AGN feedback in the FR II galaxy 3C 220.1

Liu, Wenhao; Sun, Ming; Nulsen, P. E. J.; Worrall, D. M.; Birkinshaw, Mark; Sarazin, Craig L.; Forman, W.; Jones, C.; Ge, Chong

doi:10.1093/mnras/staa005

Cited by 11 publications

(5 citation statements)

References 76 publications

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“…Additionally, we checked whether new detections had been claimed after the work of Liu et al (2019), finding no new results. Surface brightness edges were identified in 3C 220.1 by Liu et al (2020) and 3C 320 by Vagshette et al (2019); however, due to the insufficient number of counts, a spectral confirmation of their shock front nature was not performed. We also consider Perseus due to the putative weak shock surrounding its inner X-ray cavities (Graham et al 2008b).…”

Section: Shock and Cavity Heating Of Hot Atmospheresmentioning

confidence: 99%

Multiple Shock Fronts in RBS 797: The Chandra Window on Shock Heating in Galaxy Clusters

Ubertosi

Gitti

Brighenti

et al. 2023

ApJ

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Using ∼427 ks of Chandra observations, we present a study of shock heating and intracluster medium (ICM) cooling in the galaxy cluster RBS 797. We discover three nested pairs of weak shocks at roughly 50, 80, and 130 kpc from the center. The total energy associated with the shocks is ∼6 × 1061 erg, with the central active galactic nucleus (AGN) driving a pair of weak shocks every 20–30 Myr with a power P sh ≈ 1046 erg s−1. Based on its morphology and age (∼30 Myr), the inner cocoon shock is associated with the four equidistant X-ray cavities previously discovered. From the thermodynamic analysis of the inner 30 kpc, we find evidence for ICM condensation into colder gas between and behind the X-ray cavities. The total AGN mechanical power (cavities and shocks) of 3.4 × 1046 erg s−1 can balance the ICM radiative losses, estimated as L cool = 2.3 × 1045 erg s−1. By building plots of P cav versus L cool, P shock versus L cool, and P tot versus L cool for RBS 797 and 14 other galaxy clusters, galaxy groups, and elliptical galaxies where both cavities and shocks are detected, we verify that the most powerful outbursts are found in the strongest cooling systems. Ultimately, we observe that the mechanical power of the AGN exceeds the gas radiative losses by a factor that is different for FR I and FR II radio galaxies, being less than a few tens for FR Is (as RBS 797) and more than roughly 100 for FR IIs.

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Section: Shock and Cavity Heating Of Hot Atmospheresmentioning

confidence: 99%

Multiple Shock Fronts in RBS 797: The Chandra Window on Shock Heating in Galaxy Clusters

Ubertosi

Gitti

Brighenti

et al. 2023

ApJ

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“…Considering, for example, odd polynomials, or the addition of odd and even polynomials, will yield asymmetric velocity fields. This last might even suggest the existence of an intrinsic component to observed morphological and energetic jet asymmetries such as the ones often observed in FR II systems (e.g., Hardcastle et al (1999) or Liu et al (2020)). As the Legendre polynomials form an orthogonal basis, any given axisymmetric flow configuration can be reproduced with the velocity solutions presented here, with the model then yielding a corresponding self-consistent density configuration.…”

Section: Deviations From Spherical Symmetrymentioning

confidence: 85%

A New Hydrodynamic Spherical Accretion Exact Solution and Its Quasi-spherical Perturbations

Hernández

Nasser

Aguayo-Ortiz

2023

ApJ

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We present an exact γ = 5/3 spherical accretion solution that modifies the Bondi boundary condition of ρ → constant as r → ∞ to ρ → 0 as r → ∞. This change allows for simple power-law solutions on the density and infall velocity fields, ranging from a cold empty freefall condition where pressure tends to zero, to a hot hydrostatic equilibrium limit with no infall velocity. As in the case of the Bondi solution, a maximum accretion rate appears. As in the γ = 5/3 case of the Bondi solution, no sonic radius appears, this time however, because the flow is always characterized by a constant Mach number. This number equals 1 for the case of the maximum accretion rate, diverges toward the cold empty state, and becomes subsonic toward the hydrostatic equilibrium limit. It can be shown that in the limit r → 0, the Bondi solution tends to the new solution presented, extending the validity of the Bondi accretion value to cases where the accretion density profile does not remain at a fixed constant value out to infinity. We then explore small deviations from sphericity and the presence of angular momentum through an analytic perturbative analysis. Such perturbed solutions yield a rich phenomenology through density and velocity fields in terms of Legendre polynomials, which we begin to explore for simple angular velocity boundary conditions having zeros on the plane and pole. The new solution presented provides complementary physical insight into accretion problems in general.

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“…Models of relativistic jets interacting with inclined or curved lobe/ICM interfaces may also be applied to other observed interactions, such as the eastern jet of Cygnus A and the FRII source 3C 220.1, which shows a jet potentially deflected against an interface at multiple locations [27].…”

Section: Discussionmentioning

confidence: 99%

Hydrodynamic Simulations of a Relativistic Jet Interacting with the Intracluster Medium: Application to Cygnus A

et al. 2023

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The Fanaroff–Riley Class II radio galaxy Cygnus A hosts jets that produce radio emission, X-ray cavities, cocoon shocks, and X-ray hotspots, where the jet interacts with the ICM. Surrounding one hotspot is a peculiar “hole” feature, which appears as a deficit in X-ray emission. We used relativistic hydrodynamic simulations of a collimated jet interacting with an inclined interface between lobe and cluster plasma to model the basic processes that may lead to such a feature. We found that the jet reflects off of the interface into a broad, turbulent flow back out into the lobe, which is dominated by gas stripped from the interface at first and from the intracluster medium itself at later times. We produced simple models of X-ray emission from the ICM, the hotspot, and the reflected jet to show that a hole of emission surrounding the hotspot as seen in Cygnus A may be produced by Doppler de-boosting of the emission from the reflected jet, as seen by an observer with a sight line nearly along the axis of the outgoing material.

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AGN feedback in the FR II galaxy 3C 220.1

Cited by 11 publications

References 76 publications

Multiple Shock Fronts in RBS 797: The Chandra Window on Shock Heating in Galaxy Clusters

Multiple Shock Fronts in RBS 797: The Chandra Window on Shock Heating in Galaxy Clusters

A New Hydrodynamic Spherical Accretion Exact Solution and Its Quasi-spherical Perturbations

Hydrodynamic Simulations of a Relativistic Jet Interacting with the Intracluster Medium: Application to Cygnus A

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