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For refcode 1990MNRAS.246..477P:
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Copyright by Royal Astronomical Society. 1990MNRAS.246..477P The radio structure of NGC 1275 A. Pedlar, H. S. Ghataure, R. D. Davies and B. A. Harrison Nuffield Radio Astronomy Laboraiories, Jodrell Bank, Macclesfeld, Cheshire SK11 9DL R. Perley and P. C. Crane National Radio Astronomy Observatory, Socorro, NM 87801, USA, S. W. Unger Royal Greenwich Observatory, Herstmonceux Castle, Hailsham, Sussex BN27 1RP Accepted 1990 April 24. Received 1990 April 20; in original form 1990 March 16. SUMMARY We present high dynamic range VLA and MERLIN images of NGC 1275 at wavelengths of 18, 22, 90 and 199 cm with angular resolutions ranging from 0.3 to 40 arcsec. Over the central 30 arcsec there is evidence for collimated ejection mainly in PA 160^deg^. Outside this region the radio structure shows evidence of a sharp change in direction to approximately PA 235^deg^, before merging into the 10-arcmin radio halo. On arcsec and arcmin angular scales, there is considerable asymmetry between the structure north and south of the active nucleus. We consider the radio source structure to be consistent with an asymmetrical Fanaroff-Riley type I source, with the jet collimation axis close to the line-of-sight. The radio 'halo' consists of the outer lobes of this structure. Apart from the unresolved core, we see little change in spectral index across the central arcminute between 199, 90 and 22 cm, and no unambiguous evidence for free-free absorption by ionized gas in the system. The collimation axis of the radio jet is approximately perpendicular to the major axes of the integrated optical line emission from both the low- and high-velocity optical systems. We consider the possibility that the high-velocity system is interacting with the collimated outflow from the nucleus, and propose that this could account for some of the unusual optical and radio properties of this source. Similarities are noted between the high-velocity system and Minkowski's object, which also appears to contain a cloud interacting with a radio jet. The total energy of relativistic particles in the radio halo could be as high as ~10^59^ erg (assuming the ratio of relativistic protons to electrons to be 100). Hence, if the age of the radio halo/lobes is ~10^8^ yr, this implies a lower limit to the average energy input to relativistic particles in the halo of 104~ erg s-1. Thus, unless the process by which relativistic particles are accelerated is remarkably efficient, a similar amount of energy will be deposited as heat into the central part of the cluster. This quantity is comparable to the X-ray luminosity over the central region of the cluster ( ~10^44^ erg s^-1^), and its effects should be considered in models of cooling inflows in the central parts of the Perseus cluster.
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