EDP Sciences
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Erratum
This article is an erratum for: [this article]

Issue
A&A
Volume 617, September 2018
Article Number C2
Number of page(s) 2
Section Cosmology (including clusters of galaxies)
DOI https://doi.org/10.1051/0004-6361/201731445e
Published online 25 September 2018

In the Valotti et al. (2018) paper, Figs. 2, 3, and 10 were published at low resolution, resulting in images that are not easy to read. We provide higher-quality figures here in the downloadable pdf.

thumbnail Fig. 2.

X-ray observable diagram computed for a 700 deg2 cluster survey, observed with 10 ks XMM exposures. Panels 1-6: 2D projections of the distribution of the four cluster parameters involved in the present study: CR in [0.5–2] keV, HR1 ([1–2]/[0.5–1] keV), HR2 ([2–5]/[0.5–2]) keV, angular cluster size rc. The diagrams are integrated over the 0 < z < 2 range, but this fifth dimension can be uncompressed if redshifts are available, which significantly increases the cosmological constraining power of the ASpiX method. Error measurements are not implemented in this example.

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thumbnail Fig. 3.

Cumulative dark matter halo number density as a function of mass at different epochs. Blue dots show Aardvark simulations. The pink areas show the mass range encompassed by the C1 selection. The mass scale of 1013.2 M represents the halo mass resolution limit of the simulations.

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thumbnail Fig. 10.

Effects of measurement errors on the C1 CLEAN sample. The plots show from left to right the 2D diagrams CR-HR, CR-rc, and HR-rc. The first row stands for the nominal CR, HR, and rc values stored in the Aardvark catalogues. The second row shows the result of the implementation of the error model displayed in Fig. 9.

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© ESO 2018

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