An X-ray and radio study of the Hubble Frontier Field cluster Abell S1063

Rahaman, Majidul; Raja, Ramij; Datta, Abhirup; Burns, Jack O.; Alden, Brian; Rapetti, David

doi:10.1093/mnras/stab1225

Cited by 17 publications

(11 citation statements)

References 70 publications

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“…A virial mass value of (2.17 ± 0.06) × 10 15 M was estimated by Sartoris et al (2020). Despite its regular shape, it appears to have recently undergone an off-axis merger, as inferred by Gómez et al (2012) and Rahaman et al (2021) from X-ray data, and by Mercurio et al (2021) from the dynamics of the members. Its high mass and redshift make it a very effective gravitational lens, which allows us to use the observed position of 55 spectroscopically confirmed multiple images from 20 background sources, distributed over a wide range of redshifts (z = 0.73−6.11; see Caminha et al 2016), to build an SL model.…”

Section: Abell S1063: Data and Analysismentioning

confidence: 97%

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Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063

Granata

Mercurio

Grillo

et al. 2022

A&A

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Aims. From accurate photometric and spectroscopic information, we build the Fundamental Plane (FP) relation for the early-type galaxies of the cluster Abell S1063. We use this relation to develop an improved strong lensing model of the cluster, and we decompose the cluster’s cumulative projected total mass profile into its stellar, hot gas, and dark matter mass components. We compare our results with the predictions of cosmological simulations. Methods. We calibrate the FP using Hubble Frontier Fields photometry and data from the Multi Unit Spectroscopic Explorer on the Very Large Telescope. The FP allows us to determine the velocity dispersions of all 222 cluster members included in the model from their measured structural parameters. As for their truncation radii, we test a proportionality relation with the observed half-light radii. Fixing the mass contribution of the hot gas component from X-ray data, the mass density distributions of the diffuse dark matter haloes are optimised by comparing the observed and model-predicted positions of 55 multiple images of 20 background sources distributed over the redshift range 0.73 − 6.11. We determine the uncertainties on the model parameters with Monte Carlo Markov chains. Results. We find that the most accurate predictions of the positions of the multiple images are obtained when the truncation radii of the member galaxies are approximately 2.3 times their effective radii. Compared to earlier work on the same cluster, our model allows for the inclusion of some scatter on the relation between the total mass and the velocity dispersion of the cluster members. We notice a lower statistical uncertainty on the value of some model parameters. For instance, the main dark matter halo of the cluster has a core radius of 86 ± 2 kpc: the uncertainty on this value decreases by more than 30% with respect to previous work. Taking advantage of a new estimate of the stellar mass of all cluster members from the HST multi-band data, we measure the cumulative two-dimensional mass profiles out to a radius of 350 kpc for all baryonic and dark matter components of the cluster. At the outermost radius of 350 kpc, we obtain a baryon fraction of 0.147 ± 0.002. We study the stellar-to-total mass fraction of the high-mass cluster members in our model, finding good agreement with the observations of wide galaxy surveys and some disagreement with the predictions of halo occupation distribution studies based on N-body simulations. Finally, we compare the features of the sub-haloes as described by our model with those predicted by high-resolution hydrodynamical simulations. We obtain compatible results in terms of the stellar over total mass fraction. On the other hand, we report some discrepancies both in terms of the maximum circular velocity, which is an indication of the halo compactness, and the sub-halo total mass function in the central cluster regions.

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Section: Abell S1063: Data and Analysismentioning

confidence: 97%

“…The cluster is also a very bright X-ray source (L X ≈ 2.5 × 10 45 erg s −1 in the 0.1−2.4 keV band), due to the emission of the hot (T ≈ 12 keV) ICM (Rahaman et al 2021): it was identified as RXJ2248.7−4431 in the ROSAT All-Sky Survey (De Grandi et al 1999;Guzzo et al 1999).…”

Section: Abell S1063: Data and Analysismentioning

confidence: 99%

Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063

Granata

Mercurio

Grillo

et al. 2022

A&A

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“…If the dynamical state of the cluster has been debated, recent work combining X-ray and radio observations indicates a disturbed state. AS 1063 is in an early stage of merging (see Rahaman et al 2021, and references therein).…”

