and State of the Art (2009). H.-W. Rix IMPRS Galaxies Course March 11, 2011. Goal:. Determine . n. *. (M. *. ,. t. age. ,[Fe. /H],. R. ). . for a population of galaxies. How many stars of what mass and metallicity . formed when and where in galaxies?. The FDSN and Sustainable Seismic Networks. Gerardo. . Su. árez. Instituto de Geofísica, UNAM. México. Federation of Digital Broad-Band Seismograph Networks. The FDSN: Origins. Founded in 1985 to bring together digital broad-. Hydrogen Gas. AAO. . Colloquium . . 5th February 2015. Philip Lah. Collaborators:. Frank Briggs (ANU. ). Jayaram Chengalur (NCRA) . Matthew Colless (. ANU). Roberto De Propris (FINCA. POWER . RADIO. GALAXIES AS BEACONS FOR CLUSTERS . AT . 1<z<2. Marco Chiaberge. INAF-IRA. Space Telescope Science Institute. A. . Capetti. INAF- OATO. G. Tremblay RIT. P. . Tozzi. INAF-OATS. These are called . active. . galaxies. .. . Active Galaxies and Quasars. By looking far away and back in time, astronomers have discovered:. The origin of active galaxy energy sources and outbursts were closely related to the formation and history of galaxies.. 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..