The enrichment history of the intracluster medium: a Bayesian approach

Andreon, S.

doi:10.1051/0004-6361/201219194

Cited by 37 publications

(41 citation statements)

References 35 publications

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“…We use the method of Andreon (2012) to convert the generally asymmetric errors reported by XSPEC into a log-normal likelihood. We note that the errors on the temperature given in Table 1 are those reported by XSPEC.…”

Section: Resultsmentioning

confidence: 99%

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The XXL Survey

Giles

Maughan

Pacaud

et al. 2016

A&A

103

102

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Context. The XXL Survey is the largest homogeneous survey carried out with XMM-Newton. Covering an area of 50 deg 2 , the survey contains several hundred galaxy clusters out to a redshift of ∼2 above an X-ray flux limit of ∼5 × 10 −15 erg cm −2 s −1 . This paper belongs to the first series of XXL papers focusing on the bright cluster sample. Aims. We investigate the luminosity-temperature (LT) relation for the brightest clusters detected in the XXL Survey, taking fully into account the selection biases. We investigate the form of the LT relation, placing constraints on its evolution. Methods. We have classified the 100 brightest clusters in the XXL Survey based on their measured X-ray flux. These 100 clusters have been analysed to determine their luminosity and temperature to evaluate the LT relation. We used three methods to fit the form of the LT relation, with two of these methods providing a prescription to fully take into account the selection effects of the survey. We measure the evolution of the LT relation internally using the broad redshift range of the sample. Results. Taking fully into account selection effects, we find a slope of the bolometric LT relation of B LT = 3.08±0.15, steeper than the self-similar expectation (B LT = 2). Our best-fit result for the evolution factor is E(z)1.64±0.77 , fully consistent with "strong self-similar" evolution where clusters scale self-similarly with both mass and redshift. However, this result is marginally stronger than "weak selfsimilar" evolution, where clusters scale with redshift alone. We investigate the sensitivity of our results to the assumptions made in our fitting model, finding that using an external LT relation as a low-z baseline can have a profound effect on the measured evolution. However, more clusters are needed in order to break the degeneracy between the choice of likelihood model and mass-temperature relation on the derived evolution.

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Section: Resultsmentioning

confidence: 99%

“…Andreon 2012). We scale the luminosity of each point by E(z) γ LT for the value of γ LT currently considered and use the modified χ 2 described in Press et al (1986), which includes the uncertainties in both L and T .…”

Section: Posterior Predictive Checksmentioning

confidence: 99%

The XXL Survey

Giles

Maughan

Pacaud

et al. 2016

A&A

103

102

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“…Furthermore, the slope depicted in Fig. 3 is not "too shallow" compared to the data, a steeper slope would systematically over-or underestimate the cluster richness (see Andreon & Hurn 2010, 2012 for a brief astronomical introduction on regression fitting).…”

Section: Side Commentsmentioning

confidence: 98%

Richness-mass relation self-calibration for galaxy clusters

Andreon

Bergé

2012

A&A

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This work attains a threefold objective: first, we derived the richness-mass scaling in the local Universe from data of 53 clusters with individual measurements of mass. We found a 0.46 ± 0.12 slope and a 0.25 ± 0.03 dex scatter measuring richness with a previously developed method. Second, we showed on a real sample of 250 0.06 < z < 0.9 clusters, most of which are at z < 0.3, with spectroscopic redshift that the colour of the red sequence allows us to measure the clusters' redshift to better than Δz = 0.02. Third, we computed the predicted prior of the richness-mass scaling to forecast the capabilities of future wide-field-area surveys of galaxy clusters to constrain cosmological parameters. To this aim, we generated a simulated universe obeying the richness-mass scaling that we found. We observed it with a PanStarrs 1+Euclid-like survey, allowing for intrinsic scatter between mass and richness, for errors on mass, on richness, and for photometric redshift errors. We fitted the observations with an evolving five-parameter richness-mass scaling with parameters to be determined. Input parameters were recovered, but only if the cluster mass function and the weak-lensing redshift-dependent selection function were accounted for in the fitting of the mass-richness scaling. This emphasizes the limitations of often adopted simplifying assumptions, such as having a mass-complete redshift-independent sample. We derived the uncertainty and the covariance matrix of the (evolving) richness-mass scaling, which are the input ingredients of cosmological forecasts using cluster counts. We find that the richness-mass scaling parameters can be determined 10 5 times better than estimated in previous works that did not use weak-lensing mass estimates, although we emphasize that this high factor was derived with scaling relations with different parameterizations. The better knowledge of the scaling parameters likely has a strong impact on the relative importance of the different probes used to constrain cosmological parameters. The fitting code used for computing the predicted prior, including the treatment of the mass function and of the weak-lensing selection function, is provided in Appendix A. It can be re-used, for example, to derive the predicted prior of other observable-mass scalings, such as the L X -mass relation.

