Einstein observations of the X-ray structure of Centaurus A - Evidence for the radio-lobe energy source

Schreier, E.; Feigelson, E. D.; Delvaille, J. P.; Giacconi, R.; Grindlay, Jonathan E.; Schwartz, D. A.; Fabian, A. C.

doi:10.1086/183105

Cited by 67 publications

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“…2 seem to support the expanding jet model with induced shocks as a method for powering the extended radio source. This model is also supported by evidence of ongoing activity in the nucleus (Kellermann 1974;Morganti et al 1992;Botti et al 1993), and by X-ray, optical and radio observations of the inner jet of the source (Schreier et al 1979;Feigelson et al 1981;Burns et al 1983;Haynes et al 1983;Meier et al 1989). …”

Section: Commentsmentioning

confidence: 66%

The large-scale radio spectral index distribution of Centaurus A

Combi

Romero

1997

Astron. Astrophys. Suppl. Ser.

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Section: Commentsmentioning

confidence: 66%

The large-scale radio spectral index distribution of Centaurus A

Combi

Romero

1997

Astron. Astrophys. Suppl. Ser.

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“…All rights reserved. Printed in U.S.A. Schreier et al 1979;Döbereiner et al 1996;Kraft et al 2001). Feigelson et al (1981) used Einstein HRI data to demonstrate that the X-ray emission arises mostly in a small number of knots that are often spatially coincident with radio knots near the center of the galaxy.…”

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confidence: 99%

ChandraX‐Ray Observations of the Inner Optical Filaments in Centaurus A

Evans

Koratkar

2004

ApJ

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We have obtained Chandra High Resolution Camera (0.1-10 keV) X-ray imaging of the inner optical filaments of Cen A. Faint X-ray emission is observed associated with the filaments with significance levels of 2-3.5 when the data are adaptively smoothed. Comparison with optical [O iii] k5007 emission-line imaging suggests that the X-ray-emitting gas is associated with the northwest edge of the optical line-emitting gas. This region of the filaments is closest to the radio jet and is therefore a candidate for shock heating induced by turbulent instabilities in the interstellar medium. The observed X-ray luminosity is significantly smaller than that predicted by purely radiative shock models of the filaments, implying that mechanical energy input does not provide 100% of the ionizing energy budget for the filaments.

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“…The optical "jet" first described by Blanco et al, 1975, is at a position angle of 58 degrees and a distance of 15 minutes from the center of NGC 5128. It is fairly closely aligned with the "nuclear" X-ray and radio jet which has a length of approxi mately four minutes (Schreier et al, 1979(Schreier et al, , 1981. The faint optical HII regions (25 1 from the nucleus) and the middle radio lobe are more close ly aligned with the well-known inner double radio source at position angle 45 degrees.…”

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confidence: 73%

Emission Regions in Centaurus A

Price¹,

Graham

1982

Symp. - Int. Astron. Union

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Centaurus A, at an estimated distance of five megaparsecs, is the closest radio galaxy. It presents the best opportunity to examine in detail the physical mechanisms and resulting structures that are to be found in radio galaxies. Centaurus was first studied in detail at radio wavelengths by Cooper, Price and Cole (1965), hence CPC. Many of the comments, interpretations, and conclusions recorded in that paper remain valid today and provide the broader framework in which the more detailed studies using today's more powerful instrumentation can be understood. Historically, it is also interesting to note that Centaurus A was the first extragalactic radio source in which linear polarization and Faraday rotation were discovered and extensively studied.

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Einstein observations of the X-ray structure of Centaurus A - Evidence for the radio-lobe energy source

Cited by 67 publications

References 0 publications

The large-scale radio spectral index distribution of Centaurus A

The large-scale radio spectral index distribution of Centaurus A

ChandraX‐Ray Observations of the Inner Optical Filaments in Centaurus A

Emission Regions in Centaurus A

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