Mass Profiles of Galaxy Clusters from X-ray Analysis

Ettori, S.; Donnarumma, Annamaria; Pointecouteau, É.; Reiprich, T. H.; Giodini, S.; Lovisari, Lorenzo; Schmidt, Robert W.

doi:10.1007/s11214-013-9976-7

Cited by 170 publications

(134 citation statements)

References 233 publications

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“…The method to reconstruct K(r) and P (r) Amodeo et al (2016) presented the method applied to constrain the mass distribution of the galaxy clusters in our sample under the assumption that a spherically symmetric ICM is in hydrostatic equilibrium with the underlying dark matter potential. The backward method adopted (see Ettori et al 2013) allows to constrain the parameters of a mass model, i.e. the concentration and the scale radius for a NFW model (Navarro et al 1997), using both the gas density profile, obtained from the geometrical deprojection of the X-ray surface brightness profile, and the spatially resolved spectroscopic measurements of the gas temperature.…”

Section: Sample Propertiesmentioning

confidence: 99%

On the evolution of the entropy and pressure profiles in X-ray luminous galaxy clusters atz> 0.4

Ghirardini

Ettori

Amodeo

et al. 2017

A&A

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Context. Galaxy clusters are the most recent products of hierarchical accretion over cosmological scales. The gas accreted from the cosmic field is thermalized inside the cluster halo. Gas entropy and pressure are expected to have a self-similar behaviour with their radial distribution following a power law and a generalized Navarro-Frenk-White profile, respectively. This has been shown also in many different hydrodynamical simulations. Aims. We derive the spatially-resolved thermodynamical properties of 47 X-ray galaxy clusters observed with Chandra in the redshift range 0.4 < z < 1.2, one of the largest sample investigated so far with X-ray spectroscopy and with mass reconstructed using hydrostatic equilibrium equation, with a particular care in reconstructing the gas entropy and pressure radial profiles. We search for deviation from the self-similar behaviour and look for possible evolution with redshift. Methods. Under the assumption of a spherically symmetric distribution of the intracluster plasma, we combine the deprojected gas density and the deprojected spectral temperature profiles via the hydrostatic equilibrium equation in order to constrain the concentration and the scale radius, which are the parameters that describe a Navarro-Frenk-White profile for each of the cluster in our sample. The temperature profile, that combined with the observed gas density profile reproduces the best-fit mass model, is then used to reconstruct the profiles of the entropy and pressure. These profiles cover a median radial interval of [0.04 R500 -0.76 R500]. After interpolating on the same radial grid and partially extrapolating up to R500, these profiles are then stacked in order to increase the precision of the analysis, also in 3 independent redshift bins. The gas mass fraction is then used in order to improve the self-similar behaviour of the profiles, by reducing the scatter among the profiles by a factor 3. Results. The entropy and pressure profiles lie very close to the baseline prediction from gravitational structure formation. We show that these profiles deviate from the baseline prediction as function of redshift, in particular at z > 0.75, where, in the central regions, we observe higher values of the entropy (by a factor of ∼ 2.2) and systematically lower estimates (by a factor of ∼ 2.5) of the pressure. The effective polytropic index, which retains informations about the thermal distribution of the gas, shows a slight linear positive evolution with the redshift and the concentration of the dark matter distribution. A prevalence of non-cool-core, disturbed systems, as we observe at higher redshifts, can explain such behaviours.

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Section: Sample Propertiesmentioning

confidence: 99%

On the evolution of the entropy and pressure profiles in X-ray luminous galaxy clusters atz> 0.4

Ghirardini

Ettori

Amodeo

et al. 2017

A&A

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“…Even more difficult is the estimate of clusters masses and mass profiles that are biased by various effects depending on the applied methods. The masses inferred from either X-ray (e.g., Ettori et al 2013;Maughan et al 2016) or optical data are, for example, based on the assumption of dynamical equilibrium, while those obtained by gravitational lensing (e.g., Umetsu et al 2014;Merten et al 2015) require a good knowledge of the geometry of the potential well. Discrepancies by a factor of 2-3 between the masses obtained by various methods have been reported (e.g., Wu & Fang 1997).…”

