'Radio galaxies' diaporamas de présentation

Active Galaxies, Shocks and High Energy Particles

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Universe Eighth Edition

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Radio Astronomy

Radio Astronomy. The 2nd window on the Universe: The atmosphere is transparent in the centimeter & meter bands ?< 5 mm mostly absorbed by molecular bands ?>15 m or so, absorbed or reflected by the ionosphere. Summary History of Radio Astronomy.

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Radio Wavelength Evidence for High Energy Particles in the Nearby Universe

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Active Galactic Nuclei

Active Galactic Nuclei. Questions to be addressed: What are active galactic nuclei (AGN)? What are the main properties of AGN? (3) What is the source of power for AGN?. Observationally,What are AGNs?.

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Radio galaxies in 6dFGS: influence of the supercluster environment ?

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Astrophysical Accelerators of Ultra High Energy Cosmic Rays

Astrophysical Accelerators of Ultra High Energy Cosmic Rays. ? Kyoto U. Susumu Inoue (NAOJ). GRBs. AGNs. clusters. collaborators:. AGNs: H. Takami, T. Yamamoto, K. Sato. GRBs: K. Asano, P. Meszaros. clusters: G. Sigl, F. Miniati, E. Armengaud

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UV/optical properties of z~2.5 RG

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Magnetic fields and particle content in FRII radio sources

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Two distinct Accretion processes in radio galaxies

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Low frequency results from the GMRT and the role of the E-LOFAR

Low frequency results from the GMRT and the role of the E-LOFAR. Dharam Vir Lal (MPIfR, Bonn). Overview. Expectation: as the radio emitting plasma flows away from hot-spots in radio galaxies, it ages;

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Particles and Fields in Lobes of Radio Galaxies

Particles and Fields in Lobes of Radio Galaxies. Naoki Isobe (NASDA, MAXI Mission) Makoto Tashiro (Saitama Univ.) Kazuo Makishima (Univ. of Tokyo) Hidehiro Kaneda, Naoko Iyomoto (ISAS). Jet. Hot Spot. Nucleus. Lobe. time-integrated information on past activities of the jets.

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Thermal blackbody radiation

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FRI RADIO GALAXIES AT z > 1 STUDYING THE BUILDING BLOCKS OF

FRI RADIO GALAXIES AT z > 1 STUDYING THE BUILDING BLOCKS OF TODAY'S MOST MASSIVE GALAXIES AND CLUSTERS Marco Chiaberge Space Telescope Science Institute and INAF-IRA Bologna G. Tremblay (STScI) A. Capetti (INAF-OATO) D. Macchetto (STScI) W.B. Sparks (STScI) P. Tozzi (INAF-OATS).

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Most of the power of ordinary galaxies come from the stars

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Statistical Properties of Radio Galaxies in the local Universe

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Double Trouble: ASKAP Early Science using Radio Galaxies

Double Trouble: ASKAP Early Science using Radio Galaxies. Lawrence Rudnick, University of Minnesota. CR origins in radio galaxies: in the AGN? or in situ ? ( a vs. z) RG environments + small scale Galactic structure. Deep+wideband+polarization. ~30 m Jy,800sq deg 700-1800.

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When Galaxies Collide

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MeV gamma emission from cocoons of young radio galaxies

MeV gamma emission from cocoons of young radio galaxies. Motoki Kino (Osaka Univ.). ~Abstract~

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Brigthest Cluster Galaxies

Brigthest Cluster Galaxies. most luminous most massive extended source. ? cD galaxy - only in clusters - L vs cluster properties also giant E and D galaxy. Unique class of objects. strong offset from FP but little scatter

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