On the jet contribution to the active galactic nuclei cosmic energy budget

Cattaneo, Andrea; Best, P. N.

doi:10.1111/j.1365-2966.2009.14557.x

Cited by 66 publications

(63 citation statements)

References 47 publications

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“…Less straightforward is to compile a kinetic luminosity function. It has been done however by Merloni & Heinz (2008), Cattaneo & Best (2009) and Mocz et al (2012). The accretion history is inferred from the radiant luminosity functions, and some assumption is made connecting that to the kinetic power history.…”

Section: The Kinetic Luminosity Functionmentioning

confidence: 99%

Observational Evidence of Active Galactic Nuclei Feedback

Fabian

2012

Annu. Rev. Astron. Astrophys.

2,449

2,070

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Radiation, winds and jets from the active nucleus of a massive galaxy can interact with its interstellar medium leading to ejection or heating of the gas. This can terminate star formation in the galaxy and stifle accretion onto the black hole. Such Active Galactic Nucleus (AGN) feedback can account for the observed proportionality between central black hole and host galaxy mass. Direct observational evidence for the radiative or quasar mode of feedback, which occurs when the AGN is very luminous, has been difficult to obtain but is accumulating from a few exceptional objects. Feedback from the kinetic or radio mode, which uses the mechanical energy of radio-emitting jets often seen when the AGN is operating at a lower level, is common in massive elliptical galaxies. This mode is well observed directly through X-ray observations of the central galaxies of cool core clusters in the form of bubbles in the hot surrounding medium. The energy flow, which is roughly continuous, heats the hot intracluster gas and reduces radiative cooling and subsequent star formation by an order of magnitude. Feedback appears to maintain a long-lived heating/cooling balance. Powerful, jetted radio outbursts may represent a further mode of energy feedback which affect the cores of groups and subclusters. New telescopes and instruments from the radio to X-ray bands will come into operation over the next few years and lead to a rapid expansion in observational data on all modes of AGN feedback.

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Section: The Kinetic Luminosity Functionmentioning

confidence: 99%

Observational Evidence of Active Galactic Nuclei Feedback

Fabian

2012

Annu. Rev. Astron. Astrophys.

2,449

2,070

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“…Knowledge of the kinetic power of active galactic nucleus (AGN) jets is vital for quantifying the energetics of AGN feedback and its effect on the host galaxy formation and evolution (Croton et al 2006;Cattaneo & Best 2009;Shabala & Alexander 2009). This kinetic jet-mode of feedback is dominant at the present epoch, whilst the radiative quasarmode was prevalent in the early universe (z ∼ 2-3; Fabian 2012).…”

Section: Introductionmentioning

confidence: 99%

RAiSE III: 3C radio AGN energetics and composition

Turner

Shabala

Krause

2017

Monthly Notices of the Royal Astronomical Society

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Kinetic jet power estimates based exclusively on observed monochromatic radio luminosities are highly uncertain due to confounding variables and a lack of knowledge about some aspects of the physics of active galactic nuclei (AGNs). We propose a new methodology to calculate the jet powers of the largest, most powerful radio sources based on combinations of their size, lobe luminosity and shape of their radio spectrum; this approach avoids the uncertainties encountered by previous relationships. The outputs of our model are calibrated using hydrodynamical simulations and tested against independent X-ray inverse-Compton measurements. The jet powers and lobe magnetic field strengths of radio sources are found to be recovered using solely the lobe luminosity and spectral curvature, enabling the intrinsic properties of unresolved highredshift sources to be inferred. By contrast, the radio source ages cannot be estimated without knowledge of the lobe volumes. The monochromatic lobe luminosity alone is incapable of accurately estimating the jet power or source age without knowledge of the lobe magnetic field strength and size respectively. We find that, on average, the lobes of the 3C radio sources have magnetic field strengths approximately a factor three lower than the equipartition value, inconsistent with equal energy in the particles and the fields at the 5σ level. The particle content of 3C radio lobes is discussed in the context of complementary observations; we do not find evidence favouring an energetically-dominant proton population.

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“…The number density of AGN cannot exceed that of their potential hosts: this argument has been used by Mauch & Sadler (2007) and Cattaneo & Best (2009) to constrain the low luminosity behavior of their RLF. They found that a break must occur at a radio luminosity log(Pr/ W Hz −1 ) ∼ 19.5 and 19.2, respectively.…”

Section: The Radio Agn Luminosity Functionmentioning

confidence: 99%

Looking below the floor: constraints on the AGN radio luminosity functions at low power

Capetti

Raiteri

2015

Monthly Notices of the Royal Astronomical Society: Letters

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We constrain the behavior of the radio luminosity function (RLF) of two classes of active galactic nuclei (AGN) namely AGN of low radio power (LRP) and BL Lac objects. The extrapolation of the observed steep RLFs to low power predicts a space density of such objects that exceeds that of the sources that can harbor them and this requires a break to a shallower slope. For LRP AGN we obtain P br,LRP 10 20.5 W Hz −1 at 1.4 GHz to limit their density to be smaller than that of elliptical galaxies with black hole masses M BH > 10 7.5 M ⊙ . By combining this value with the limit derived by the observations the break must occur at P br,LRP ∼ 10 20.5 − 10 21.5 W Hz −1 . For BL Lacs we find P br,BLLAC 10 23.3 W Hz −1 otherwise they would outnumber the density of weak-lined and compact radio sources, while the observations indicate P br,BLLAC 10 24.5 W Hz −1 . In the framework of the AGN unified model a low luminosity break in the RLF of LRP AGN must correspond to a break in the RLF of BL Lacs. The ratio between P br,LRP and P br,BLLAC is ∼ 10 3 , as expected for a jet Doppler factor of ∼ 10.

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On the jet contribution to the active galactic nuclei cosmic energy budget

Cited by 66 publications

References 47 publications

Observational Evidence of Active Galactic Nuclei Feedback

Observational Evidence of Active Galactic Nuclei Feedback

RAiSE III: 3C radio AGN energetics and composition

Looking below the floor: constraints on the AGN radio luminosity functions at low power

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