Results 211 to 220 of about 132,038 (243)

Extended radio sources and elliptical galaxies. II. A search for radio cores using the VLA.

, 1978
E. B. Fomalont, A. H. Bridle
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Low Frequency Radio Observations of the Andromeda Galaxy

, 1972
J. M. Durdin, Yervant Terzian
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High-velocity gas in the jet in the radio galaxy DA 240

, 1978
E. M. Burbidge, G. R. Burbidge, H. E. Smith   +2 more
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Observations at wavelengths of 2.2 and 4.5 centimeters of the linear polarization of radio galaxies and quasars

, 1974
J. P. Vallée, P. P. Kronberg
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Radio galaxies in the coma cluster. II

, 1977
W. G. Tift, M. Tarenghi
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Radio Observations of Galaxies

The Astrophysical Journal, 1967
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Radio Galaxies and Quasars [PDF]

Annals of the New York Academy of Sciences, 1974
The discrete sources of radio emission were first distinguished from the general background radiation during the 1940’s as a result of their rapid amplitude scintillations ; and initially, it was thought that the scintillations were due to fluctuations in the intrinsic intensity of the discrete sources. Assuming that the dimensions of the sources could
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Radio Galaxies and Their Environment [PDF]

, 2002
In this paper we review the properties of radio galaxies in connection to the effect of the dynamic gaseous environment inside clusters in which they are embedded. The external gas can interact with a radio source in different ways: modifying its morphology via ram-pressure, confining the radio lobes, possibly feeding the active nucleus, enhancing star
Tiziana Venturi, Luigina Feretti
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Radio Galaxies and Quasars in Clusters of Galaxies

Publications of the Astronomical Society of Australia, 1983
The study of radio galaxies situated within clusters of galaxies has become a broad field, with hundreds of papers published in the last few years. This review will therefore be restricted mainly to consideration of the interactions between the extended components of radio sources in clusters and the diffuse gas (intracluster medium, ICM) which occurs ...
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Galaxy Interactions and the Radio Galaxy Phenomenon

1990
We have been studying powerful radio galaxies (which we define as having radio power at 178MHz, P 178 ≥ 5xl024 Watts/Hz for a cosmology of H o = 100 km sec-1 Mpc-1 and q o = 0) in order to determine their origins. There are two distinct classes of powerful radio galaxies (PRGs), the so called class A and B radio galaxies (Hine and Longair 1979; Heckman
T. M. Heckman, E. P. Smith
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