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

By M. Hardcastle, D. Worrall, M. Birkinshaw, R. Laing, A. Bridle. 2002

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We have observed the twin-jet radio galaxy 3C 296 with Chandra. X-ray emission is detected from the nucleus, from the inner parts of the radio jet and from a small-scale thermal environment around the jet deceleration region. As we have found in previous observations of other twin-jet radio galaxies, the X-ray jet and a steep pressure gradient in the external thermal environment are associated with the region where strong bulk deceleration of the jet material is suggested by radio observations. Our observations provide additional evidence that the inner jets of twin-jet objects are always associated with a relatively cool, dense central X-ray emitting component with a short cooling time.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5a397eb60775e61f9c735f903dffd5efb692aacc

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Citations in the corpus

Dynamical models for jet deceleration in the radio galaxy 3C 31 (2002, methodology): “…≈ 8.1 × 105 m−3 for an e−p+ jet (note that nrad consistently includes all radiating species).1 Finally, we deduce a lower limit to the magnetic field, B 2.9 × 10−5 T using the X-ray core flux density at 1 keV from Hardcastle et al. (2002) as an upper limit to the synchrotron self-Compton emission.”
Chandra and XMM-Newton Observations of a Sample of Low-Redshift FR I and FR II Radio Galaxy Nuclei (2005, background): “As discussed by Hardcastle et al. (2002), the discrepancy may be resolved by postulating that there exists an additional, unresolved dense component of thermal emission that lies close to the core.”
Relativistic models and the jet velocity field in the radio galaxy 3C 31 (2002, background): “We neglect synchrotron losses, on the grounds that the observed spectrum is a power law with α = 0.55 between 1.4 and 8.4 GHz (and extends to much higher frequencies; Hardcastle et al. 2002).”
Radio galaxies and feedback from AGN jets (2020, background): “Constraints derived from luminosity functions of blazars and their presumed parent population of radio galaxies (Urry et al., 1991; Hardcastle et al., 2002) imply bulk beaming speeds of Γ ∼ 3–5.”
X-Ray Emission from Extragalactic Jets (2006, unknown): “References 1 Kataoka et al. (2003); 2 Worrall, Birkinshaw & Hardcastle (2003); 3 Hardcastle et al. (2002); 4 Worrall, Birkinshaw & Hardcastle (2001); 5 Hardcastle, Birkinshaw & Worrall (2001); 6 Harris, Mossman & Walker (2004); 7 Harris, Krawczynski & Taylor (2002); 8 Birkinshaw, Worrall &…”
The 400 Square Degree ROSAT PSPC Galaxy Cluster Survey: Catalog and Statistical Calibration (2006, result): “Therefore we identify this object as a galaxy group, a conclusion that is confirmed by a Chandra observation of this field (Hardcastle et al. 2002).”
X-Ray Emission from the Hot Interstellar Medium and Southwest Radio Lobe of the Nearby Radio Galaxy Centaurus A (2003, background): “The jet/ lobe morphology of Cen A is clearly different than the ‘‘ tailed twin-jet ’’ morphology (Leahy 1993) commonly associated with objects like 3C 31 (Hardcastle et al. 2002b; Laing & Bridle 2002a, 2002b) and 3C 449 (Feretti et al. 1999).”
Dynamics and high-energy emission of the flaring HST-1 knot in the M 87 jet (2006, background): “…additional central component increases, only slightly, the X-ray surface brightness, in particular by a factor of 2–3 within r p 100 pc. Interestingly, Hardcastle et al. (2002) reported larger, by a factor of 2, number of counts from a thermal X-ray halo surrounding the central regions (r p < 500…”
X-Ray Emission Properties of Large-Scale Jets, Hot Spots, and Lobes in Active Galactic Nuclei (2004, background): “…but the X-ray emissions from the hotspots and radio lobes are also reported in a 1e-mail:kataoka@hp.phys.titech.ac.jp 2e-mail:stawarz@oa.uj.edu.pl number of FR II radio galaxies and quasars (e.g., Wilson, Young & Shopbell 2000; 2001; Hardcastle et al. 2002b; 2004, Tashiro et al. 1998; Isobe 2002).”
A Survey of Extended Radio Jets with Chandra and the Hubble Space Telescope (2004, background): “In addition, Chandra is now showing that the terminal lobes and hot spots in powerful Fanaroff-Riley II (FR II) jets emit at X-ray, although the origin of the X-ray flux from these structures is still a matter of debate (e.g., Hardcastle et al. 2002a).”
Radio and X-Ray Observations of the Jet in Centaurus A (2003, background): “…notable arthe tendency for the inner parts of the jet to have a higher X-ray to radio flux density ratio, and the offsets between the peak positions of X-ray and radio knots, which are typically in the sense that the X-ray knot’s position is closer to the core (Hardcastle et al. 2001, 2002).”
X-Ray Thermal Coronae of Galaxies in Hot Clusters: Ubiquity of Embedded Mini-Cooling Cores (2006, background): “We note that dense coronae have also been found around the nuclei of luminous radio sources in cooler groups or clusters, e.g., 3C 31 (Hardcastle et al. 2002), 3C 296 (Hardcastle et al. 2005), cD galaxies of A160 and A2462 (Jetha et al. 2005).”
Three-dimensional relativistic MHD simulations of active galactic nuclei jets: magnetic kink instability and Fanaroff–Riley dichotomy (2015, background): “Although on average FRII jets are more spatially extended than FRI jets, some FRI jets reach Mpc distances (Hardcastle et al. 2002; Laing et al. 2008).”
The active nuclei of z < 1.0 3CRR radio sources (2009, background): “…absorbing component, presumably related to large-scale dust rings in the host galaxy, is required to allow a good single power-law fit (e.g. Hardcastle et al. 2002; Hardcastle, Sakelliou & Worrall 2005): as this is a rather different situation to genuine nuclear absorption, we do not…”