DeepXMM‐NewtonandChandraObservations of Cl J1226.9+3332: A Detailed X‐Ray Mass Analysis of az= 0.89 Galaxy Cluster

Maughan, Ben; Jones, C.; Jones, Laura; Speybroeck, L. van

doi:10.1086/512669

Cited by 56 publications

(128 citation statements)

References 59 publications

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“…Any cool component in the core is expected to bias downwards the emission-weighted cluster temperature. We have checked the statistical effect of this bias by considering the sample of 90 clusters with temperatures >4 keV for which Maughan et al (2007) obtained from Chandra observations a measure of the temperature both in the range (0−1)R 500 and in the range (0.15−1)R 500 . We obtain a mean T 0.15−1 /T 0−1 of 1.01, with a dispersion of 0.14, suggesting that, even though on average a cool core does not significantly affect the cluster temperature, the scatter in the distribution of the measured temperatures can be high.…”

Section: Comparison With Previous Workmentioning

confidence: 99%

“…To study this effect, we have considered the measurements of the centroid shift for the 43 objects in common with the sample of 90 clusters analysed by Maughan et al (2007) with T gas > 4 keV. We consider as relaxed objects the 18 clusters with a centroid shift lower than the median value of 1.18 × 10 −2 measured over the entire sample of 115 clusters (see their Table 2).…”

Section: Robustness To Systematic Errorsmentioning

confidence: 99%

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The cluster gas mass fraction as a cosmological probe: a revised study

Ettori

Morandi

Tozzi

et al. 2009

A&A

187

237

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Context. We present the analysis of the baryonic content of 52 X-ray luminous galaxy clusters observed with Chandra in the redshift range 0.3-1.273. Aims. Our study aims at resolving the gas mass fraction in these objects to place constraints on the cosmological parameters Ω m , Ω Λ and the ratio between the pressure and density of the dark energy, w. Methods. We deproject the X-ray surface brightness profiles to recover the gas mass profiles and fit a single thermal component to the spectrum extracted from a region around the cluster that maximizes the signal-to-noise ratios in the observation. The measured values of the gas temperature are used to evaluate the temperature profile with a given functional form and to estimate the total gravitating mass in combination with the gas density profiles. These measured quantities are then used to statistically estimate the gas fraction and the fraction of mass in stars. By assuming that galaxy clusters are representative of the cosmic baryon budget, the distribution of the cluster baryon fraction in the hottest (T gas > 4 keV) systems as a function of redshift is used to constrain the cosmological parameters. We discuss how our constraints are affected by several systematic effects, namely the isothermality, the assumed baryon fraction in stars, the depletion parameter and the sample selection. Results. By using only the cluster baryon fraction as a proxy for the cosmological parameters, we obtain that Ω m is very well constrained at the value of 0.35 with a relative statistical uncertainty of 11% (1σ level; w = −1) and a further systematic error of about (−6, +7)%. On the other hand, constraints on Ω Λ (without the prior of flat geometry) and w (using the prior of flat geometry) are definitely weaker due to the presence of greater statistical and systematic uncertainties (of the order of 40 per cent on Ω Λ and greater than 50 per cent on w). If the WMAP 5-year best-fit results are assumed to fix the cosmological parameters, we limit the contributions expected from non-thermal pressure support and ICM clumpiness to be lower than about 10 per cent, also leaving room to accommodate baryons not accounted for either in the X-ray emitting plasma or in stars of the order of 18 per cent of the total cluster baryon budget. This value is lowered to zero for a no-flat Universe with Ω Λ > 0.7.

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Section: Comparison With Previous Workmentioning

confidence: 99%

Section: Robustness To Systematic Errorsmentioning

confidence: 99%

The cluster gas mass fraction as a cosmological probe: a revised study

Ettori

Morandi

Tozzi

et al. 2009

A&A

187

237

View full text Add to dashboard Cite

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“…where we set b = c/0.45 (as suggested in Maughan et al 2007) and therefore we are left with 7 free parameters. This functional form is usually taken to represent the 3D temperature distribution, and projected to be fit to the observed projected temperature profile.…”

