AGN Feeding and Feedback in M84: From Kiloparsec Scales to the Bondi Radius

Bambic, C. J.; Russell, H. R.; Reynolds, C. S.; Fabian, A. C.; McNamara, B. R.; Nulsen, Paul

doi:10.48550/arxiv.2301.11937

“…Observations of M87 (Russell et al 2015) suggested there are two significant temperature components within 2 kpc and did not find evidence for a temperature increase within ∼0.25 kpc. The flat temperature profile is also reported in observations of the galaxy M84 (Bambic et al 2023). This is consistent with our simulations.…”

Section: Radial Profilessupporting

confidence: 93%

Toward Horizon-scale Accretion onto Supermassive Black Holes in Elliptical Galaxies

Guo

¹

,

Stone

²

,

Kim

³

et al. 2023

ApJ

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We present high-resolution, three-dimensional hydrodynamic simulations of the fueling of supermassive black holes in elliptical galaxies from a turbulent medium on galactic scales, taking M87* as a typical case. The simulations use a new GPU-accelerated version of the Athena++ AMR code, and they span more than six orders of magnitude in radius, reaching scales similar to that of the black hole horizon. The key physical ingredients are radiative cooling and a phenomenological heating model. We find that the accretion flow takes the form of multiphase gas at radii less than about a kpc. The cold gas accretion includes two dynamically distinct stages: the typical disk stage in which the cold gas resides in a rotationally supported disk, and relatively rare chaotic stages (≲10% of the time) in which the cold gas inflows via chaotic streams. Though cold gas accretion dominates the time-averaged accretion rate at intermediate radii, accretion at the smallest radii is dominated by hot virialized gas at most times. The accretion rate scales with radius as M ̇ ∝ r 1 / 2 when hot gas dominates, and we obtain M ̇ ≃ 10 − 4 – 10 − 3 M ⊙ yr − 1 near the event horizon, similar to what is inferred from EHT observations. The orientation of the cold gas disk can differ significantly on different spatial scales. We propose a subgrid model for accretion in lower-resolution simulations in which the hot gas accretion rate is suppressed relative to the Bondi rate by ∼ ( r g / r Bondi ) 1 / 2 . Our results can also provide more realistic initial conditions for simulations of black hole accretion at the event horizon scale.

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“…An even more complex example can be found in the Perseus Galaxy Cluster (Fabian et al 2017), which shows off-axis cavities, rims, and a geometrically complex distribution of pressure waves (also see Ubertosi et al 2022, for the RBS 797 galaxy cluster). Other galaxy groups or clusters with such intricate cavity structures include, for example, M84 (Bambic et al 2023), NGC 5813 (Randall et al 2015), A2052 (Blanton et al 2011), NGC 5044 (David et al 2011, Cygnus A (Smith et al 2002), MS0735.6+7421 (McNamara et al 2009.…”

Section: Introductionmentioning

confidence: 99%

Modelling X-shaped radio galaxies: Dynamical and emission signatures from the Back-flow model

Giri

¹

,

Vaidya

²

,

Rossi

³

et al. 2022

A&A

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Context. Active galactic nuclei typically show the presence of radio jets ranging from sub-kiloparsec to megaparsec scales. Some of these radio galaxies show distortion in their jets, forming tailed or winged sources. X-shaped radio galaxies (XRGs) are a sub-class of winged sources, the formation mechanism of which is still unclear. Aims. The focus of this work is to understand hydro-dynamical back-flows and their role in dynamics and non-thermal emission signatures (in the presence of radiative losses and diffusive shock acceleration) during the initial phase of these galaxies. Methods. We performed relativistic magneto-hydrodynamic (RMHD) simulations of an under-dense jet travelling in a tri-axial ambient using a hybrid Eulerian-Lagrangian framework to incorporate effects of micro-physical processes. Results. We demonstrate the dominant role played by pressure gradient in shaping XRGs in thermally dominated cases. We show that the prominence of the formed structure decreases as the jet deviates from the major axis of the ambient. The wing evolution is mainly governed by re-energised particles due to shocks that keep the structure active during the evolution time. The synthetic intensity maps of the radio galaxy show similarities with morphologies that are typically found in observed XRGs. This includes the cases with wider wings than the active lobes. The characteristic emission signatures in terms of its synchrotron spectra and the implication of equipartition condition in age estimation are also discussed here. Additionally, we show that age discrepancies can be attributed to the mixing of different aged particle populations. Furthermore, the effect of the viewing angle on the difference of spectral index (Δα) of the active lobes and the wings shows a large variation and degenerate behaviour. We demonstrate the role of diffusive shocks in the obtained variation and conclude that the Δα spread is not a dependable characteristic in determining the formation model of XRGs.

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“…Observations in galaxy clusters like Perseus show off-axis cavities, rims, and intricate pressure wave distributions (Fabian et al, 2017). Similarly complex structures are observed in other systems such as M84 (Bambic et al, 2023), NGC 5813 (Randall et al, 2015), A2052 (Blanton et al, 2011), NGC 5044 (David et al, 2011), Cygnus A (Smith et al, 2002), MS0735.6 + 7,421 (McNamara et al, 2009. This complexity in 1 A better estimate may be the Alfvén time scale cavity structures may indicate deflections in the path of the jets involved, highlighting a possible jet reorientation phenomenon.…”

Section: X-ray Cavities Associated With the Xrgsmentioning

confidence: 76%

X-shaped radio galaxies: probing jet evolution, ambient medium dynamics, and their intricate interconnection

Giri,

Fendt,

Thorat

et al. 2024

Front. Astron. Space Sci.

2

0

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This review explores the field of X-shaped radio galaxies (XRGs), a distinctive subset of winged radio sources that are identified by two pairs of jetted lobes which aligned by a significant angle, resulting in an inversion-symmetric structure. These lobes, encompassing active (primary) and passive (secondary) phases, exhibit a diverse range of properties across the multiple frequency bands, posing challenges in discerning their formation mechanism. The proposed mechanisms can broadly be categorized into those related either to a triaxial ambient medium, into which the jet propagates, or to a complex, central AGN mechanism, where the jet is generated. The observed characteristics of XRGs as discovered in the most substantial sample to date, challenge the idea that there is universal process at work that produces the individual sources of XRGs. Instead, the observational and numerical results rather imply the absence of an universal model and infer that distinct mechanisms may be at play for the specific sources. By scrutinizing salient and confounding properties, this review intends to propose the potential direction for future research to constrain and constrict individual models applicable to XRGs.

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AGN Feeding and Feedback in M84: From Kiloparsec Scales to the Bondi Radius

Cited by 4 publications

References 120 publications

Toward Horizon-scale Accretion onto Supermassive Black Holes in Elliptical Galaxies

Toward Horizon-scale Accretion onto Supermassive Black Holes in Elliptical Galaxies

Modelling X-shaped radio galaxies: Dynamical and emission signatures from the Back-flow model

X-shaped radio galaxies: probing jet evolution, ambient medium dynamics, and their intricate interconnection

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