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

Issue
A&A
Volume 574, February 2015
Article Number C1
Number of page(s) 2
Section Cosmology (including clusters of galaxies)
DOI https://doi.org/10.1051/0004-6361/201322450e
Published online 16 January 2015

The pseudo phase-space density profile of Abell 2142, defined with the galaxy number density profile ν instead of the cluster mass density profile ρ, was shown in Fig. 12 of Munari et al. (2014). This graph was erroneous (because we had incorrectly considered the projected number density profile instead of the 3D profile). The correct figure is shown below. The values in Table 4 are changed, and the correct ones are reported in the table below.

thumbnail Fig. 12

Same as Fig. 10 of Munari et al. (2014), but now using the radial profiles of galaxy number density instead of total mass density to estimate the PPSD.

Open with DEXTER

Table 4

Best-fit parameters of the PPSD profile.

While Fig. 12 of Munari et al. (2014) indicated that the PPSDs computed with the number density profile are significantly shallower than the theoretical relation of Dehnen & McLaughlin (2005), the corrected version of the figure shown here indicates that the PPSDs computed with the number density profile are now either consistent with the relation of Dehnen & McLaughlin (Q(r) for BLUE sample) or only slightly shallower, but not less consistent with that relation than found for the PPSDs computed with the mass density profile.

Therefore, the statement in Munari et al. (2014) that the mass density profile represents the PPSD and βγ relations better is no longer correct. Indeed, Figs. 11 and 13 of Munari et al. show that the βγ relations obtained using the mass density or tracer number density are indistinguishable for the RED and ALL samples. And therefore, the entire discussion of the greater relevance of the mass density profile relative to the galaxy number density profile must be dismissed.

References


© ESO, 2015

All Tables

Table 4

Best-fit parameters of the PPSD profile.

All Figures

thumbnail Fig. 12

Same as Fig. 10 of Munari et al. (2014), but now using the radial profiles of galaxy number density instead of total mass density to estimate the PPSD.

Open with DEXTER
In the text

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