ROSATX‐Ray Observations of Abell Clusters with Wide‐Angle Tailed Radio Sources

1997 ◽  
Vol 474 (2) ◽  
pp. 580-597 ◽  
Author(s):  
P. L. Gomez ◽  
J. Pinkney ◽  
J. O. Burns ◽  
Q. Wang ◽  
F. N. Owen ◽  
...  
Keyword(s):  
Radio Sources ◽  
Wide Angle ◽  
Abell Clusters

Radio Sources with Wide-Angle Tails in Abell Clusters of Galaxies

1976 ◽  
Vol 205 ◽  
pp. L1 ◽  
Author(s):  
Frazer N. Owen ◽  
Lawrence Rudnick
Keyword(s):  
Radio Sources ◽  
Wide Angle ◽  
Clusters Of Galaxies ◽  
Abell Clusters

What Bends Wide-Angle Tailed Radio Sources?

1982 ◽  
pp. 45-46 ◽  
Author(s):  
Jack O. Burns ◽  
Jean A. Eilek ◽  
Frazer N. Owen
Keyword(s):  
Radio Sources ◽  
Wide Angle

scholarly journals Co-Evolution of Brightest Cluster Galaxies and Galaxy Activity in the Host Clusters

2009 ◽  
Vol 5 (S267) ◽  
pp. 110-110
Author(s):  
Mei-Ling Huang ◽  
Lin-wen Chen
Keyword(s):  
Galaxy Clusters ◽  
Radio Galaxy ◽  
Host Galaxy ◽  
Radio Sources ◽  
Wide Angle ◽  
Cluster Galaxies ◽  
Brightest Cluster Galaxies ◽  
Radio Power

AbstractWe have identified ~500 relatively relaxed galaxy clusters at low redshift (z < 0.3) from the maxBCG catalog with double radio lobes at the center; about 200 radio counterparts of brightest cluster galaxies (BCGs) of these clusters appear to be wide-angle tailed (WAT) radio sources, indicating ongoing interaction between its host galaxy and the surrounding ICM. Our analysis suggests that the radio power of WAT is positively correlated with the optical luminosities of host BCGs, and increases with redshift; whereas the cluster ellipticity-radio galaxy fraction relation shows no obvious difference between WAT and non-WAT clusters.

scholarly journals Making Faranoff-Riley I radio sources

2019 ◽  
Vol 621 ◽  
pp. A132 ◽  
Author(s):  
S. Massaglia ◽  
G. Bodo ◽  
P. Rossi ◽  
S. Capetti ◽  
A. Mignone
Keyword(s):  
Low Power ◽  
Constant Pressure ◽  
Three Dimensional ◽  
Stratified Medium ◽  
Radio Sources ◽  
Wide Angle ◽  
Mhd Simulations ◽  
The Universe ◽  
Nonrelativistic Velocity

Radio sources of low power are the most common in the universe. Their jets typically move at nonrelativistic velocity and show plume-like morphologies that in many instances appear distorted and bent. We investigate the role of magnetic field on the propagation and evolution of low-power jets and the connection between the field intensity and the resulting morphology. The problem is addressed by means of three-dimensional magnetohydrodynamic (MHD) simulations. We consider supersonic jets that propagate in a stratified medium. The ambient temperature increases with distance from the jet origin maintaining constant pressure. Jets with low magnetization show an enhanced collimation at small distances with respect to hydrodynamic (HD) cases studied in a previous paper. These jets eventually evolve in a way similar to the HD cases. Jets with higher magnetization are affected by strong nonaxisymmetric modes that lead to the sudden jet energy release. From there on, distorted plumes of jet material move at subsonic velocities. This transition is associated with the formation of structures reminiscent of the “warm spots” observed in wide-angle-tail (WAT) sources.

scholarly journals What Bends Wide-Angle Tailed Radio Sources?

1982 ◽  
Vol 97 ◽  
pp. 45-46
Author(s):  
Jack O. Burns ◽  
Jean A. Eilek ◽  
Frazer N. Owen
Keyword(s):  
Radio Galaxy ◽  
Radio Sources ◽  
Wide Angle ◽  
Velocity Data ◽  
Cluster Galaxy ◽  
Potential Wells ◽  
X Ray ◽  
Ram Pressure ◽  
The Galaxy ◽  
Cd Galaxies

It has been generally assumed that wide-angle tailed (WAT) sources like 3C465 are formed in a manner similar to that of the more strongly bent U-shaped sources such as NGC 1265, i.e., by ram pressure arising from galaxy motion through a dense intracluster medium (ICM). The WAT sources were thought to be less strongly bent because of the smaller ratio of tail plasma flow momentum flux to galaxy velocity. However, as noted recently by Burns (1981), there is a serious discrepancy between the ram pressure model requirements for bending WATs and the dynamics of the associated radio galaxy. To bend the tails, we calculate that the galaxy must typically move at velocities of 0.7–1×103 km s−1 for distances comparable to the length of the radio tails (∼200 kpc for 3C465). This implied galaxy motion is inconsistent with the nature of the massive cD galaxies generally associated with WATs. Cluster galaxy velocity data, X-ray observations, and recent models suggest that these giant galaxies are nearly at rest at the bottoms of cluster potential wells, at most moving ∼200 km s−1 in an oscillatory motion of small amplitude (<0.3 of a core radius, Malumuth, 1981, private communication). Thus it appears that some other mechanism is responsible for bending WAT sources.

Narrow-angle tail radio sources and the distribution of galaxy orbits in Abell clusters

1987 ◽  
Vol 316 ◽  
pp. 113 ◽  
Author(s):  
Christopher P. O'Dea ◽  
Craig L. Sarazin ◽  
Frazer N. Owen
Keyword(s):  
Radio Sources ◽  
Narrow Angle ◽  
Abell Clusters

Radio jet propagation and wide-angle tailed radio sources in merging galaxy cluster environments

1995 ◽  
Vol 445 ◽  
pp. 80 ◽  
Author(s):  
Chris Loken ◽  
Kurt Roettiger ◽  
Jack O. Burns ◽  
Michael Norman
Keyword(s):  
Galaxy Cluster ◽  
Radio Sources ◽  
Wide Angle

scholarly journals Optical Properties of FRI Radio Galaxies

1996 ◽  
Vol 175 ◽  
pp. 238-239
Author(s):  
Michael J. Ledlow ◽  
Frazer N. Owen
Keyword(s):  
Optical Properties ◽  
Flux Density ◽  
Radio Galaxies ◽  
Cluster Center ◽  
Radio Sources ◽  
Complete Sample ◽  
Abell Clusters ◽  
Ccd Observations ◽  
Twin Jets ◽  
Compact Sources

From the VLA 20cm survey of ≃ 500 Abell clusters reported by (Ledlow and Owen, 1995), we have obtained optical R-Band CCD observations and optical spectra for 265 radio galaxies. The survey is complete for 20cm flux density greater than 10 mJy within 0.3 corrected Abell radii of the cluster center. All Abell clusters with measured z < 0.09 were surveyed. This statistically complete sample was supplemented by ≃ 200 clusters with 0.09 < z < 0.25 including sources with flux density > 200 mJy. Only 6% of the sample consists of FR II radio sources, the remainder are twin-jets, tailed, or compact sources associated with the FR I class.

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