A Chandra observation of the X-ray environment and jet of 3C 296

Hardcastle, M. J.; Worrall, D. M.; Birkinshaw, Mark; Laing, R. A.; Bridle, A. H.

doi:10.1111/j.1365-2966.2005.08765.x

Cited by 36 publications

(45 citation statements)

References 35 publications

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“…These conditions are very similar to those found in the central components of more normal, non‐WAT FR I radio galaxies hosted by groups (e.g. Hardcastle et al 2002, 2005).…”

Section: Spatial and Spectral Analysissupporting

confidence: 81%

AChandraandXMM-Newtonstudy of the wide-angle tail radio galaxy 3C 465

Hardcastle

Sakelliou

Worrall

2005

Monthly Notices of the Royal Astronomical Society

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We have observed the prototypical wide‐angle tail (WAT) 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 small‐scale, cool component of thermal emission, a number of the individual galaxies of the host cluster (Abell 2634), and the hotter thermal emission from the cluster itself. The X‐ray detection of the jet allows us to argue that synchrotron emission may be an important mechanism in other well‐collimated, fast jets, including those of classical double radio sources. The bases of the radio plumes are not detected in the X‐ray, which supports the model in which these plumes are physically different from the twin jets of lower‐power radio galaxies. The plumes are in fact spatially coincident with deficits of X‐ray emission on large scales, which argues that they contain little thermal material at the cluster temperature, although the minimum pressures throughout the source are lower than the external pressures estimated from the observed thermal emission. Our observations confirm both spatially and spectrally that a component of dense, cool gas with a short cooling time is associated with the central galaxy. However, there is no evidence for the kind of discontinuity in external properties that would be required in many models of the jet–plume transition in WATs. Although the WAT jet–plume transition appears likely to be related to the interface between this central cool component and the hotter intracluster medium, the mechanism for WAT formation remains unclear. We revisit the question of the bending of WAT plumes, and show that the plumes can be bent by plausible bulk motions of the intracluster medium, or by motion of the host galaxy with respect to the cluster, as long as the plumes are light.

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“…These conditions are very similar to those found in the central components of more normal, non‐WAT FR I radio galaxies hosted by groups (e.g. Hardcastle et al 2002, 2005).…”

Section: Spatial and Spectral Analysissupporting

confidence: 81%

AChandraandXMM-Newtonstudy of the wide-angle tail radio galaxy 3C 465

Hardcastle

Sakelliou

Worrall

2005

Monthly Notices of the Royal Astronomical Society

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“…We have repeated this calculation for several other FR I radio galaxies for which both X‐ray estimates of the central density (e.g. 3C 296, Hardcastle et al 2005) and jet power estimates from jet modelling (Laing, private communication) are available, and find that this conclusion is generally true: the central densities in the galaxy‐scale components of these sources, even those in considerably poorer large‐scale environments than 3C 31, are sufficient for Bondi accretion at a nominal 10 per cent efficiency to power the jet.…”

Section: Bondi Accretion and Powerful Radio Sourcesmentioning

confidence: 99%

Hot and cold gas accretion and feedback in radio-loud active galaxies

Hardcastle¹,

Evans²,

Croston³

2007

Monthly Notices of the Royal Astronomical Society

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The definitive version is available at www.blackwell-synergy.com.--Copyright Blackwell Publishing-- --DOI : 10.1111/j.1365-2966.2007.11572.xWe have recently shown that X-ray observations of the population of ???low-excitation??? radio galaxies, which includesmost low-power, Fanaroff-Riley class I sources as well as some more powerful Fanaroff-Riley class II objects, are consistent with a model in which the active nuclei of these objects are not radiatively efficient at any waveband. In another recent paper Allen et al. have shown that Bondi accretion of the hot, X-ray emitting phase of the intergalactic medium (IGM) is sufficient to power the jets of several nearby, low-power radio galaxies at the centres of clusters. In this paper we combine these ideas and suggest that accretion of the hot phase of the IGM is sufficient to power all low-excitation radio sources, while highexcitation sources are powered by accretion of cold gas that is in general unrelated to the hot IGM. This model explains a number of properties of the radio-loud active galaxy population, and has important implications for the energy input of radio-loud active galactic nuclei into the hot phase of the IGM: the energy supply of powerful high-excitation sources does not have a direct connection to the hot phase

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“…X‐ray observations can be used to infer the temperature, density and pressure profiles of the hot gas associated with the host galaxies of FR I radio galaxies (e.g. Hardcastle et al 2002; Worrall, Birkinshaw & Hardcastle 2003; Hardcastle et al 2005). Together with the velocity distributions derived from modelling of the radio emission, these can be used in a conservation‐law analysis (hereafter B94 Bicknell 1994) to derive jet energy fluxes and the variations of mass flux, pressure, internal density and entrainment rate with distance from the nucleus (hereafter LB02b Laing & Bridle 2002b).…”

Section: Introductionmentioning

confidence: 99%

A relativistic mixing-layer model for jets in low-luminosity radio galaxies

Wang

Kaiser

Laing

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We present an analytical model for jets in Fanaroff & Riley Class I (FR I) radio galaxies, in which an initially laminar, relativistic flow is surrounded by a shear layer. We apply the appropriate conservation laws to constrain the jet parameters, starting the model where the radio emission is observed to brighten abruptly. We assume that the laminar flow fills the jet there and that pressure balance with the surroundings is maintained from that point outwards. Entrainment continuously injects new material into the jet and forms a shear layer, which contains material from both the environment and the laminar core. The shear layer expands rapidly with distance until finally the core disappears, and all of the material is mixed into the shear layer. Beyond this point, the shear layer expands in a cone and decelerates smoothly. We apply our model to the well‐observed FR I source 3C 31 and show that there is a self‐consistent solution. We derive the jet power, together with the variations of mass flux and entrainment rate with distance from the nucleus. The predicted variation of bulk velocity with distance in the outer parts of the jets is in good agreement with model fits to Very Large Array observations. Our prediction for the shape of the laminar core can be tested with higher‐resolution imaging.

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A Chandra observation of the X-ray environment and jet of 3C 296

Cited by 36 publications

References 35 publications

AChandraandXMM-Newtonstudy of the wide-angle tail radio galaxy 3C 465

AChandraandXMM-Newtonstudy of the wide-angle tail radio galaxy 3C 465

Hot and cold gas accretion and feedback in radio-loud active galaxies

A relativistic mixing-layer model for jets in low-luminosity radio galaxies

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