The X-ray structure of Centaurus A

Feigelson, E. D.; Schreier, E.; Delvaille, J. P.; Giacconi, R.; Grindlay, J. E.; Lightman, Alan P.

doi:10.1086/159439

Cited by 135 publications

(147 citation statements)

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“…We identify this feature with the elongated, di †use X-ray emission coincident with the NML from 15@ to over 20@ from the nucleus, discovered by Feigelson et al (1981).…”

Section: X-ray Excess Coinciding With the Nmlmentioning

confidence: 60%

“…A trunk of overdense X-rayÈ emitting gas is drawn up from below the bubble, deforming it into a torus. The overdense trunk is identiÐed with the di †use X-ray excess coinciding with the NML discovered by Feigelson et al (1981). Although the ensuing phase of renewed jet activity is not addressed by our simulations, we have suggested that the pressure gradient in the upÑow region beneath the NML drew light radio plasma from the top of the newly forming inner lobe.…”

Section: Discussionmentioning

confidence: 76%

“…However, the ratio of the trunk to ambient densities, as calculated above from the observations of Feigelson et al (1981), Forman et al (1985), and Schreier et al (1981), is D7. We note, however, that in Feigelson et al (1981) the data were not presented in such a way as to facilitate an independent estimate of the trunk density ; the density of the background medium is an extrapolation. Further, high-resolution Chandra observations are required for a deÐnitive assessment.…”

Section: X-ray Excess Coinciding With the Nmlmentioning

confidence: 87%

“…Near the brightest part of the NML, Feigelson et al (1981) detected di †use soft X-ray emission from a region extending 1 kpc wide and a projected height of 5 kpc in the direction away from the galaxy. By their interpretation, if the X-rayÈemitting region is composed of thermal gas at temperatures D106 K compressed from the surrounding medium, then it must be ephemeral, with timescales of D10 and D1 Myr for cooling and dynamical expansion, respectively.…”

Section: Previous Observationsmentioning

confidence: 99%

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The Centaurus A Northern Middle Lobe as a Buoyant Bubble

Saxton

Sutherland

Bicknell

2001

ApJ

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We model the northern middle radio lobe of Centaurus A (NGC 5128) as a buoyant bubble of plasma deposited by an intermittently active jet. The extent of the rise of the bubble and its morphology imply that the ratio of its density to that of the surrounding ISM is less than 10~2, consistent with our knowledge of extragalactic jets and minimal entrainment into the precursor radio lobe. Using the morphology of the lobe to date the beginning of its rise through the atmosphere of Cen A, we conclude that the bubble has been rising for approximately 140 Myr. This timescale is consistent with that proposed by Quillen and coworkers for the settling of postmerger gas into the presently observed large-scale disk in NGC 5128, suggesting a strong connection between the delayed reestablishment of radio emission and the merger of NGC 5128 with a small gas-rich galaxy. This suggests a connection, for radio galaxies in general, between mergers and the delayed onset of radio emission. In our model, the elongated X-ray emission region discovered by Feigelson and coworkers, part of which coincides with the northern middle lobe, is thermal gas that originates from the interstellar medium below the bubble and that has been uplifted and compressed. The "" large-scale jet ÏÏ appearing in the radio images of Morganti and coworkers may be the result of the same pressure gradients that cause the uplift of the thermal gas, acting on much lighter plasma, or may represent a jet that did not turn o † completely when the northern middle lobe started to buoyantly rise. We propose that the adjacent emission-line knots (the "" outer Ðlaments ÏÏ) and star-forming regions result from the disturbance, in particular the thermal trunk, caused by the bubble moving through the extended atmosphere of NGC 5128.

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“…We identify this feature with the elongated, di †use X-ray emission coincident with the NML from 15@ to over 20@ from the nucleus, discovered by Feigelson et al (1981).…”

Section: X-ray Excess Coinciding With the Nmlmentioning

confidence: 60%

Section: Discussionmentioning

confidence: 76%

Section: X-ray Excess Coinciding With the Nmlmentioning

confidence: 87%

Section: Previous Observationsmentioning

confidence: 99%

See 2 more Smart Citations

The Centaurus A Northern Middle Lobe as a Buoyant Bubble

Saxton

Sutherland

Bicknell

2001

ApJ

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“…The spatial resolution of the Einstein HRI and ROSAT HRI instruments allowed X-ray jets to be found in Centaurus A (Feigelson et al 1981), M87 (Schreier, Gorenstein & Felgelson 1982), 3C120 (Harris et al 1999) and 3C273 (Willingale 1981). Chandra's sensitivity and arcsecond spatial resolution truly opened the study of extragalactic X-ray jets.…”

Section: Introductionmentioning

confidence: 99%

X-ray jets and nuclear emission in low redshift early-type galaxies

Jones¹,

Forman²,

Churazov

et al. 2014

Proc. IAU

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Abstract. Due to its high angular resolution, the Chandra Observatory has allowed the discovery and detailed study of extragalactic X-ray jets. Although supermassive black holes are regularly found in the cores of massive galaxies and X-ray emission is detected from ∼80% of these, X-ray and radio jets are only detected in a small fraction of "normal" galaxies. X-ray jets are either single-sided or double-sided and, with only one possible exception, are found to have radio emission. However many radio jets are not detected in current X-ray observations. The expanding jets produce cavities in the surrounding hot gas in the galaxy halos. By determining how much gas has been pushed out of these cavities, we can determine the mechanical energy and power of the jet.

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Non-Thermal Emission from Extragalactic Radio Sources: A High Resolution - Broad Band Approach

Brunetti

2004

The Role of VLBI in Astrophysics, Astrometry and Geodesy

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In the framework of the study of extragalactic radio sources, we will focus on the importance of the spatial resolution at different wavelengths, and of the combination of observations at different frequency bands. In particular, a substantial step forward in this field is now provided by the new generation X-ray telescopes which are able to image radio sources in between 0.1-10 keV with a spatial resolution comparable with that of the radio telescopes (VLA) and of the optical telescopes. After a brief description of some basic aspects of acceleration mechanisms and of the radiative processes at work in the extragalactic radio sources, we will focus on a number of recent radio, optical and X-ray observations with arcsec resolution, and discuss the deriving constraints on the physics of these sources.

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The X-ray structure of Centaurus A

Cited by 135 publications

References 0 publications

The Centaurus A Northern Middle Lobe as a Buoyant Bubble

The Centaurus A Northern Middle Lobe as a Buoyant Bubble

X-ray jets and nuclear emission in low redshift early-type galaxies

Non-Thermal Emission from Extragalactic Radio Sources: A High Resolution - Broad Band Approach

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