Testing the rotation versus merger scenario in the galaxy cluster Abell 2107

Liu, Ang; Tozzi, P.

doi:10.1093/mnras/stz713

Cited by 5 publications

(1 citation statement)

References 43 publications

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“…A possible source of bias to our results is the deviation from hydrostatic equilibrium of the ICM in J0723. This socalled "hydrostatic mass bias" can be caused by major and minor mergers (e.g., Markevitch et al 2002;Vikhlinin et al 2001), core sloshing (e.g., Markevitch et al 2001;Sanders et al 2005), gas turbulence (only a few percent, see Eckert et al 2019), possible global rotation (Liu & Tozzi 2019), and other non-gravitational processes such as AGN feedback (Fabian 2012). On the Chandra image, there are no signs of violent mergers.…”

Section: Discussionmentioning

confidence: 99%

X-ray analysis of JWST’s first galaxy cluster lens SMACS J0723.3−7327

Liu

Bülbül

Ramos-Ceja

et al. 2023

A&A

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Context. SMACS J0723.3-7327 is the first galaxy cluster lens observed by James Webb Space Telescope (JWST). Based on its early release observation data, several groups have reported the results on strong lensing analysis and mass distribution of this cluster. The new lens model dramatically improves upon previous results, thanks to JWST's unprecedented sensitivity and angular resolution. However, limited by the angular coverage of the JWST data, the strong lensing models only cover the central region. Conducting an X-ray analysis on the hot intracluster medium (ICM) is necessary to obtain a more complete constraint on the mass distribution in this very massive cluster. Aims. In this work, we perform a comprehensive X-ray analysis of J0723 with an aim to obtain accurate ICM hydrostatic mass measurements, using the X-ray data from Spectrum Roentgen Gamma (SRG)/eROSITA and Chandra X-ray observatories. By comparing the hydrostatic mass profile with the strong lensing model, we aim to provide the most reliable constraint on the distribution of mass up to R 500 . Methods. Thanks to the eROSITA all-sky survey and Chandra, which provide high signal-to-noise ratio (S/N) and high angular resolution data, respectively, we were able to constrain the ICM gas density profile and temperature profile with good accuracy both in the core and to the outskirts. With the density and temperature profiles, we computed the hydrostatic mass profile, which was then projected along the line of sight to compare with the mass distribution obtained from the recent strong lensing analysis based on JWST data. We also deprojected the strong lensing mass distribution using the hydrostatic mass profile obtained in this work. Results. The X-ray results obtained from eROSITA and Chandra are in very good agreement. The hydrostatic mass profiles we measured in this work, both projected and deprojected, are in good agreement with recent strong lensing results based on JWST data, at all radii. The projected hydrostatic mass within 128 kpc (the estimated Einstein radius) is (8.0 ± 0.7) × 10 13 M ⊙ , consistent with the strong lensing mass reported in recent literature. With the hydrostatic mass profile, we measured R 2500 = 0.54 ± 0.04 Mpc and M 2500 = (3.5 ± 0.8) × 10 14 M ⊙ , while the R 500 and M 500 are 1.32 ± 0.23 Mpc and (9.8 ± 5.1) × 10 14 M ⊙ , with a relatively larger error bar due to the rapidly decreasing S/N in the outskirts. We also find that the radial acceleration relation in J0723 is inconsistent with the RAR for spiral galaxies, implying that the latter is not a universal property of gravity across all mass scales.

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Section: Discussionmentioning

confidence: 99%

X-ray analysis of JWST’s first galaxy cluster lens SMACS J0723.3−7327

Liu

Bülbül

Ramos-Ceja

et al. 2023

A&A

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Dynamics of the galactic component of Abell S1063 and MACS J1206.2−0847

Ferrami¹,

Bertin²,

Grillo³

et al. 2023

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Context. The galactic component in clusters is commonly thought to be generally nonrotating and in a dynamical state different from that of a collisionally relaxed system. In practice, a test for such conditions is often not available. Aims. We consider the member galaxies of the two clusters Abell S1063 and MACS J1206.2−0847 and study the possible presence of mean rotation and some properties of their distribution in phase space. We look for empirical evidence of factors normally found in collisionally relaxed systems and other characteristics of violently relaxed collisionless systems. Methods. Starting from the CLASH-VLT data, we obtained positions, stellar masses, and individual line-of-sight velocities for a large number of galaxies (NAS1063 ≈ 1200 and NM1206 ≈ 650) extending out to ≈1.6 (Abell) and ≈2.5 (MACS) times the radius r200. We studied the spatial distribution of the galaxy velocities and the properties of the available galaxy sets when divided into stellar mass bins. To test the presence of velocity dispersion anisotropy, we compared the results based on the Jeans equations with those obtained by assuming a specific form of the galaxy distribution function incorporating the picture of violent relaxation, where the total gravitational potential is imposed as set by the available gravitational lensing observations. Results. We find evidence of systematic rotation in both clusters, with significant rotation in each core (within 0.5′ from the center) and no signatures of rotation at large radii. While no signs of energy equipartition were found, there is a clear indication of (stellar) mass segregation. Velocity dispersion anisotropy is present and qualitatively similar to what has been found in violently relaxed collisionless systems. This last conclusion is strengthened by the overall success in matching the observations with the predictions of the physically justified distribution function.

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Gas rotation and dark matter halo shape in cool-core clusters of galaxies

Bartalesi,

Ettori,

Nipoti

2024

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We study the possibility that the gas in cool-core clusters of galaxies has non-negligible rotation support, the impact of gas rotation on mass estimates from current X-ray observations, and the ability of forthcoming X-ray observatories to detect such rotation. We present three representative models of massive cool-core clusters with a rotating intracluster medium (ICM) in equilibrium in cosmologically motivated spherical, oblate, or prolate dark matter halos, represented by physical density-potential pairs. In the models, the gas follows a composite-polytropic distribution, and has rotation velocity profiles consistent with current observational constraints and similar to those found in clusters formed in cosmological simulations. We show that the models are consistent with available measurements of the ICM properties of the massive cluster population: the thermodynamic profiles, the shape of the surface brightness distribution, the hydrostatic mass bias, and the broadening of X-ray emitting lines. Using the configuration for the microcalorimeter onboard the XRISM satellite, we generated a set of mock X-ray spectra for our cluster models, which we then analyzed to make predictions about the rotation speed that will be obtained with such an instrument. We then assessed what fraction of the hydrostatic mass bias of our models could be accounted for by detecting the rotation speed with XRISM spectroscopy over the range $(0.1-1)r_ $, sampled with three nonoverlapping pointings. Current data leave room for the rotating ICM in cool-core clusters, with peaks in the rotation speed as high as $600\ km/s $. We show that such rotation, if present, will be detected with upcoming X-ray facilities such as XRISM and that $60-70<!PCT!>$ of the hydrostatic mass bias due to rotation can be accounted for using the line-of-sight velocity measured from X-ray spectroscopy with XRISM with a residual bias smaller than $3<!PCT!>$ at an overdensity of 500. In this way XRISM will allow us to pin down any mass bias of a different origin from the rotation.

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Testing the rotation versus merger scenario in the galaxy cluster Abell 2107

Cited by 5 publications

References 43 publications

X-ray analysis of JWST’s first galaxy cluster lens SMACS J0723.3−7327

X-ray analysis of JWST’s first galaxy cluster lens SMACS J0723.3−7327

Dynamics of the galactic component of Abell S1063 and MACS J1206.2−0847

Gas rotation and dark matter halo shape in cool-core clusters of galaxies

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