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J/A+A/546/A6        Metal abundances of galaxy clusters          (Andreon, 2012)

The enrichment history of the intracluster medium: a Bayesian approach. Anfreon S. <Astron. Astrophys. 546, A6 (2012)> =2012A&A...546A...6A
ADC_Keywords: Clusters, galaxy ; Redshifts ; Abundances Keywords: galaxies: clusters: general - galaxies: clusters: intracluster medium - X-ray: diffuse background - methods: statistical Abstract: This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1<z<1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 47 130 Id, Redshift, metal abundances, temperatures, and their σ values, and data source (zero for Chandra, one for XMM--Newton)
See also: J/ApJS/174/117 : Properties and metal abundances of clusters (Maughan+, 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 17 A17 --- Name Cluster name (1) 19- 23 F5.3 --- z Redshift (1) 25- 29 F5.2 [Sun] Z Metal abundance, modeZ{Fe,i}, in Z_{Fe,☉} units 31- 34 F4.2 [Sun] e_Z rms uncertainty on Z, in Z_{Fe,☉} units 36- 40 F5.2 keV T Temperature, modeTi 42- 45 F4.2 keV e_T rms uncertainty on T 47 I1 --- Ref [0/1] Data source: 0 for Chandra, 1 for XMM-Newton
Note (1): From Maughan et al. (2008, Cat. J/ApJS/174/117) or Anderson et al. (2009ApJ...698..317A).
Acknowledgements: Stefano Andreon, stefano.andreon(at)
(End) Patricia Vannier [CDS] 23-Aug-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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