The Physics of Galaxy Cluster Outskirts

Walker, Stephen; Simionescu, A.; Nagai, Daisuke; Okabe, Nobuhiko; Eckert, D.; Mroczkowski, Tony; Akamatsu, Hiroki; Ettori, S.; Ghirardini, Vittorio

doi:10.1007/s11214-018-0572-8

Cited by 126 publications

(107 citation statements)

References 170 publications

(158 reference statements)

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“…The entropy profile is expected to follow a power law outside of the core; simulations predict it will only turn over beyond R 200 , while a handful of observations, largely of merging systems, show a turnover at and perhaps just interior to R 200 (e.g. Walker et al 2019). Thus, the turnover just before R 500 appears suspect, especially as it only concerns one pressure profile bin.…”

Section: Additional Thermodynamic Profilesmentioning

confidence: 99%

Pressure Profiles and Mass Estimates Using High-resolution Sunyaev–Zel’dovich Effect Observations of Zwicky 3146 with MUSTANG-2

Romero

Sievers

Ghirardini

et al. 2020

ApJ

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The galaxy cluster Zwicky 3146 is a sloshing cool core cluster at z = 0.291 that in X-ray imaging does not appear to exhibit significant pressure substructure in the intracluster medium (ICM). The published M 500 values range between 3.88 +0.62 −0.58 to 22.50 ± 7.58 × 10 14 M , where ICM-based estimates with reported errors < 20% suggest that we should expect to find a mass between 6.53 +0.44 −0.44 × 10 14 M (from Planck, with an 8.4σ detection) and 8.52 +1.77 −1.47 × 10 14 M (from ACT, with a 14σ detection). This broad range of masses is suggestive that there is ample room for improvement for all methods. Here, we investigate the ability to estimate the mass of Zwicky 3146 via the Sunyaev-Zel'dovich (SZ) effect with data taken at 90 GHz by MUSTANG-2 to a noise level better than 15 µK at the center, and a cluster detection of 104σ. We derive a pressure profile from our SZ data which is in excellent agreement with that derived from X-ray data. From our SZ-derived pressure profiles, we infer M 500 and M 2500 via three methods -Y -M scaling relations, the virial theorem, and hydrostatic equilibrium -where we employ X-ray constraints from XMM-Newton on the electron density profile when assuming hydrostatic equilibrium. Depending on the model and estimation method, our M 500 estimates range from 6.23 ± 0.59 to 10.6 ± 0.95 × 10 14 M , where our estimate from hydrostatic equilibrium, is 8.29 +1.93 −1.24 (±19.1% stat) +0.74 −0.68 (±8.6% sys, calibration) ×10 14 M . Our fiducial mass, derived from a Y -M relation is 8.16 +0.44 −0.54 (±5.5% stat) +0.46 −0.43 (±5.5% sys, Y -M ) +0.59 −0.55 (±7.0% sys, cal.) ×10 14 M . We investigate the consistency of our mass estimates and potential for otherwise unaddressed systematic errors within the MUSTANG-2 data. The inconsistencies among our mass estimates are not well explained by a potential systematic error in the MUSTANG-2 data.

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Section: Additional Thermodynamic Profilesmentioning

confidence: 99%

Pressure Profiles and Mass Estimates Using High-resolution Sunyaev–Zel’dovich Effect Observations of Zwicky 3146 with MUSTANG-2

Romero

Sievers

Ghirardini

et al. 2020

ApJ

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“…Cluster outskirts are undoubtedly a region of great interest as they contain most of the cluster volume and provide direct information on how the ICM forms, accretes and contributes to the growth of large scale structures (Walker et al 2019, in this topical collection). Due to the low X-ray surface brightness of these outermost regions, however, metallicity measurements beyond onehalf of their virial radii remain sparse.…”

Section: Metals In Cluster Outskirtsmentioning

confidence: 99%

Enrichment of the Hot Intracluster Medium: Observations

et al. 2018

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Four decades ago, the firm detection of an Fe-K emission feature in the X-ray spectrum of the Perseus cluster revealed the presence of iron in its hot intracluster medium (ICM). With more advanced missions successfully launched over the last 20 years, this discovery has been extended to many other metals and to the hot atmospheres of many other galaxy clusters, groups, and giant elliptical galaxies, as evidence that the elemental bricks of life -synthesized by stars and supernovae -are also found at the largest scales of the Universe. Because the ICM, emitting in X-rays, is in collisional ionisation equilibrium, its elemental abundances can in principle be accurately measured. These abundance measurements, in turn, are valuable to constrain the physics and environmental conditions of the Type Ia and core-collapse supernovae that exploded and enriched the ICM over the entire cluster volume. On the other hand, the spatial distribution of metals across the ICM constitutes a remarkable signature of the chemical history and evolution of clusters, groups, and ellipticals. Here, we summarise the most significant achievements in measuring elemental abundances in the ICM, from the very first attempts up to the era of XMM-Newton, Chandra, and Suzaku and the unprecedented results obtained by Hitomi. We also discuss the current systematic limitations of these measurements and how the future missions XRISM and Athena will further improve our current knowledge of the ICM enrichment.

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“…Nagai et al 2007;Lau et al 2013;Nelson et al 2014a;Shi et al 2016;Biffi et al 2016), and (iii) gas clumping in galaxy cluster outskirts, which biases the density and temperature profile measurements in the outskirts of clusters (e.g. Nagai & Lau 2011;Vazza et al 2013;Rasia et al 2014;Avestruz et al 2016;Walker et al 2019, for a review).…”

Section: Introductionmentioning

confidence: 99%

Probing cosmology and cluster astrophysics with multiwavelength surveys – I. Correlation statistics

Shirasaki

Lau

Nagai

2019

Monthly Notices of the Royal Astronomical Society

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Upcoming multi-wavelength astronomical surveys will soon discover all massive galaxy clusters and provide unprecedented constraints on cosmology and cluster astrophysics. In this paper, we investigate the constraining power of the multi-band cluster surveys, through a joint analysis of three observables associated with clusters of galaxies, including thermal Sunyaev-Zel'dovich (tSZ) effect in cosmic microwave background (CMB), X-ray emission of ionized gas, and gravitational weak lensing effect of background galaxies by the cluster's gravitational potential. We develop a theoretical framework to predict and interpret two-point correlation statistics among the three observables using a semi-analytic model of intracluster medium (ICM) and halo-based approach. In this work, we show that the auto-and cross-angular power spectra in tSZ, X-ray and lensing statistics from upcoming missions (eROSITA, CMB-S4, and LSST) can help break the degeneracy between cosmology and ICM physics. These correlation statistics are less sensitive to selection biases, and are able to probe ICM physics in distant, faint and small clusters that are otherwise difficult to be detected individually. We show that the correlation statistics are able to provide cosmological constraints comparable to the conventional cluster abundance measurements, while constraining cluster astrophysics at the same time. Our results indicate that the correlation statistics can significantly enhance the scientific returns of upcoming multi-wavelength cluster surveys.

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The Physics of Galaxy Cluster Outskirts

Cited by 126 publications

References 170 publications

Pressure Profiles and Mass Estimates Using High-resolution Sunyaev–Zel’dovich Effect Observations of Zwicky 3146 with MUSTANG-2

Pressure Profiles and Mass Estimates Using High-resolution Sunyaev–Zel’dovich Effect Observations of Zwicky 3146 with MUSTANG-2

Enrichment of the Hot Intracluster Medium: Observations

Probing cosmology and cluster astrophysics with multiwavelength surveys – I. Correlation statistics

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