SIMBAD references

2005MNRAS.363...79G - Mon. Not. R. Astron. Soc., 363, 79-92 (2005/October-2)

A Very Small Array search for the extended Sunyaev-Zel'dovich effect in the Corona Borealis supercluster.

GENOVA-SANTOS R., RUBINO-MARTIN J.A., REBOLO R., CLEARY K., DAVIES R.D., DAVIS R.J., DICKINSON C., FALCON N., GRAINGE K., GUTIERREZ C.M., HOBSON M.P., JONES M.E., KNEISSL R., LANCASTER K., PADILLA-TORRES C.P., SAUNDERS R.D.E., SCOTT P.F., TAYLOR A.C. and WATSON R.A.

Abstract (from CDS):

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 deg2 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. Hydrodynamical simulations suggest that a significant part of the missing baryons in the Local Universe may be located in superclusters.

The maps constructed from these observations have a significant contribution from primordial fluctuations. We measure negative flux values in the positions of the 10 richest clusters in the region. Collectively, this implies a 3.0σ detection of the SZ effect. For two of these clusters, A2061 and A2065, we find decrements of approximately 2σ each.

Our main result is the detection of two strong and resolved negative features at -70±12 mJy/beam (-157±27µK) and -103±10 mJy/beam (-230±23µK), respectively, located in a region with no known clusters, near the centre of the supercluster. We discuss their possible origins in terms of primordial cosmic microwave background (CMB) anisotropies and/or SZ signals related either to 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 per cent). For the stronger one, neither primordial CMB (probability of 0.38 per cent) 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.


Abstract Copyright: 2005 RAS

Journal keyword(s): techniques: interferometric - galaxies: clusters: general - cosmic microwave background - cosmology: observations

Simbad objects: 38

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