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Low Luminosity Radio Galaxies

Published online by Cambridge University Press:  25 May 2016

P. Parma ,
H.R. DE RUITER  and
R. Fanti
P. Parma
Affiliation:
Istituto di Radioastronomia del CNR via Gobetti, 101, 40129 Bologna Osservatorio Astronomico di Bologna via Zamboni, 33, 40126 Bologna
H.R. DE RUITER
Affiliation:
Istituto di Radioastronomia del CNR via Gobetti, 101, 40129 Bologna Osservatorio Astronomico di Bologna via Zamboni, 33, 40126 Bologna
R. Fanti
Affiliation:
Istituto di Radioastronomia del CNR via Gobetti, 101, 40129 Bologna Osservatorio Astronomico di Bologna via Zamboni, 33, 40126 Bologna

Extract

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This review talk will deal almost exclusively with the radio aspects of low luminosity radio galaxies, as the other wavelength bands (optical, X, IR) are covered by others during this conference. By low radio luminosity we mean a radio power at 20 cm in the range 1019 to 1024,5 W Hz–1 (Hubble constant of 100, as throughout this talk). At the upper limit occurs the “break” in the radio luminosity (RLF) (Auriemma et al 1977) as well as the transition from Fanaroff -Riley type I to type II (Fanaroff & Riley, 1974). This limitation to weak radio powers does not necessarily imply that such radio sources constitute a homogeneous class of objects; it has been shown by Wrobel & Heeschen (1991) that a number of radio galaxies of very low luminosity have a ratio between far-infrared and radio emission similar to spiral galaxies and this might suggest that these objects are powered by star formation phenomena. Long baseline interferometry is able to pinpoint compact radio nuclei and therefore can distinguish starburst related radio sources from those powered by nuclear activity (see Slee et al 1994).

Type
Properties of Radio Sources
Information
Symposium - International Astronomical Union , Volume 175: Extragalactic Radio Sources , 1996 , pp. 137 - 142
Copyright
Copyright © Kluwer 1996 

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