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“…A few others have constrained the evolution of the metal abundance at z > ∼ 0.3 (e.g. Balestra et al 2007;Maughan et al 2008;Anderson et al 2009; a statistical analysis of the combination of these different data sets is presented in Andreon 2012). In Baldi et al (2012a), we have presented Article published by EDP Sciences A46, page 1 of 5 the XMM-Newton analysis of 39 galaxy clusters at 0.4 < z < 1.4, covering a temperature range of 2 < ∼ kT < ∼ 12.8 keV.…”

Section: Introductionmentioning

confidence: 99%

The evolution of the spatially resolved metal abundance in galaxy clusters up toz= 1.4

Ettori

Baldi

Balestra

et al. 2015

A&A

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Context. We present the combined analysis of the metal content of 83 objects in the redshift range 0.09−1.39, and spatially resolved in the three bins (0−0.15, 0.15−0.4, >0.4) R 500 , as obtained with similar analysis using XMM-Newton data in our previous two papers. Aims. By combining these two large data sets, we investigate the relations between abundance, temperature, radial position and redshift holding in the intracluster medium. Methods. We fit functional forms to the combination of the different physical quantities of interest, i.e., intracluster medium (ICM) metal abundance, radius, and redshift. We use the pseudo-entropy ratio to separate the cool core (CC) cluster population, where the central gas density tends to be relatively higher, cooler and more metal rich, from the non-cool core systems. Results. The average, redshift-independent, metal abundance measured in the three radial bins decreases moving outwards, with a mean metallicity in the core that is even three (two) times higher than the value of 0.16 times the solar abundance in Anders & Grevesse (1989, Geochim. Cosmochim. Acta, 53, 197) estimated at r > 0.4 R 500 in CC (NCC) objects. We find that the values of the emission-weighted metallicity are well fitted by the relation Z(z) = Z 0 (1 + z) −γ at the given radius. A significant scatter, intrinsic to the observed distribution and of the order of 0.05−0.15, is observed below 0.4 R 500 . The nominal best-fit value of γ is significantly different from zero (>3σ) in the inner cluster regions (γ = 1.6 ± 0.2) and in CC clusters only. These results are also confirmed with a bootstrap analysis, which provides a still significant negative evolution in the core of CC systems (P > 99.9 per cent, when counting the number of random repetitions, which yields γ > 0). No redshift evolution is observed when regions above the core (r > 0.15 R 500 ) are considered. A reasonable good fit of both the radial and redshift dependence is provided from the functional form Z(r, z) = Z 0 (1 + (r/0.15 R 500 ) 2 ) −β (1 + z) −γ , with (Z 0 , β, γ) = (0.83 ± 0.13, 0.55 ± 0.07, 1.7 ± 0.6) in CC clusters and (0.39 ± 0.04, 0.37 ± 0.15, 0.5 ± 0.5) for NCC systems. Conclusions. Our results represent the most extensive study of the spatially resolved metal distribution in the cluster plasma as function of redshift. Our study defines the limits that numerical and analytic models describing the metal enrichment in the ICM have to meet.

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The enrichment history of the intracluster medium: a Bayesian approach

Cited by 37 publications

References 35 publications

The XXL Survey

The XXL Survey

Richness-mass relation self-calibration for galaxy clusters

The evolution of the spatially resolved metal abundance in galaxy clusters up toz= 1.4

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