Publications by Philip James Marshall


A blind detection of a large, complex, Sunyaev-Zel'dovich structure

Monthly Notices of the Royal Astronomical Society 423 (2012) 1463-1473

TW Shimwell, RW Barker, P Biddulph, D Bly, RC Boysen, AR Brown, ML Brown, C Clementson, M Crofts, TL Culverhouse, J Czeres, RJ Dace, ML Davies, R D'Alessandro, P Doherty, K Duggan, JA Ely, M Felvus, F Feroz, W Flynn, TMO Franzen, J Geisbüsch, R Génova-Santos, KJB Grainge, WF Grainger, D Hammett, MP Hobson, CM Holler, N Hurley-Walker, R Jilley, T Kaneko, R Kneissl, K Lancaster, AN Lasenby, PJ Marshall, F Newton, O Norris, I Northrop, DM Odell, M Olamaie, YC Perrott, JC Pober, GG Pooley, MW Pospieszalski, V Quy, C Rodríguez-Gonzálvez, RDE Saunders, AMM Scaife, MP Schammel, J Schofield, PF Scott, C Shaw, H Smith, DJ Titterington, M Velić, EM Waldram, S West, BA Wood, G Yassin, JTL Zwart

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. In follow-up deep pointed observations the SZ effect is detected with a maximum peak decrement greater than eight 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 (≈10arcmin) 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 β 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. approximation to Press & Schechter correctly gives the number density of clusters as a function of mass and redshift, then, in the search area, the formal Bayesian probability ratio of the AMI detection of this cluster is 7.9 × 10 4 :1; alternatively assuming Jenkins et al. as the true prior, the formal Bayesian probability ratio of detection is 2.1 × 10 5 :1. (b) The cluster mass is (c) Abandoning a physical model with number density prior and instead simply modelling the SZ decrement using a phenomenological β model of temperature decrement as a function of angular distance, we find a central SZ temperature decrement of K - this allows for cosmic microwave background primary anisotropies, receiver noise and radio sources. We are unsure if the cluster system we observe is a merging system or two separate clusters. © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS.


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