Observations of the Structure of Radio Sources in the 3C Catalogue--I

Macdonald, G. H.; Kenderdine, S.; Neville, Ann C.

doi:10.1093/mnras/138.3.259

Cited by 103 publications

(29 citation statements)

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“…Because the Compton/synchrotron mechanism has more time to act on the electrons in these inner components_ their radio spectrum is expected to be steeper than that of the outer lobes. This prediction is in accord with the finding of Macdonald et al (1968) that the emission from between the main components has a steeper spectrum than the source as a whole.…”

Section: • the Supercoherent Modesupporting

confidence: 92%

The effect of adiabatic focusing upon charged-particle propagation in random magnetic fields

Earl¹

1976

ApJ

152

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Section: • the Supercoherent Modesupporting

confidence: 92%

The effect of adiabatic focusing upon charged-particle propagation in random magnetic fields

Earl¹

1976

ApJ

152

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“…The C-band map of Giovannini et al (1988) shows two typical lobes. The source is not resolved in the only L-band map available (Macdonald, Kenderdine, & Neville 1968).…”

Section: Comments On Individual Sourcesmentioning

confidence: 99%

A Study of 3CR Radio Galaxies from [ITAL][CLC]z[/CLC][/ITAL] = 0.15 to [ITAL][CLC]z[/CLC][/ITAL] = 0.65. II. Evidence for an Evolving Radio Structure

Harvanek

Stocke

2002

The Astronomical Journal

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Radio morphology data have been collected for a sample of radio galaxies from the Revised Third Cambridge Catalog in the redshift range 0.15 < z < 0.65. Radio structure parameters including largest physical size, projected bending angle ( ), lobe length asymmetry (Q), and hot spot placement (Fanaroff-Riley ratio) have been measured from the highest-quality radio maps available. Combined with similar data for quasars in the same redshift range, these morphology data are used in conjunction with a quantification of the richness of the cluster environment around these objects (the amplitude of the galaxy-galaxy spatial covariance function, B gg ) to search for indirect evidence of a dense intracluster medium (ICM). This is accomplished by searching for confinement and distortions of the radio structure that are correlated with B gg . Correlations between physical size and hot spot placement with B gg show evidence for an ICM only at z 0.4, but there are no correlations at z ! 0.4, suggesting an epoch of z $ 0.4 for the formation of the ICM in these Abell richness class 0-1, FR2-selected clusters. X-ray-selected clusters at comparable redshifts, which contain FR1 type sources exclusively, are demonstrably richer than the FR2-selected clusters found in this study. The majority of the radio sources with high B gg values at z 0.4 can be described as '' fat doubles '' or intermediate FR2-FR1s. The lack of correlation between B gg and or B gg and Q suggests that these types of radio source distortion are caused by something other than interaction with a dense ICM. Therefore, a large cannot be used as an unambiguous indicator of a rich cluster around powerful radio sources. These results support the hypothesis made in our earlier paper that cluster quasars fade to become FR2s, then FR1s, on a timescale of 0.9 Gyr (for H 0 = 50 km s À1 Mpc À1 ).

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“…An extensive study of 3C sources [14] with the 1 mile telescope confirmed the existence of double structures, though more complex structures were also found, as was also found by the Green Bank Interferometer [15]. A major breakthrough occurred in the early 1970s, when the Cambridge 5-km telescope was built.…”

Section: Aperture Synthesis Imagingmentioning

confidence: 66%

An Old Fogey’s History of Radio Jets

Spencer

2017

Galaxies

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This paper describes a personal view of the discovery of radio jets in celestial radio sources. The existence of narrow, collimated optical features in distant objects has been known about since the early 20th century; however, the advent of radio astronomy in the 1940s and 1950s revealed the existence of a large number of discrete radio sources. The realization that many of these objects were not primarily stellar or local to our own galaxy, but rather extragalactic, followed the determination of accurate radio positions, enabling identifications with optical objects. High-resolution radio interferometers found that they were often compact, and with a double lobed structure, implying outflow from a central object. Shortly afterwards, accurate techniques for the measurement of polarization were developed. However it was not until the advent of synthesis instruments in the 1970s that radio images of the sources were produced, and the existence of radio jets firmly established and their polarization characteristics found.

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Observations of the Structure of Radio Sources in the 3C Catalogue--I

Cited by 103 publications

References 0 publications

The effect of adiabatic focusing upon charged-particle propagation in random magnetic fields

The effect of adiabatic focusing upon charged-particle propagation in random magnetic fields

A Study of 3CR Radio Galaxies from [ITAL][CLC]z[/CLC][/ITAL] = 0.15 to [ITAL][CLC]z[/CLC][/ITAL] = 0.65. II. Evidence for an Evolving Radio Structure

An Old Fogey’s History of Radio Jets

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