Jets, plumes and hotspots in the wide-angle tail source 3C 130

  title={Jets, plumes and hotspots in the wide-angle tail source 3C 130},
  author={Martin J. Hardcastle},
  journal={Monthly Notices of the Royal Astronomical Society},
  • M. Hardcastle
  • Published 24 March 1998
  • Physics
  • Monthly Notices of the Royal Astronomical Society
I present 1.5- and 8.4-GHz observations with all configurations of the NRAO VLA of the wide-angle tail source 3C130. The source has a pair of relatively symmetrical, wellcollimated inner jets, one of which terminates in a compact hot spot. Archival ROSAT PSPC data confirm that 3C130’s environment is a luminous cluster with little sign of sub-structure in the X-ray-emitting plasma. I compare the source to other wide-angle tail objects and discuss the properties of the class as a whole. None of… 

Figures and Tables from this paper

Jet termination in wide-angle tail radio sources
Wide-angle tail radio galaxies (WATs) are an uncommon class of radio sources with luminosities near the FRI/FRII break, and are usually associated with central cluster galaxies. Their defining
A high-resolution view of the jets in 3C 465
We present new high-resolution and high-sensitivity studies of the jets in the WAT source 3C 465, using deep transverse-resolved radio observations from e-MERLIN, and with complementary
We present a Chandra X-ray observation and Very Large Array radio observations of the nearby (z = 0.11) galaxy cluster A562 and the wide angle tail (WAT) radio source 0647+693. The cluster displays
A Chandra and XMM–Newton study of the wide‐angle tail radio galaxy 3C 465
We have observed the prototypical wide-angle tail radio galaxy 3C 465 with Chandra and XMM-Newton. X-ray emission is detected from the active nucleus and the inner radio jet, as well as a
The Dynamics of the Wide-angle Tailed (WAT) Galaxy Cluster A562
We present the first in-depth dynamical analysis of the archetypal wide-angle tailed (WAT) cluster A562. We have combined Gemini observations with archival data from the literature to form a sample
Numerical simulations of colliding jets in an external wind: application to 3C 75
The radio galaxy 3C 75 is remarkable because it contains a pair of radio-loud active galaxies, each of which produces a two-sided jet, with the jet beams appearing to collide and merge to the west
Interactions of radio galaxies and the intracluster medium in Abell 160 and Abell 2462
We present Chandraand VLA observations of two galaxy clusters, Abell 160 and Abell 2462, whose brightest cluster galaxies (BCGs) host wide angle tailed radio galaxies (WATs). We search for evidence
The Fanaroff-Riley transition and the optical luminosity of the host elliptical galaxy
We show that a model for radio source dynamics we had earlier proposed can readily reproduce the relationship between the radio power division separating the two Fanaroff-Riley classes of
3C 40 in Abell 194: can tail radio galaxies exist in a quiescent cluster?
The nearby cluster Abell 194 hosts two luminous, distorted radio galaxies. Both reside within the cluster’s core region, being separated in projec tion by only 100 kpc. It is often suggested that
GMRT detection of a New Wide-Angle Tail (WAT) radio source associated with the galaxy PGC 1519010
We report the serendipitous detection of a Wide-Angle Tail (WAT) radio galaxy at 240 and 610 MHz, using the Giant Metrewave Radio Telescope (GMRT). This WAT is hosted by a cD galaxy PGC 1519010 whose


Beams and jets in astrophysics
1. Introduction: synchrotron and inverse-Compton radiation P. A. Hughes and L. Miller 2. Observations of large scale extragalactic jets T. W. B. Muxlow and S. T. Garrington 3. Interpretation of large
Energy Transport in Radio Galaxies and Quasars
Burns J.O
  • Burns J.O
MPE/OGIP Calibration Memo
  • 1995
MPE/OGIP Calibration Memo CAL/ROS/93-015, version
  • 1995
Extragalactic Radio Sources, IAU Symposium 97
  • Extragalactic Radio Sources, IAU Symposium 97
  • 1982
This paper has been produced using the Royal Astronomical Society/Blackwell Science L A T E X style file
  • This paper has been produced using the Royal Astronomical Society/Blackwell Science L A T E X style file