Feeding and Feedback in the Powerful Radio Galaxy 3C 120

Tombesi, Francesco; Mushotzky, R. F.; Reynolds, C. S.; Kallman, T. R.; Reeves, J. N.; Braito, V.; Ueda, Yoshihiro; Leutenegger, Maurice A.; Williams, Brian J.; Stawarz, Ł.; Cappi, M.

doi:10.3847/1538-4357/aa6342

Cited by 17 publications

(13 citation statements)

References 121 publications

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“…Marscher et al 2002;Chatterjee et al 2009Chatterjee et al , 2011. In addition, Tombesi et al (2012Tombesi et al ( , 2013Tombesi et al ( , 2017 presented the evidence for the presence of mildlyrelativistic disk outflows in both sources, possibly related to the "X-ray dips/radio-outburst" cycles, and powerful enough to affect the surrounding interstellar medium in a feedback loop, as well as to collimate the radio jets. Any comparable characterization of the disk-jet connection in other radio galaxies, would require a long-term monitoring of particularly bright sources, for which the disk and the jet emission components are both accessible observationally.…”

Section: Introductionmentioning

confidence: 87%

Signatures of the Disk–Jet Coupling in the Broad-line Radio Quasar 4C+74.26

Bhatta

Stawarz

Markowitz

et al. 2018

ApJ

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Here we explore the disk-jet connection in the broad-line radio quasar 4C+74.26, utilizing the results of the multiwavelength monitoring of the source. The target is unique in that its radiative output at radio wavelengths is dominated by a moderately-beamed nuclear jet, at optical frequencies by the accretion disk, and in the hard X-ray range by the disk corona. Our analysis reveals a correlation (local and global significance of 96% and 98%, respectively) between the optical and radio bands, with the disk lagging behind the jet by 250 ± 42 days. We discuss the possible explanation for this, speculating that the observed disk and the jet flux changes are generated by magnetic fluctuations originating within the innermost parts of a truncated disk, and that the lag is related to a delayed radiative response of the disk when compared with the propagation timescale of magnetic perturbations along relativistic outflow. This scenario is supported by the re-analysis of the NuSTAR data, modelled in terms of a relativistic reflection from the disk illuminated by the coronal emission, which returns the inner disk radius R in /R ISCO = 35 +40 −16 . We discuss the global energetics in the system, arguing that while the accretion proceeds at the Eddington rate, with the accretion-related bolometric luminosity L bol ∼ 9 × 10 46 erg s −1 ∼ 0.2L Edd , the jet total kinetic energy L j ∼ 4 × 10 44 erg s −1 , inferred from the dynamical modelling of the giant radio lobes in the source, constitutes only a small fraction of the available accretion power.

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Section: Introductionmentioning

confidence: 87%

Signatures of the Disk–Jet Coupling in the Broad-line Radio Quasar 4C+74.26

Bhatta

Stawarz

Markowitz

et al. 2018

ApJ

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“…Deep and spatially resolved soft X-ray and radio observations may help to distinguish between energy-or momentum-conserving flows given that the emission from the shocked gas is expected to be different in these two cases (e.g., Bourne & Nayakshin 2013;Nims et al 2015). Some attempts have been reported in the literature (e.g., Zakamska & Greene 2014;Tombesi et al 2017).…”

Section: Connection With Galaxy-scale Molecular Outflowsmentioning

confidence: 99%

NuSTAR View of the Black Hole Wind in the Galaxy Merger IRAS F11119+3257

Tombesi

Veilleux

Meléndez

et al. 2017

ApJ

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Galactic winds driven by active galactic nuclei (AGNs) have been invoked to play a fundamental role in the coevolution between supermassive black holes and their host galaxies. Finding observational evidence of such feedback mechanisms is of crucial importance and it requires a multi-wavelength approach in order to compare winds at different scales and phases. In Tombesi et al., we reported the detection of a powerful ultra-fast outflow (UFO) in the Suzaku X-ray spectrum of the ultra-luminous infrared galaxy IRASF11119+3257. The comparison with a galaxy-scale OH molecular outflow observed with Herschel in the same source supported the energyconserving scenario for AGN feedback. The main objective of this work is to perform an independent check of the Suzaku results using the higher sensitivity and wider X-ray continuum coverage of NuSTAR. We clearly detect a highly ionized Fe K UFO in the 100 ks NuSTAR spectrum with parameters N H =(3.2±1.5)×10 24 cm −2 , log ξ= - 0.061 . The launching radius is likely at a distance of r16r s from the black hole. The mass outflow rate is in the range ofṀ out ;0.5-2 M e yr −1 . The UFO momentum rate and power areṖ out ;0.5-2 L AGN /c andĖ out ;7%-27% L AGN , respectively. The UFO parameters are consistent between the 2013 Suzaku and the 2015 NuSTAR observations. Only the column density is found to be variable, possibly suggesting a clumpy wind. The comparison with the energetics of molecular outflows estimated in infrared and millimeter wavelengths support a connection between the nuclear and galaxy-scale winds in luminous AGNs.

