The Spectacular Radio-Near-Ir-X-Ray Jet of 3c 111: The X-Ray Emission Mechanism and Jet Kinematics

Clautice, Devon; Perlman, Eric S.; Georganopoulos, Markos; Lister, M. L.; Tombesi, Francesco; Cara, Mihai; Marshall, Herman L.; Hogan, Brandon M.; Kazanas, D.

doi:10.3847/0004-637x/826/2/109

Cited by 25 publications

(20 citation statements)

References 53 publications

(50 reference statements)

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“…We can also observe many features of the jet beams: in run 0000, the beams of the youngest jet and its recollimation shocks are the brightest features, standing out for about 50 kpc in both directions. The recollimation shocks appear brighter than the terminal shocks, similar to what was recently observed by Clautice et al (2016) in the (rather favourable) case of 3C 111. Run 0030 is offering perhaps the most interesting insight on the jet kinematics, as the beam is clearly seen to bend at the hot spots in a centrally symmetric S-shape.…”

Section: Zoom-in X-ray and Projection Effectssupporting

confidence: 87%

Feedback from reorienting AGN jets

Cielo

Babul

Antonuccio-Delogu

et al. 2018

A&A

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Aims. We test the effects of re-orienting jets from an active galactic nucleus (AGN) on the intracluster medium in a galaxy cluster environment with short central cooling time. We investigate both the appearance and the properties of the resulting cavities, and the efficiency of the jets in providing near-isotropic heating to the cooling cluster core. Methods. We use numerical simulations to explore four models of AGN jets over several active/inactive cycles. We keep the jet power and duration fixed across the models, varying only the jet re-orientation angle prescription. We track the total energy of the intracluster medium (ICM) in the cluster core over time, and the fraction of the jet energy transferred to the ICM. We pay particular attention to where the energy is deposited. We also generate synthetic X-ray images of the simulated cluster and compare them qualitatively to actual observations. Results. Jets whose re-orientation is minimal (≲20°) typically produce conical structures of interconnected cavities, with the opening angle of the cones being ~15–20°, extending to ~300 kpc from the cluster centre. Such jets transfer about 60% of their energy to the ICM, yet they are not very efficient at heating the cluster core, and even less efficient at heating it isotropically, because the jet energy is deposited further out. Jets that re-orientate by ≳20° generally produce multiple pairs of detached cavities. Although smaller, these cavities are inflated within the central 50 kpc and are more isotropically distributed, resulting in more effective heating of the core. Such jets, over hundreds of millions of years, can deposit up to 80% of their energy precisely where it is required. Consequently, these models come the closest in terms of approaching a heating/cooling balance and mitigating runaway cooling of the cluster core even though all models have identical jet power/duration profiles. Additionally, the corresponding synthetic X-ray images exhibit structures and features closely resembling those seen in real cool-core clusters.

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Section: Zoom-in X-ray and Projection Effectssupporting

confidence: 87%

Feedback from reorienting AGN jets

Cielo

Babul

Antonuccio-Delogu

et al. 2018

A&A

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“…The possibility that the electrons are scattering CMB photons has been suggested, but this requires high bulk Lorentz factors and angles close to the line of sight. A comprehensive discussion of this problem and its possible solutions has been given by Georganopoulos et al (2016).…”

Section: Oir Uv and X-ray Observationsmentioning

confidence: 99%

Relativistic Jets from Active Galactic Nuclei

Blandford

Meier

Readhead

2019

Annu. Rev. Astron. Astrophys.

644

466

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The nuclei of most normal galaxies contain supermassive black holes, which can accrete gas through a disk and become active. These active galactic nuclei (AGNs) can form jets that are observed on scales from astronomical units to megaparsecs and from meter wavelengths to TeV energies. High-resolution radio imaging and multiwavelength/messenger campaigns are elucidating the conditions under which this happens. Evidence is presented that: ▪ Relativistic AGN jets are formed when the black hole spins and the the accretion disk is strongly magnetized, perhaps on account of gas accreting at high latitude beyond the black hole sphere of influence. ▪ AGN jets are collimated close to the black hole by magnetic stress associated with a disk wind. ▪ Higher-power jets can emerge from their galactic nuclei in a relativistic, supersonic, and proton-dominated state, and they terminate in strong, hot spot shocks; lower-power jets are degraded to buoyant plumes and bubbles. ▪ Jets may accelerate protons to EeV energies, which contribute to the cosmic ray spectrum and may initiate pair cascades that can efficiently radiate synchrotron γ-rays. ▪ Jets were far more common when the Universe was a few billion years old and black holes and massive galaxies were growing rapidly. ▪ Jets can have a major influence on their environments, stimulating and limiting the growth of galaxies. The observational prospects for securing our understanding of AGN jets are bright.

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“…Spectral features indicating reflection from the inner accretion disk and the parsec scale torus or broad line region have been reported in several radio galaxies as well (e.g., Kataoka et al 2007;Sambruna et al 2009;Tombesi et al 2013b;Tazaki et al 2013;Bostrom et al 2014;Lohfink et al 2015). Indeed, the presence of signatures of the accretion disk, winds, and jets in the composite broad-band spectra of broad-line radio galaxies (BLRGs) make them the ideal objects to study the interplay among these components (e.g., Marscher et al 2002;Chatterjee et al 2009Chatterjee et al , 2011Tombesi et al , 2012Tombesi et al , 2013bLohfink et al 2013;Fukumura et al 2014;Clautice et al 2016).…”

Section: Introductionmentioning

confidence: 97%

Feeding and Feedback in the Powerful Radio Galaxy 3C 120

Tombesi

Mushotzky

Reynolds

et al. 2017

ApJ

Self Cite

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We present the spectral analysis of a 200 ks observation of the broad-line radio galaxy 3C 120 performed with the high energy transmission grating (HETG) spectrometer on board the Chandra X-ray Observatory. We find (i) a neutral absorption component intrinsic to the source with column density of logN H = 20.67 ± 0.05 cm −2 , (ii) no evidence for a warm absorber with an upper limit on the column density of just logN H < 19.7 cm −2 assuming the typical ionization parameter logξ≃2.5 erg s −1 cm, the warm absorber may instead be replaced by (iii) a hot emitting gas with temperature kT ≃ 0.7 keV observed as soft X-ray emission from ionized Fe L-shell lines which may originate from a kpc scale shocked bubble inflated by the AGN wind or jet with a shock velocity of about 1,000 km s −1 determined by the emission line width, (iv) a neutral Fe Kα line and accompanying emission lines indicative of a Compton-thick cold reflector with low reflection fraction R ≃ 0.2, suggesting a large opening angle of the torus, (v) a highly ionized Fe XXV emission feature indicative of photoionized gas with ionization parameter logξ=3.75 +0.27 −0.38 erg s −1 cm and a column density of logN H > 22 cm −2 localized within ∼2 pc from the X-ray source, and (vi) possible signatures for a highly ionized disk wind. Together with previous evidence for intense molecular line emission, these results indicate that 3C 120 is likely a late state merger undergoing strong AGN feedback.

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The Spectacular Radio-Near-Ir-X-Ray Jet of 3c 111: The X-Ray Emission Mechanism and Jet Kinematics

Cited by 25 publications

References 53 publications

Feedback from reorienting AGN jets

Feedback from reorienting AGN jets

Relativistic Jets from Active Galactic Nuclei

Feeding and Feedback in the Powerful Radio Galaxy 3C 120

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