Issue |
A&A
Volume 525, January 2011
|
|
---|---|---|
Article Number | A139 | |
Number of page(s) | 11 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361/201013999 | |
Published online | 09 December 2010 |
The galaxy cluster YSZ−LX and YSZ−M relations from the WMAP 5-yr data
1
DSM/Irfu/SPP, CEA/Saclay, 91191
Gif-sur-Yvette Cedex,
France
e-mail: jean-baptiste.melin@cea.fr
2
APC – Université Paris Diderot, 10 rue Alice Domon et Léonie Duquet,
75205
Paris Cedex 13,
France
e-mail: bartlett@apc.univ-paris7.fr
3
APC – CNRS, 10
rue Alice Domon et Léonie Duquet, 75205
Paris Cedex 13,
France
e-mail: delabrouille@apc.univ-paris7.fr
4
DSM/Irfu/SAp, CEA/Saclay, 91191
Gif-sur-Yvette Cedex,
France
e-mail: monique.arnaud@cea.fr; rocco.piffaretti@cea.fr; gabriel.pratt@cea.fr
Received:
6
January
2010
Accepted:
21
October
2010
We use multifrequency matched filters to estimate, in the WMAP 5-year data, the Sunyaev-Zel’dovich (SZ) fluxes of 893 ROSAT NORAS/REFLEX clusters spanning the luminosity range LX,[0.1−2.4] keV = 2 × 1041−3.5 × 1045 erg s-1. The filters are spatially optimised by using the universal pressure profile recently obtained from combining XMM-Newton observations of the REXCESSsample and numerical simulations. Although the clusters are individually only marginally detected, we are able to firmly measure the SZ signal (>10σ) when averaging the data in luminosity/mass bins. The comparison between the bin-averaged SZ signal versus luminosity and X-ray model predictions shows excellent agreement, implying that there is no deficit in SZ signal strength relative to expectations from the X-ray properties of clusters. Using the individual cluster SZ flux measurements, we directly constrain the Y500−LX and Y500−M500 relations, where Y500 is the Compton y-parameter integrated over a sphere of radius r500. The Y500−M500 relation, derived for the first time in such a wide mass range, has a normalisation at M500 = 3 × 1014 h-1 M⊙, in excellent agreement with the X-ray prediction of 1.54 × 10-3 arcmin2, and a mass exponent of α = 1.79 ± 0.17, consistent with the self-similar expectation of 5/3. Constraints on the redshift exponent are weak due to the limited redshift range of the sample, although they are compatible with self-similar evolution.
Key words: cosmology: observations / galaxies: clusters: general / galaxies: clusters: intracluster medium / cosmic background radiation / X-rays: galaxies: clusters
© ESO, 2010
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