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A VSA search for the extended Sunyaev-Zel'dovich Effect in the Corona Borealis Supercluster | | Ricardo Genova-Santos
; Jose Alberto Rubino-Martin
; Rafael Rebolo
; Kieran Cleary
; Rod D. Davies
; Richard J. Davis
; Clive Dickinson
; Nelson Falcon
; Keith Grainge
; Carlos M. Gutierrez
; Michael P. Hobson
; Michael E. Jones
; Ruediger Kneissl
; Katy Lancaster
; Carmen P. Padilla-Torres
; Richard D.E. Saunders
; Paul F. Scott
; Angela C. Taylor & Robert A. Watson
; | | Date: |
12 Jul 2005 | | Subject: | astro-ph | | Abstract: | We present interferometric imaging at 33 GHz of the Corona Borealis supercluster, using the extended configuration of the Very Small Array. A total area of 24 deg^2 has been imaged, with an angular resolution of 11 arcmin and a sensitivity of 12 mJy/beam. The aim of these observations is to search for Sunyaev-Zel’dovich (SZ) detections from known clusters of galaxies in this supercluster and for a possible extended SZ decrement due to diffuse warm/hot gas in the intercluster medium. We measure negative flux values in the positions of the ten richest clusters in the region. Collectively, this implies a 3.0-sigma detection of the SZ effect. In the clusters A2061 and A2065 we find decrements of approximately 2-sigma. Our main result is the detection of two strong and resolved negative features at -70+-12 mJy/beam (-157+-27 microK) and -103+-10 mJy/beam (-230+-23 microK), respectively, located in a region with no known clusters, near the centre of the supercluster. We discuss their possible origins in terms of primordial CMB anisotropies and/or SZ signals related to either unknown clusters or to a diffuse extended warm/hot gas distribution. Our analyses have revealed that a primordial CMB fluctuation is a plausible explanation for the weaker feature (probability of 37.82%). For the stronger one, neither primordial CMB (probability of 0.33%) nor SZ can account alone for its size and total intensity. The most reasonable explanation, then, is a combination of both primordial CMB and SZ signal. Finally, we explore what characteristics would be required for a filamentary structure consisting of warm/hot diffuse gas in order to produce a significant contribution to such a spot taking into account the constraints set by X-ray data. | | Source: | arXiv, astro-ph/0507285 | | Services: | Forum | Review | PDF | Favorites | |
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