A [ITAL]Chandra[/ITAL] High-Resolution X-ray Image of Centaurus A

Kraft, Ralph; Forman, W.; Jones, Christine; Kenter, A.; Murray, Stephen S.; Aldcroft, Thomas L.; Elvis, M.; Evans, I. N.; Fabbiano, G.; Isobe, Takashi; Jerius, D.; Karovska, M.; Kim, D.-W.; Prestwich, Andrea; Primini, F. A.; Schwartz, D. A.; Schreier, E.; Vikhlinin, A.

doi:10.1086/312519

Cited by 76 publications

(45 citation statements)

References 27 publications

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“…CenA is known to show a complex morphology in X-rays as seen with Einstein, ROSAT, and Chandra (Feigelson et al 1981;Turner et al 1997;Kraft et al 2000Kraft et al , 2002Evans et al 2004). In addition to an extended X-ray jet and point sources in the host galaxy, the AGN is surrounded by faint diffuse emission, extending about 1 ¢ (≈1 kpc) around the core.…”

Section: Appendix the Diffuse Emission As Seen With Chandramentioning

confidence: 98%

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NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X-RAY SPECTRUM OF CENTAURUS A

Fürst

Müller

Madsen

et al. 2016

ApJ

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We present simultaneous XMM-Newton and Nuclear Spectroscopic Telescope Array (NuSTAR) observations spanning 3-78 keV of the nearest radio galaxy, CentaurusA (Cen A). The accretion geometry around the central engine in CenA is still debated, and we investigate possible configurations using detailed X-ray spectral modeling. NuSTAR imaged the central region of CenA with subarcminute resolution at X-ray energies above 10 keV for the first time, but found no evidence for an extended source or other off-nuclear point sources. The XMM-Newton and NuSTAR spectra agree well and can be described with an absorbed power law with a photon index Γ=1.815±0.005 and a fluorescent Fe Ka line in good agreement with literature values. The spectrum does not require a high-energy exponential rollover, with a constraint of E fold >1 MeV. A thermal Comptonization continuum describes the data well, with parameters that agree with values measured by INTEGRAL, in particular an electron temperature kT e between ≈100-300 keV and seed photon input temperatures between 5 and 50 eV. We do not find evidence for reflection or a broad iron line and put stringent upper limits of R<0.01 on the reflection fraction and accretion disk illumination. We use archival Chandra data to estimate the contribution from diffuse emission, extra-nuclear point sources, and the outer X-ray jet to the observed NuSTAR and XMM-Newton X-ray spectra and find the contribution to be negligible. We discuss different scenarios for the physical origin of the observed hard X-ray spectrum and conclude that the inner disk is replaced by an advection-dominated accretion flow or that the X-rays are dominated by synchrotron self-Compton emission from the inner regions of the radio jet or a combination thereof.

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Section: Appendix the Diffuse Emission As Seen With Chandramentioning

confidence: 98%

“…The PSF smears out the very bright core over most of the bright jet emission. When summing up the counts observed by Chandra in knots AX and BX, as described by Kraft et al (2000), we would expect a count rate of ≈5×10 −3 counts s…”

Section: Imagingmentioning

confidence: 99%

NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X-RAY SPECTRUM OF CENTAURUS A

Fürst

Müller

Madsen

et al. 2016

ApJ

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“…Its popularity is not only due to its brightness, but also to its many unusual features: (i) there is a prominent dust band containing young stars and Hii regions (Unger et al 2000;Wild & Eckart 2000;Graham 1979); (ii) there is an active nucleus with a radio and X-ray jet, radio lobes and optical filaments (Cooper et al 1965;Feigelson et al 1981;Kraft et al 2000;Schreier et al 1981;Clarke et al 1992;Blanco et al 1975;Dufour & van den Bergh 1978); (iii) Malin et al (1983) discovered a large number of faint narrow shells of stars surrounding the galaxy; (iv) Schiminovich et al (1994) detected 4 × 10 8 M of Hi gas associated with the stellar shells, but slightly displaced outside the shells; and (v) most recently, molecular CO gas has been found associated with the Hi gas and the stellar shells (Charmandaris et al 2000). All of these are clear indications of a recent interaction with a gas-rich galaxy.…”

Section: Introductionmentioning

confidence: 99%

Stellar populations in NGC 5128 with the VLT: Evidence for recent star formation

Rejkuba

Minniti²,

Silva

et al. 2001

A&A

107

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Abstract. We resolve stars of the nearest giant elliptical galaxy NGC 5128 using VLT with FORS1 and ISAAC. We construct deep U , V and Ks color-magnitude and color-color diagrams in two different halo fields (in the halo and in the north-eastern diffuse shell). In the outer, shell field, at ∼14 kpc from the center of the galaxy, there is a significant recent star formation with stars as young as 10 Myr, approximately aligned with the prominent radio and X-ray jet from the nucleus of the host AGN. Ionized gas filaments are evident in ultraviolet images near the area where neutral Hi and CO molecular gas was previously observed. The underlying stellar population of the halo of the giant elliptical is predominantly old with a very broad metallicity distribution. The presence of an extended giant branch reaching M bol = −5 mag suggests the existence of a significant intermediate-age AGB population in the halo of this galaxy.

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“…(1) ROSAT HRI, Döbereiner et al (1996); (2) Chandra, Kraft et al (2000); (3) the galaxies and fills large parts of the galaxy halos, as e.g. the plume and outer halo emission in NGC 253 (Pietsch et al 2000) or the nuclear superbubble and halo emission of NGC 3079 (Pietsch et al 1998) show.…”

Section: Discussionmentioning

confidence: 99%

A possible X-ray jet from the starburst galaxy NGC 6217

Pietsch

Arp

2001

A&A

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Abstract. Deep ROSAT PSPC and HRI observations of the nuclear starburst, UV flat spectrum spiral NGC 6217 reveal a jet-like X-ray filament extending out 2. 7 (18.8 kpc) to the SW of the galaxy. Radio images of NGC 6217 show an extent in the same direction, giving further evidence for a one-sided X-ray jet interpretation of this feature. Its X-ray spectrum is harder than that of NGC 6217 and the luminosity in the 0.5-2.0 keV band is ∼1.7 ×10 39 erg s −1 . We compare our findings to parameters of other X-ray jets from other active galaxies. We also give positions of a total of 91 X-ray sources detected in the field to a limiting 0.5-2.0 keV flux of ∼2.2 ×10 −15 erg cm −2 s −1 and propose optical and radio identifications. Some of these sources have been identified in the RIXOS program.

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A [ITAL]Chandra[/ITAL] High-Resolution X-ray Image of Centaurus A

Cited by 76 publications

References 27 publications

NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X-RAY SPECTRUM OF CENTAURUS A

NuSTAR AND XMM-NEWTON OBSERVATIONS OF THE HARD X-RAY SPECTRUM OF CENTAURUS A

Stellar populations in NGC 5128 with the VLT: Evidence for recent star formation

A possible X-ray jet from the starburst galaxy NGC 6217

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