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“…A hot ISM with a temperature of kT ∼ 1 keV located within ∼ 4 kpc of the AGN is recently reported also in the Chandra grating spectra of two bright radio galaxies, namely 3C 390.3 and 3C 120 (Tombesi et al 2016(Tombesi et al , 2017. These radio galaxies show evidence of both powerful wind and jets, and it is suggested that their mechanical power may be enough to provide a heating source for the hot ISM (see, e.g., Tombesi et al 2017).…”

Section: Discussionmentioning

confidence: 85%

“…Using the relation of X-ray luminosity and star formation rate given by Mineo et al (2014), L X(0.5−8.0keV) 4 × 10 39 ( Ṁ * /M yr −1 ), we found a star formation rate of Ṁ * ∼ 40 M yr −1 . This value is more than an order of magnitude larger than the star formation rate expected from radio galaxies (see, e.g., Tombesi et al 2017;Westhues et al 2016), and is not likely adequate to supply enough heating to balance the cooling.…”

Section: Discussionmentioning

confidence: 87%

“…We performed an order of magnitude estimation of the cooling time at r = 3 kpc centered at NGC 5718 with Chandra following the procedure implemented by Tombesi et al (2017). The normalization of the XSPEC model apec is defined as; 10 −14 /4π [D A (1 + z)] 2 n e n H dV, where the integrant is the emission measure (EM), n e and n H are electron and hydrogen densities in cm −3 , and the angular diameter distance to NGC 5718 is D A 3.55 × 10 26 cm.…”

Section: Cooling Time Profilementioning

confidence: 99%

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Exploring the multiphase medium in MKW 08: from the central active galaxy up to cluster scales

Tümer

Tombesi

Bourdin

et al. 2019

A&A

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Context. The study of the brightest cluster galaxy (BCG) coronae embedded in noncool core (NCC) galaxy clusters is crucial to understand the BCG's role in galaxy cluster evolution as well as the activation of the self-regulated cooling and heating mechanism in the central regions of galaxy clusters. Aims. We explore the X-ray properties of the intracluster medium (ICM) of the NCC galaxy cluster MKW 08 and the BCG corona, along with their interface region. With recent and deep archival Chandra observations, we study the BCG corona in detail, and with archival XMM-Newton observations, we investigate the implications of the central active galactic nuclei (AGN) on the BCG. Methods. We carry out imaging and spectral analyses of MKW 08 with archival XMM-Newton and Chandra X-ray observations. Results. Our spectral analysis suggests the presence of a central AGN by a power-law with a photon index of Γ 1.8 at the core of its BCG. Although the ICM does not exhibit a cluster scale cool core, the BCG manifests itself as a mini cool core characterized by a cooling time as short as 64 Myr at r = 3 kpc centered at the galaxy. The isothermality of the BCG corona seems to favor mechanical feedback from the central AGN as the major source of gas heating. The gas pressure profile of this mini cool core suggests that the BCG coronal gas reaches pressure equilibrium with the hotter and less dense ICM inside an interface of nearly constant pressure, delimited by radii 4 r 10 kpc at the galactic center. As revealed by the presence of a metal enriched tail (Z 0.5 -0.9 Z ) extending up to 40 kpc, the BCG corona seems to be experiencing ram-pressure stripping by the surrounding ICM and/or interacting with a nearby galaxy, IC 1042.

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Feeding and Feedback in the Powerful Radio Galaxy 3C 120

Cited by 17 publications

References 121 publications

Signatures of the Disk–Jet Coupling in the Broad-line Radio Quasar 4C+74.26

Signatures of the Disk–Jet Coupling in the Broad-line Radio Quasar 4C+74.26

NuSTAR View of the Black Hole Wind in the Galaxy Merger IRAS F11119+3257

Exploring the multiphase medium in MKW 08: from the central active galaxy up to cluster scales

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