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A blind detection of a large, complex, Sunyaev--Zel'dovich structure | | AMI Consortium
; T. W. Shimwell
; R. W. Barker
; P. Biddulph
; D. Bly
; R. C. Boysen
; A. R. Brown
; M. L. Brown
; C. Clementson
; M. Crofts
; T. L. Culverhouse
; J. Czeres
; R. J. Dace
; M. L. Davies
; R. D'Alessandro
; P. Doherty
; K. Duggan
; J. A. Ely
; M. Felvus
; F. Feroz
; W. Flynn
; T. M. O. Franzen
; J. Geisbusch
; R. Genova-Santos
; K. J. B. Grainge
; W. F. Grainger
; D. Hammett
; M. P. Hobson
; C. M. Holler
; N. Hurley-Walker
; R. Jilley
; T. Kaneko
; R. Kneissl
; K. Lancaster
; A. N. Lasenby
; P. J. Marshall
; F. Newton
; O. Norris
; I. Northrop
; D. M. Odell
; M. Olamaie
; Y. C. Perrott J. C. Pober
; G. G. Pooley
; M. W. Pospieszalski
; V. Quy
; C. Rodriguez-Gonzalvez
; R. D. E. Saunders
; A. M. M. Scaife
; M. P. Schammel
; J. Schofield
; P. F. Scott
; C. Shaw
; H. Smith
; D. J. Titterington
; M. Velic
; E. M. Waldram
; S. West
; B. A. Wood
; G. Yassin
; J. T. L. Zwart
; | | Date: |
20 Dec 2010 | | Abstract: | We present an interesting Sunyaev-Zel’dovich (SZ) detection in the first of
the Arcminute Microkelvin Imager (AMI) ’blind’, degree-square fields to have
been observed down to our target sensitivity of 100 microJy/beam. In follow-up
deep pointed observations the SZ effect is detected with a maximum peak
decrement greater than 8 times the thermal noise. No corresponding emission is
visible in the ROSAT all-sky X-ray survey and no cluster is evident in the
Palomar all-sky optical survey. Compared with existing SZ images of distant
clusters, the extent is large (approximately 10’) and complex; our analysis
favours a model containing two clusters rather than a single cluster. Our
Bayesian analysis is currently limited to modelling each cluster with an
ellipsoidal (or spherical) beta-model, which does not do justice to this
decrement. Fitting an ellipsoid to the deeper candidate we find the following:
(a) Assuming that the Evrard et al. (2002) approximation to Press & Schechter
(1974) correctly gives the number density of clusters as a function of mass and
redshift, then, in the search area, the probability ratio of the AMI detection
of this cluster is 7.9 x 10^4:1; alternatively assuming Jenkins et al. (2001)
as the true prior, the probability ratio of detection is 2.1 x 10^5:1. (b) The
cluster mass is M200= 5.5 x 10^14 h70^-1Msun. (c) Finally, abandoning modelling
the cluster physically, and instead simply modelling the SZ decrement using a
beta-model, we find a central SZ temperature decrement of -295microK after
allowing for CMB primary anisotropies, receiver noise and sources. We are
unsure if the cluster system we observe is a merging system or two separate
clusters. | | Source: | arXiv, 1012.4441 | | Services: | Forum | Review | PDF | Favorites | |
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