<i>Suzaku</i>measurement of Abell 2204's intracluster gas temperature profile out to 1800 kpc

Reiprich, T. H.; Hudson, Daniel S.; Zhang, Y.-Y.; Sato, Kosuke; Ishisaki, Yoshitaka; Hoshino, Akio; Ohashi, T.; Ota, Naomi; Fujita, Yutaka

doi:10.1051/0004-6361/200810404

Cited by 105 publications

(113 citation statements)

References 39 publications

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“…Recently Reiprich et al (2009) determined the temperature of this cluster out to ∼r 200 using Suzaku. They find that the temperature declines all the way from 0.3 r 200 to r 200 , consistent with predictions of simulations.…”

Section: C53 A2204mentioning

confidence: 99%

What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limitedHIFLUGCScluster sample

Hudson¹,

Mittal

Reiprich³

et al. 2010

A&A

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429

597

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We use the largest complete sample of 64 galaxy clusters (HIghest X-ray FLUx Galaxy Cluster Sample) with available high-quality X-ray data from Chandra, and apply 16 cool-core diagnostics to them, some of them new. In order to identify the best parameter for characterizing cool-core clusters and quantify its relation to other parameters, we mainly use very high spatial resolution profiles of central gas density and temperature, and quantities derived from them. We also correlate optical properties of brightest cluster galaxies (BCGs) with X-ray properties. To segregate cool core and non-cool-core clusters, we find that central cooling time, t cool , is the best parameter for low redshift clusters with high quality data, and that cuspiness is the best parameter for high redshift clusters. 72% of clusters in our sample have a cool core (t cool < 7.7 h −1/2 71 Gyr) and 44% have strong cool cores (t cool < 1.0 h −1/2 71 Gyr). We find strong cool-core clusters are characterized as having low central entropy and a systematic central temperature drop. Weak cool-core clusters have enhanced central entropies and temperature profiles that are flat or decrease slightly towards the center. Non-cool-core clusters have high central entropies.For the first time we show quantitatively that the discrepancy in classical and spectroscopic mass deposition rates can not be explained with a recent formation of the cool cores, demonstrating the need for a heating mechanism to explain the cooling flow problem. We find that strong cool-core clusters have a distribution of central temperature drops, centered on 0.4T vir . However, the radius at which the temperature begins to drop varies. This lack of a universal inner temperature profile probably reflects the complex physics in cluster cores not directly related to the cluster as a whole. Our results suggest that the central temperature does not correlate with the mass of the BCGs and weakly correlates with the expected radiative cooling only for strong cool-core clusters. Since 88% of the clusters in our sample have a BCG within a projected distance of 50 h −1 71 kpc from the X-ray peak, we argue that it is easier to heat the gas (e.g. with mergers or non-gravitational processes) than to separate the dense core from the brightest cluster galaxy. Diffuse, Mpc-scale radio emission, believed to be associated with major mergers, has not been unambiguously detected in any of the strong cool-core clusters in our sample. Of the weak cool-core clusters and non-cool-core clusters, most of the clusters (seven out of eight) that have diffuse, Mpc-scale radio emission have a large (>50 h −1 71 kpc) projected separation between their BCG and X-ray peak. In contrast, only two of the 56 clusters with a small separation between the BCG and X-ray peak (<50 h −1 71 kpc) show large-scale radio emission. Based on this result, we argue that a large projected separation between the BCG and the X-ray peak is a good indicator of a major merger. The properties of weak cool-core clusters as an intermedi...

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Section: C53 A2204mentioning

confidence: 99%

What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limitedHIFLUGCScluster sample

Hudson¹,

Mittal

Reiprich³

et al. 2010

A&A

Self Cite

429

597

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“…Only a few X-ray observations with XMM-Newton, Chandra and/or Suzaku constrain the density, temperature or gas fraction profiles out to ∼R 200 1.4 R 500 (George et al 2009;Reiprich et al 2009;Urban et al 2011;Simionescu et al 2011;Walker et al 2012). This type of X-ray detection remains very challenging and requires very long exposure times, as at larger radii the X-ray emission is extremely faint.…”

Section: The Outskirtsmentioning

confidence: 99%

“…As already mentioned, X-ray measurements hardly reach density contrasts of ∼200 (e.g., George et al 2009;Reiprich et al 2009;Urban et al 2011;Simionescu et al 2011), so modelling beyond R 200 only relies on predictions from numerical simulations. We used our Planck and XMM-Newton derived pressure profile to investigate the average gas mass fraction distribution across our sample.…”

