A Multiwavelength Study of the Cool Core Cluster MACS J1447.4+0827

Prasow-Émond, M.; Hlavacek-Larrondo, J.; Rhea, Carter; Latulippe, M.; Gendron-Marsolais, Marie-Lou; Richard-Laferrière, A.; Sanders, J. S.; Edge, A. C.; Allen, S. W.; Mantz, Adam; Linden, Anja von der

doi:10.3847/1538-3881/ab9ff3

Cited by 9 publications

(4 citation statements)

References 119 publications

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“…This galaxy cluster is located at z = 0.376. The presence of small X-ray cavities and sloshing signatures in this object has been reported by Prasow-Émond et al (2020). On VLBA scales, the source is clearly resolved in a two-sided structure oriented northwest-southeast.…”

Section: Appendix Esupporting

confidence: 68%

Jet Reorientation in Central Galaxies of Clusters and Groups: Insights from VLBA and Chandra Data

Ubertosi,

Schellenberger,

O’Sullivan

et al. 2024

ApJ

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Recent observations of galaxy clusters and groups with misalignments between their central active galactic nucleus jets and X-ray cavities, or with multiple misaligned cavities, have raised concerns about the jet–bubble connection in cooling cores, and the processes responsible for jet realignment. To investigate the frequency and causes of such misalignments, we construct a sample of 16 cool core galaxy clusters and groups. Using Very Long Baseline Array radio data, we measure the parsec-scale position angle of the jets, and compare it with the position angle of the X-ray cavities detected in Chandra data. Using the overall sample and selected subsets, we consistently find that there is a 30%–38% chance to find a misalignment larger than ΔΨ = 45° when observing a cluster/group with a detected jet and at least one cavity. We determine that projection may account for an apparently large ΔΨ only in a fraction of objects (∼35%), and given that gas dynamical disturbances (such as sloshing) are found in both aligned and misaligned systems, we exclude environmental perturbation as the main driver of cavity–jet misalignment. Moreover, we find that large misalignments (up to ∼90°) are favored over smaller ones (45° ≤ ΔΨ ≤ 70°), and that the change in jet direction can occur on timescales between one and a few tens of Myr. We conclude that misalignments are more likely related to actual reorientation of the jet axis, and we discuss several engine-based mechanisms that may cause these dramatic changes.

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Section: Appendix Esupporting

confidence: 68%

Jet Reorientation in Central Galaxies of Clusters and Groups: Insights from VLBA and Chandra Data

Ubertosi,

Schellenberger,

O’Sullivan

et al. 2024

ApJ

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“…X-ray cavities can take many forms and provide a means of investigating galaxy and cluster formation at high redshift since cluster cooling flows are strong X-ray sources. MACS J1447.4+0827 (z = 0.3755) provides a recent example of jet evacuated cavities (Prasow-Émond et al 2020). Unlike Cygnus A, in this case two separate cavities on a scale of 100 kpc are detected.…”

Section: Discussionmentioning

confidence: 90%

Three-dimensional simulations of X-ray cavities inflated by radio galaxies

Smith

Donohoe

2021

Monthly Notices of the Royal Astronomical Society

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Vast cavities in the intergalactic medium are excavated by radio galaxies. The cavities appear as such in X-ray images because the external medium has been swept-up, leaving a hot but low-density bubble surrounding the radio lobes. We explore here the predicted thermal X-ray emission from a large set of high-resolution three-dimensional simulations of radio galaxies driven by supersonic jets. We assume adiabatic non-relativistic hydrodynamics with injected straight and precessing jets of supersonic gas emitted from nozzles. Images of X-ray bremsstrahlung emission tend to generate oval cavities in the soft keV bands and leading arcuate structures in hard X-rays. However, the cavity shape is sensitive to the jet-ambient density contrast, varying from concave-shaped at η = 0.1 to convex for η = 0.0001 where η is the jet/ambient density ratio. We find lateral ribs in the soft X-rays in certain cases and propose this as an explanation for those detected in the vicinity of Cygnus A. In bi-lobed or X-shaped sources and in curved or deflected jets, the strongest X-ray emission is not associated with the hotspot but with the relic lobe or deflection location. This is because the hot high-pressure and dense high-compression regions do not coincide. Directed towards the observer, the cavity becomes a deep round hole surrounded by circular ripples. With short radio-mode outbursts with a duty cycle of 10 per cent, the intracluster medium simmers with low Mach number shocks widely dissipating the jet energy in between active jet episodes.

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“…In the cool cores of relaxed clusters of galaxies, the central radio galaxy is often surrounded by diffuse, steep-spectrum 5 synchrotron sources, called radio minihalos (see, e.g., van Weeren et al 2019, for a review). The number of known minihalos sums up to about 40 detections including candidates (e.g., Giacintucci et al 2019;Richard-Laferrière et al 2020, and references therein); for recent detections, see Giovannini et al (2020), Prasow-Émond et al (2020), Duchesne et al (2021), Ubertosi et al (2021), Kale et al (2022), Knowles et al (2022), Bégin et al (2023), Lusetti et al (2023), and Riseley et al (2023). They are usually found in high-mass clusters, with a high incidence of ∼80% in the most massive systems (M 500 > 6 × 10 14 M e ) 6 among the cool-core cluster population (Giacintucci et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Are Radio Minihalos Confined by Cold Fronts in Galaxy Clusters? Minihalos and Large-scale Sloshing in A3444 and MS 1455.0+2232

Giacintucci,

Venturi,

Markevitch

et al. 2024

ApJ

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We present radio and X-ray studies of A3444 and MS1455.0+2232, two galaxy clusters with radio minihalos in their cool cores. A3444 is imaged using the Giant Metrewave Radio Telescope (GMRT) at 333, 607, and 1300 MHz and the Very Large Array at 1435 MHz. Most of the minihalo is contained within r < 120 kpc, but a fainter extension, stretching out to 380 kpc southwest of the center, is detected at 607 MHz. Using Chandra, we detect four X-ray sloshing cold fronts: three in the cool core at r = 60, 120, and 230 kpc, and a fourth one at r = 400 kpc—in the region of the southwestern radio extension—suggesting that the intracluster medium (ICM) is sloshing on a cluster-wide scale. The radio emission is contained within the envelope defined by these fronts. We also analyzed archival 383 MHz GMRT and Chandra observations of MS 1455.0+2232, which exhibits a known minihalo with its bright part delineated by cold fronts inside the cool core, but with a faint extension beyond the core. Similarly to A3444, we find a cold front at r ∼ 425 kpc, containing the radio emission. Thus the entire diffuse radio emission seen in these clusters appears to be related to large-scale sloshing of the ICM. The radio spectrum of the A3444 minihalo is a power law with a steep index α = 1.0 ± 0.1. The spectrum steepens with increasing distance from the center, as expected if the minihalo originates from reacceleration of relativistic particles by the sloshing-induced turbulence in the ICM.

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A Multiwavelength Study of the Cool Core Cluster MACS J1447.4+0827

Cited by 9 publications

References 119 publications

Jet Reorientation in Central Galaxies of Clusters and Groups: Insights from VLBA and Chandra Data

Jet Reorientation in Central Galaxies of Clusters and Groups: Insights from VLBA and Chandra Data

Three-dimensional simulations of X-ray cavities inflated by radio galaxies

Are Radio Minihalos Confined by Cold Fronts in Galaxy Clusters? Minihalos and Large-scale Sloshing in A3444 and MS 1455.0+2232

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