2005MNRAS.363...79G

Query : 2005MNRAS.363...79G

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: 37

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Number of rows : 37
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 5141 2
2 ACO 2005 ClG 14 58 36.94 +27 50 00.6           ~ 37 0
3 BWE 1457+2720 QSO 14 59 39.9192 +27 08 18.800           ~ 6 1
4 ACO 2019 ClG 15 02 57 +27 11.3           ~ 28 0
5 ACO 2022 ClG 15 04 18.34 +28 30 25.5           ~ 95 0
6 7C 150219.6+290607 QSO 15 04 26.6967436608 +28 54 30.546778212   19.01 18.86     ~ 59 1
7 7C 1507+2654 BLL 15 09 39.0196835160 +26 43 00.059230020   19.47 19.14     ~ 20 1
8 SDSS J151420.88+293103.5 QSO 15 14 20.8868625336 +29 31 03.573312096   19.86 19.69     ~ 21 1
9 NVSS J151439+285541 Rad 15 14 39.4419 +28 55 41.169           ~ 6 1
10 ACO 2056 ClG 15 19 12 +28 16.2           ~ 49 0
11 ACO 2059 ClG 15 20.2 +28 54           ~ 17 0
12 ACO 2061 ClG 15 21 19.90 +30 37 13.0           ~ 214 1
13 7C 1520+3154 Bla 15 22 09.99173254 +31 44 14.3819383   20.45 19.89 19.87   ~ 230 1
14 NAME CrB-H-Spot ? 15 22 11.47 +28 54 06.2           ~ 4 0
15 ACO 2065 ClG 15 22 22.7 +27 44 20           ~ 398 0
16 ACO 2067 ClG 15 23 14 +30 54.4           ~ 111 1
17 ACO 2069 ClG 15 24 02.92 +29 53 20.3           ~ 165 0
18 NAME CrB Supercluster SCG 15 25 +29.5           ~ 148 0
19 ACO 2073 ClG 15 25 54.55 +28 27 48.3           ~ 32 0
20 7C 152516.8+312546 Bla 15 27 18.7370223240 +31 15 24.385268844   19.67 19.30 18.6   ~ 69 1
21 ACO 2079 ClG 15 28 04.7 +28 52 40           ~ 138 0
22 NVSS J152852+315725 Rad 15 28 52.7775 +31 57 25.409           ~ 10 1
23 ACO 2083 ClG 15 29 26 +30 44.7           ~ 35 0
24 NVSS J152936+322521 rG 15 29 36.07745 +32 25 21.7830           ~ 5 1
25 NVSS J153120+281910 Rad 15 31 20.7992434763 +28 19 10.920886002           ~ 4 1
26 NVSS J153220+291932 Rad 15 32 20.8859 +29 19 31.609           ~ 6 1
27 ACO 2089 ClG 15 32 36.89 +28 02 10.1           ~ 108 0
28 ACO 2092 ClG 15 33 19.99 +31 09 12.3           ~ 130 0
29 6C 153358+313617 QSO 15 35 59.3481661824 +31 26 30.776690184   19.97 19.79     ~ 9 1
30 NVSS J153857+355709 rG 15 38 57.8320641528 +35 57 09.332963064           ~ 10 1
31 7C 1537+3113 Bla 15 39 16.17432018 +31 04 07.6747584       21.30   ~ 28 1
32 ICRF J153939.1+274438 Bla 15 39 39.13713864 +27 44 38.2113620   19.13 18.76 17.29   ~ 118 1
33 ACO 2112 ClG 15 39 53 +36 17.4           ~ 4 0
34 NVSS J154033+353824 rG 15 40 33.20131 +35 38 23.9505           ~ 4 1
35 ACO 2122 ClG 15 44 55.93 +36 06 05.2           ~ 243 0
36 7C 154447.29+365334.00 QSO 15 46 38.3104478880 +36 44 20.237508564   18.76 18.50     ~ 27 1
37 SDSS J154754.12+351842.2 QSO 15 47 54.12293 +35 18 42.2545           ~ 15 0

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