On the Presence of Thermal SZ Induced Signal in the First Year WMAP Temperature Maps

Details On the Presence of Thermal SZ Induced Signal in the First Year WMAP Temperature Maps On the Presence of Thermal SZ Induced Signal in the First Year WMAP Temperature Maps

2003-05-30

arxiv.org/abs/astro-ph/0305606v2

Mon.Not.Roy.Astron.Soc. 347 (2004) 403

Astronomy and Astrophysics

Astrophysics

MNRAS accepted. New section and minor changes included

Scientific paper

10.1111/j.1365-2966.2004.07205.x

Using available optical and X-ray catalogues of clusters and superclusters of galaxies, we build templates of tSZ emission as they should be detected by the WMAP experiment. We compute the cross-correlation of our templates with WMAP temperature maps, and interpret our results separately for clusters and for superclusters of galaxies. For clusters of galaxies, we claim 2-5 $\sigma$ detections in our templates built from BCS Ebeling et al. (1998), NORAS (Boehringer et al. 2000) and de Grandi et al. (1999) catalogues. In these templates, the typical cluster temperature decrements in WMAP maps are around 15-35 $\mu$K in the RJ range (no beam deconvolution applied). Several tests probing the possible influence of foregrounds in our analyses demonstrate that our results are robust against galactic contamination. On supercluster scales, we detect a diffuse component in the V & W WMAP bands which cannot be generated by superclusters in our catalogues (Einasto et al. 1994, 1997), and which is not present in the clean map of Tegmark, de Oliveira-Costa & Hamilton (2003). Using this clean map, our analyses yield, for Einasto's supercluster catalogues, the following upper limit for the comptonization parameter associated to supercluster scales: $y_{SC} < 2.18 \time s 10^{-8}$ at the 95% confidence limit.

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