Dynamical modelling and emission signatures of a candidate dual AGN with precessing radio jets

Giri, Gourab; Dubey, Ravi Pratap; Rubinur, K; Vaidya, Bhargav; Kharb, P.

doi:10.1093/mnras/stac1628

Cited by 8 publications

(12 citation statements)

References 70 publications

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“…√ 4πρ) at time 114 Myr is 4.97 (super Alfvénic state), a regime enabling the KHIs to grow (Acharya et al 2021;Giri et al 2022a). Such turbulent structure further generates sites of random shocks, therefore making these radio galaxies an ideal target for studying particle acceleration (see e.g., Mukherjee et al 2021).…”

Section: The Average Alfvénic Mach Number Of the Cocoon (Mmentioning

confidence: 99%

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

Giri

Vaidya

Rossi

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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Section: The Average Alfvénic Mach Number Of the Cocoon (Mmentioning

confidence: 99%

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

Giri

Vaidya

Rossi

et al. 2022

A&A

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“…This investigation entails modeling the morphology, for example, using kinematic jet precession models (Hjellming and Johnston, 1981;. Studies, exemplified by observational research from ; Gong et al (2011);Rubinur et al (2017); Krause et al (2019); Nandi et al (2021), along with pivotal simulation contributions by Horton et al (2020); Giri et al (2022a), have explored different aspects of such cases, e.g., mass ratios, precession period and separation of the SMBH pair, shedding light on the potential parameter space for such binaries.…”

Section: Host Agnmentioning

confidence: 99%

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

Giri,

Fendt,

Thorat

et al. 2024

Front. Astron. Space Sci.

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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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“…) at 114 Myr is 4.97 (super-Alfvénic state), a regime enabling the KH instabilities to grow (Acharya et al 2021;Giri et al 2022a). This turbulent structure further generates sites of random shocks, thereby making these radio galaxies an ideal target for studying particle acceleration (see, e.g., Mukherjee et al 2021).…”

Section: Reference Casementioning

confidence: 99%

Deciphering the Morphological Origins of X-shaped Radio Galaxies: Numerical Modeling of Backflow versus Jet Reorientation

Giri,

Vaidya,

Fendt

2023

ApJS

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X-shaped radio galaxies (XRGs) develop when certain extragalactic jets deviate from their propagation path. An asymmetric ambient medium (backflow model) or complex active galactic nucleus activity (jet-reorientation model) enforcing the jet direction to deviate may cause these structures. In this context, the present investigation focuses on the modeling of XRGs by performing 3D relativistic magnetohydrodynamic simulations. We implement different jet-propagation models applying an initially identical jet-ambient medium configuration to understand distinctive features. This study, the first of its kind, demonstrates that all adopted models produce XRGs with notable properties, thereby challenging the notion of a universal model. Jet reorientation naturally explains several contentious properties of XRGs, including wing alignment along the ambient medium’s primary axis, development of collimated lobes, and the formation of noticeably longer wings than active lobes. These XRGs disrupt the cluster medium by generating isotropic shocks and channeling more energy than in the backflow scenario. Our synthetic thermal X-ray maps of the cluster medium reveal four clear elongated cavities associated with the wing-lobe alignment, regardless of projection effects, but they affect their age estimation. We show that the depth and geometric alignment of the evolved cavities may qualify as promising characteristics of XRGs, which may be used to disentangle different formation scenarios.

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Dynamical modelling and emission signatures of a candidate dual AGN with precessing radio jets

Cited by 8 publications

References 70 publications

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

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

Deciphering the Morphological Origins of X-shaped Radio Galaxies: Numerical Modeling of Backflow versus Jet Reorientation

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