Section: As 1063mentioning

confidence: 99%

Dark matter in galaxy clusters: Parametric strong-lensing approach

Limousin

Beauchesne

Jullo

2022

A&A

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Context. We present a parametric strong-lensing analysis of three massive galaxy clusters for which Hubble Space Telescope imaging is available, as well as spectroscopy of multiply imaged systems and galaxy cluster members. Our aim is to probe the inner shape of dark matter haloes, in particular the existence of a core. We adopted the following working hypothesis: any group-or cluster-scale dark matter clump introduced in the modelling should be associated with a luminous counterpart. We also adopted some additional well-motivated priors in the analysis, even when this degraded the quality of the fit, quantified using the root mean square between the observed and model-generated images. In particular, in order to alleviate the degeneracy between the smooth underlying component and the galaxy-scale perturbers, we used the results from previous spectroscopic campaigns, which allowed us to fix the mass of the galaxy-scale component. In the unimodal galaxy cluster AS 1063, a core mass model is favoured over a non-core mass model, and this is also the case in the multimodal cluster MACS J0416. In the unimodal cluster MACS J1206, we fail to reproduce the strong-lensing constraints using a parametric approach within the adopted working hypothesis. We then successfully added a mild perturbation in the form of a superposition of B-spline potentials, which allowed us to obtain a decent fit (root mean square = 0.5 ′′ ), and finally find that a core mass model is favoured. Overall, our analysis suggest evidence for core cluster-scale dark matter haloes in these three clusters. These findings may be useful for the interpretation within alternative dark matter scenario, such as self-interacting dark matter. We propose a working hypothesis for parametric strong-lensing modelling in which the quest for the best-fit model is balanced by the quest for presenting a physically motivated mass model, in particular by imposing priors. Aims.Methods. Results. Gravitational lensing: strong lensing -Galaxies: cluster -Conclusions.

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“…ACB temperature map was produced by using a method described in Datta et al (2014); Schenck et al (2014); Hallman et al (2018);Alden et al (2019); Rahaman et al (2021). Spectra were extracted from the circular region centered on every pixel.…”

Section: Adaptive Circular Binning (Acb) Methodsmentioning

confidence: 99%

On the detection of multiple shock fronts in A1914 using deep Chandra X-ray observations

Rahaman,

Raja,

Datta

2021

Preprint

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Here, we report the new detection of three shock fronts using archival Chandra X-ray observations in Abell 1914, which also hosts a radio halo, a radio phoenix, and a head-tail galaxy. In this study, we report the X-ray shock front at the position of the radio phoenix, which further strengthens the scenario that radio phoenix traces old plasma that gets lit up when compressed by shock passage. We further analyze the thermodynamic structure of the cluster in detail. We create temperature maps of A1914 using three different techniques, Adaptive Circular Binning (ACB), Weighted Voronoi Tessellations (WVT), and Contour binning (Contbin) method. These thermodynamic maps, along with the pseudo pressure and the pseudo entropy maps for the cluster, are evidence of disturbed morphology produced by multiple merger events. These merger events create cluster-wide turbulence, which may re-accelerate the relativistic particles and result in a radio halo within the cluster. Further, comparing X-ray and radio images reveals that the radio halo is contained within two X-ray shock fronts. Our analysis suggests that A1914 has both equatorial shock and axial shock within the cluster's ICM. We proposed a dual merging scenario based on the shock position and analysis of the thermodynamic maps obtained from the deeper Chandra X-ray observations.

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An X-ray and radio study of the Hubble Frontier Field cluster Abell S1063

Cited by 17 publications

References 70 publications

Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063

Improved strong lensing modelling of galaxy clusters using the Fundamental Plane: Detailed mapping of the baryonic and dark matter mass distribution of Abell S1063

Dark matter in galaxy clusters: Parametric strong-lensing approach

On the detection of multiple shock fronts in A1914 using deep Chandra X-ray observations

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