Planckintermediate results

Abstract

We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal D 2 A Y 500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an M WL −D 2 A Y 500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R 500 are on average ∼20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations.

Interacting dark energy models in Cosmology and large-scale structure observational tests

“…We analyzed the virial ratios of a set of clusters using a simple model based on the Layzer-Irvine equation [106][107][108][109][110][111], using weak-lensing mass profiles and intracluster gas temperatures from optical and X-ray observations [117,118]. Our treatment involved assessing the virial balance of each cluster as well as their equilibrium state, using a Monte Carlo statistical analysis on the data.…”

“…The spectroscopically determined temperatures T X are measured within r 500 and are all given in ref. [118], with the exceptions of A115 and A697 from Landry et al These two NFW parameters are always positive. In order to guarantee that their uncertainties will not lead to negative values in any of the random realizations, we choose the log-logistic distribution, for it being a non-negative probability distribution whose probability density function (PDF) and cumulative distribution function (CDF) have simple analytical forms.…”

“…Cosmologically interesting observations of clusters are produced in many surveys and studies such as Okabe et al [117] and Planck Collaboration [118]. In order to maximize our sample, while being able to separately evaluate from observations the kinetic and potential energy states of each cluster, we have restricted inputs to weak-lensing NFW fit parameters, X-ray derived c 500 NFW fits, and X-ray temperatures.…”

“…Their weak lensing data are shown in table 6.1. We also include four more clusters from Planck Collaboration [118]: A520, A963, A1914 and A2034 (data in table 6.2). Weak lensing masses M 500 and best fitting NFW concentration parameter c 500 are given instead of M vir , c vir and M 200 for these clusters.…”

“…However, the error bars for c 500 were estimated from the X-ray data, since they are not given by ref. [118]. The spectroscopically determined temperatures T X are measured within r 500 and are all given in ref.…”