Section: Constraint On the Gas Mass Fractionmentioning

confidence: 99%

“…Observations with X-ray telescopes have only recently started to provide insight into the physical properties of the gas in the cluster outskirts beyond R 500 (George et al 2009;Reiprich et al 2009;Urban et al 2011). The steep decline of the X-ray emission with cluster-centric radius makes such observations extremely challenging with current instruments.…”

Section: Introductionmentioning

confidence: 99%

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Planckintermediate results

Ade

Aghanim

Arnaud

et al. 2013

A&A

291

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Taking advantage of the all-sky coverage and broad frequency range of the Planck satellite, we study the Sunyaev-Zeldovich (SZ) and pressure profiles of 62 nearby massive clusters detected at high significance in the 14-month nominal survey. Careful reconstruction of the SZ signal indicates that most clusters are individually detected at least out to R 500 . By stacking the radial profiles, we have statistically detected the radial SZ signal out to 3 × R 500 , i.e., at a density contrast of about 50-100, though the dispersion about the mean profile dominates the statistical errors across the whole radial range. Our measurement is fully consistent with previous Planck results on integrated SZ fluxes, further strengthening the agreement between SZ and X-ray measurements inside R 500 . Correcting for the effects of the Planck beam, we have calculated the corresponding pressure profiles. This new constraint from SZ measurements is consistent with the X-ray constraints from XMM-Newton in the region in which the profiles overlap (i.e., [0.1-1] R 500 ), and is in fairly good agreement with theoretical predictions within the expected dispersion. At larger radii the average pressure profile is slightly flatter than most predictions from numerical simulations. Combining the SZ and X-ray observed profiles into a joint fit to a generalised pressure profile gives best-fit parameters [P 0 , c 500 , γ, α, β] = [6.41, 1.81, 0.31, 1.33, 4.13]. Using a reasonable hypothesis for the gas temperature in the cluster outskirts we reconstruct from our stacked pressure profile the gas mass fraction profile out to 3 R 500 . Within the temperature driven uncertainties, our Planck constraints are compatible with the cosmic baryon fraction and expected gas fraction in halos. Key words. cosmology: observations -galaxies: clusters: general -galaxies: clusters: intracluster medium -submillimeter: general -X-rays: general Appendices are available in electronic form at

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“…Reiprich et al (2008) determined the temperature profile for the rich, massive, cooling core cluster Abell 2204 from ∼10 to 1,800 kpc, close to the estimated r 200 . They find that the temperature profile between 0.3 and 1.0r 200 is consistent with a drop of 0.6, as predicted by simulations.…”

Section: At and Beyond The Virial Radiusmentioning

confidence: 52%

X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories

Böhringer

Werner

2009

Astron Astrophys Rev

195

142

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Galaxy clusters, the largest clearly defined objects in our Universe, are ideal laboratories to study in detail the cosmic evolution of the intergalactic intracluster medium (ICM) and the cluster galaxy population. For the ICM, which is heated to X-ray radiating temperatures, X-ray spectroscopy is the most important tool to obtain insight into the structure and astrophysics of galaxy clusters. The ICM is also the hottest plasma that can be well studied under thermal equilibrium conditions. In this review we recall the basic principles of the interpretation of X-ray spectra from a hot, tenuous plasma and we illustrate the wide range of scientific applications of X-ray spectroscopy. The determination of galaxy cluster masses, the most important prerequisite for using clusters in cosmological studies, rest crucially on a precise spectroscopic determination of the ICM temperature distribution. The study of the thermal structure of the ICM provides a very interesting fossil record of the energy release during galaxy formation and evolution, giving important constraints on galaxy formation models. The temperature and pressure distribution of the ICM gives us important insight into the process of galaxy cluster merging and the dissipation of the merger energy in form of turbulent motion. Cooling cores in the centers of about half of the cluster population are interesting laboratories to investigate the interplay between gas cooling, star-and black hole formation and energy feedback, which is diagnosed by means of X-ray spectroscopy. The element abundances deduced from X-ray spectra of the ICM provide a cosmic history record of the contribution of different supernovae to the nucleosynthesis of heavy elements and their spatial distribution partly reflects important transport processes in the ICM. Some discussion of plasma diagnostics for conditions out of thermal equilibrium and an outlook on the future prospects of X-ray spectroscopic cluster studies complete our review.

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Suzakumeasurement of Abell 2204's intracluster gas temperature profile out to 1800 kpc

Cited by 105 publications

References 39 publications

What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limitedHIFLUGCScluster sample

What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limitedHIFLUGCScluster sample

Planckintermediate results

X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories

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