Section: Deprojection and Mass Profilementioning

confidence: 99%

DeepChandraobservation of the galaxy cluster WARPJ1415.1+3612 atz=1

Santos

Tozzi

Rosati

et al. 2012

A&A

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Aims. Using the deepest (370 ks) Chandra observation of a high-redshift galaxy cluster, we perform a detailed characterization of the intra-cluster medium (ICM) of WARPJ1415.1+3612 at z = 1.03, particularly its core region. We also explore the connection between the ICM core properties and the radio/optical properties of the brightest cluster galaxy (BCG). Methods. We perform a spatially resolved analysis of the ICM to obtain temperature, metallicity and surface brightness profiles over the 8-400 kpc radial range. We measure the following cool-core diagnostics: central temperature drop, central metallicity excess, central cooling time, and central entropy. Using the deprojected temperature and density profiles, we accurately derive the cluster hydrostatic mass at different overdensities. In addition to the X-ray data, we use archival radio VLA imaging and optical GMOS spectroscopy of the central galaxy to investigate the feedback between the central galaxy and the ICM. Results. Our spatially resolved spectral analysis shows a significant temperature drop from a maximum of 8.0 keV to a projected core value T c = 4.6 ± 0.4 keV, and a remarkably high central iron abundance peak, Z Fe,c = 3.60 +1.50 −0.85 Z , measured within a radius of 12 kpc. We measure M 500 = M(r < R 500 ) = 2.4 ± 0.4 M and a corresponding gas fraction f gas = 0.10 ± 0.02. The central cooling time is shorter than 0.1 Gyr and the entropy K c is equal to 9.9 keV cm 2 . We detect a strong [OII] emission line in the optical spectra of the BCG with an equivalent width of -25 Å, for which we derive a star formation rate within the range 2-8 M yr −1 . The VLA data reveals a central radio source coincident with the BCG with a luminosity L 1.4 GHz = 2.0 × 10 25 W Hz −1 , and a faint one-sided jet-like feature with an extent of ∼80 kpc. We do not find clear evidence for cavities associated to the radio AGN activity. Conclusions. Our analysis shows that WARPJ1415 has a well developed cool-core with ICM properties similar to those found in the local Universe. Its properties and the clear sign of feedback activity found in the central galaxy in the optical and radio bands, show that feedback processes are already established at z ∼ 1 (a lookback time of 7.8 Gyr). In addition, the presence of a strong metallicity peak shows that the central regions have been promptly enriched by star formation processes in the central galaxy already at z > 1. Our results significantly constrain the timescale for the formation and self-stabilization of cool-cores.

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“…RX J1226.9+3332 (Maughan et al 2007): the same quantities were measured in this case: T = 10.4 ± 0.6 keV, z = 0.89 and f X [0.5,2] keV = 3.27 × 10 −13 erg/s/cm 2 (Vikhlinin et al 2009a). Moreover, the observation of the temperature profile, combined with the assumption of hydrostatic equilibrium, enabled a determination of the total mass and gas mass profiles, and thus an estimate of the cluster mass: M 500 = 5.2 +1.0 −0.8 × 10 14 M .…”

Section: Xmm-newton Follow-up Of the New Planck Clustersmentioning

confidence: 99%

ThePlanckSZ Cluster Catalog: expected X-ray properties

Chamballu¹,

Bartlett²,

Melin³

2012

A&A

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Surveys based on the Sunyaev-Zel'dovich (SZ) effect provide a fresh view of the galaxy cluster population, one that is complementary to X-ray surveys. To better understand the relation between these two kinds of survey, we construct an empirical cluster model using scaling relations constrained by current X-ray and SZ data. We apply our model to predict the X-ray properties of the Planck SZ Cluster Catalog (PCC) and compare them to existing X-ray cluster catalogs. We find that Planck should significantly extend the depth of the previous all-sky cluster survey, performed in the early 1990s by the ROSAT satellite, and should be particularly effective at finding hot, massive clusters (T > 6 keV) out to redshift unity. These are rare objects, and our findings suggest that Planck could increase the observational sample at z > 0.6 by an order of magnitude. This would open the way for detailed studies of massive clusters out to these higher redshifts. Specifically, we find that the majority of newly-detected Planck clusters should have X-ray fluxes 10 −13 erg/s/cm 2 < f X [0.5−2 keV] < 10 −12 erg/s/cm 2 , i.e., distributed over the decade in flux just below the ROSAT All Sky Survey limit. This is sufficiently bright for extensive X-ray follow-up campaigns. Once Planck finds these objects, XMM-Newton and Chandra could measure temperatures to 10% for a sample of ∼100 clusters in the range 0.5 < z < 1, a valuable increase in the number of massive clusters studied over this range.

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DeepXMM‐NewtonandChandraObservations of Cl J1226.9+3332: A Detailed X‐Ray Mass Analysis of az= 0.89 Galaxy Cluster

Cited by 56 publications

References 59 publications

The cluster gas mass fraction as a cosmological probe: a revised study

The cluster gas mass fraction as a cosmological probe: a revised study

DeepChandraobservation of the galaxy cluster WARPJ1415.1+3612 atz=1

ThePlanckSZ Cluster Catalog: expected X-ray properties

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