Section: Introductionmentioning

confidence: 99%

Characterization of Omega-WINGS galaxy clusters

Cariddi

D’Onofrio

Fasano

et al. 2018

A&A

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Context. Galaxy clusters are the largest virialized structures in the observable Universe. Knowledge of their properties provides many useful astrophysical and cosmological information. Aims. Our aim is to derive the luminosity and stellar mass profiles of the nearby galaxy clusters of the Omega-WINGS survey and to study the main scaling relations valid for such systems. Methods. We merged data from the WINGS and Omega-WINGS databases, sorted the sources according to the distance from the brightest cluster galaxy (BCG), and calculated the integrated luminosity profiles in the B and V bands, taking into account extinction, photometric and spatial completeness, K correction, and background contribution. Then, by exploiting the spectroscopic sample we derived the stellar mass profiles of the clusters. Results. We obtained the luminosity profiles of 46 galaxy clusters, reaching r 200 in 30 cases, and the stellar mass profiles of 42 of our objects. We successfully fitted all the integrated luminosity growth profiles with one or two embedded Sérsic components, deriving the main clusters parameters. Finally, we checked the main scaling relation among the clusters parameters in comparison with those obtained for a selected sample of early-type galaxies (ETGs) of the same clusters. Conclusions. We found that the nearby galaxy clusters are non-homologous structures such as ETGs and exhibit a color-magnitude (CM) red-sequence relation very similar to that observed for galaxies in clusters. These properties are not expected in the current cluster formation scenarios. In particular the existence of a CM relation for clusters, shown here for the first time, suggests that the baryonic structures grow and evolve in a similar way at all scales.

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“…This result can be primarily attributed to an additional pressure support provided by the bulk motions in the ICM. The departure from the hydrostatic assumption is one of the largest sources of systematic uncertainties in cluster cosmology (e.g., Lau et al 2009;Rasia et al 2012;Ettori et al 2013). …”

Section: Introductionmentioning

confidence: 99%

Search for gas bulk motions in eight nearby clusters of galaxies with Suzaku

Ota

Yoshida

2016

Publications of the Astronomical Society of Japan

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To search for bulk motions of the intracluster medium, we analyzed the X-ray spectra taken with the Suzaku satellite and measured the Doppler shift of Fe-K line emission from eight nearby clusters of galaxies with various X-ray morphologies. In the cores of the Centaurus and Perseus clusters, the gas bulk velocity does not exceed the sound velocity, which confirms the results of previous research. For the Cen45 subcluster, we found that the radial velocity relative to the Centaurus core, < 780 km s −1 , is significantly smaller than that reported in the optical band at the 3.9σ level, which suggests an offset between the gas and galaxy distributions along the line of sight due to the subcluster merger. In A2199, A2142, A3667, and A133, no significant bulk motion was detected, indicating an upper limit on the radial velocity of 3000 − 4000 km s −1 . A sign of large bulk velocity in excess of the instrumental calibration uncertainty was found near the center of cool-core cluster A2029 and in the subcluster of the merging cluster A2255, suggesting that the nonthermal pressure support is not negligible in estimating the total gravitational mass of not only merging clusters but also relaxed clusters as predicted by numerical simulations. To improve the significance of the detection, however, a further examination by follow-up observations is required. The present study provides a pilot survey prior to the future high-resolution spectroscopy with ASTRO-H, which is expected to play a critical role in revealing the dynamical evolutions of clusters.

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Mass Profiles of Galaxy Clusters from X-ray Analysis

Abstract: We review the methods adopted to reconstruct the mass profiles in X-ray luminous galaxy clusters. We discuss the limitations and the biases affecting these measurements and how these mass profiles can be used as cosmological proxies.

Cited by 170 publications

References 233 publications

On the evolution of the entropy and pressure profiles in X-ray luminous galaxy clusters atz> 0.4

On the evolution of the entropy and pressure profiles in X-ray luminous galaxy clusters atz> 0.4

Characterization of Omega-WINGS galaxy clusters

Search for gas bulk motions in eight nearby clusters of galaxies with Suzaku

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