arXiv:1101.5590v1 [astro-ph.CO] 28 Jan 2011 Mon. Not. R. Astron. Soc. 000, 1–17 (0000) Printed 31 January 2011 (MN L A T E X style file v2.2) Sunyaev-Zel’dovich observations of LoCuSS clusters with the Arcminute Microkelvin Imager: high X-ray luminosity sample ⋆ AMI Consortium: Timothy W. Shimwell 1 †, Carmen Rodr´ ıguez-Gonz´ alvez 1 ‡, Matthew L. Davies 1 , Farhan Feroz 1 , Thomas M. O. Franzen 1 , Keith J. B. Grainge 1,2 , Michael P. Hobson 1 , Natasha Hurley-Walker 1 , Anthony N. Lasenby 1,2 , Malak Olamaie 1 , Guy Pooley 1 , Richard D. E. Saunders 1,2 , Anna M. M. Scaife 3 , Michel P. Schammel 1 , Paul F. Scott 1 , David J. Titterington 1 , Elizabeth M. Waldram 1 1 Astrophysics Group, Cavendish Laboratory, J J Thomson Avenue, Cambridge CB3 0HE 2 Kavli Institute for Cosmology Cambridge, Madingley Road, Cambridge, CB3 0HA 3 Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland Accepted —; received —; in original form 31 January 2011 ABSTRACT We present observations from the Small Array of the Arcminute Microkelvin Imager (AMI) of eight high X-ray luminosity galaxy cluster systems selected from the Local Cluster Sub- structure Survey (LoCuSS) sample. We detect the Sunyaev-Zel’dovich (SZ) effect in seven of these clusters. With the assumptions that galaxy clusters are isothermal, have a density profile described by a spherical β -model and obey the theoretical M-T relation, we are able to derive cluster parameters at r 200 from our SZ data. With the additional assumption of hydrostatic equilibrium we are able to derive parameters at r 500 . We present posterior probability distri- butions for cluster parameters such as mass, radius and temperature (T SZ,MT ). Combining our sample with that of AMI Consortium: Rodr´ ıguez-Gonz´ alvez et al. (2011) and using large- radius X-ray temperature estimates (T X ) from Chandra and Suzaku observations, we find that there is reasonable correspondence between T X and T SZ,MT values at low T X , but that for clus- ters with T X above around 6keV the correspondence breaks down with T X exceeding T SZ,MT ; we stress that this finding is based on just ten clusters. Key words: cosmology: observations - Sunyaev-Zel’dovich – galaxies:clusters – X-ray – cosmic mi- crowave background– galaxies:clusters:individual (Abell 586, Abell 611, Abell 773, Abell 781, Abell 1413, Abell 1758, Zw1454.8+2233 and RXJ1720+2638) 1 INTRODUCTION The Local Cluster Substructure Survey (LoCuSS see Smith et al. 2003, 2005) sample of clusters contains 164 clusters with redshifts between 0.142 and 0.295. The LoCuSS aims to measure the rela- tionship between the structure of galaxy clusters and the evolution of the hot gas and galaxies that inhabit them using gravitational lensing data and other observations spanning the electromagnetic spectrum from the radio to X-ray. Example LoCuSS analysis pa- pers relevant to this work are Marrone et al. (2009) and Zhang et al. (2010). ⋆ We request that any reference to this paper cites ‘AMI Consortium: Shimwell et al. 2011’ † E-mail: tws29@mrao.cam.ac.uk ‡ E-mail: cr384@mrao.cam.ac.uk We have imaged a subset of LoCuSS in the Sunyaev- Zel’dovich (SZ; Sunyaev & Zeldovich 1972) effect with the Ar- cminute Microkelvin Imager (AMI; see e.g. AMI Consortium: Zwart et al. 2008) centred at 16 GHz. The SZ signal arises from the inverse Compton scattering of cosmic microwave background (CMB) photons by the hot cluster plasma (see e.g. Birkinshaw 1999 and Carlstrom, Holder & Reese 2002), with a surface bright- ness that is independent of redshift and dependencies on plasma density and temperature that are different to those for e.g. X-ray bremsstrahlung emission. Hereafter, we assume a concordance ΛCDM cosmology with Ω m = 0.3, Ω Λ = 0.7 and H 0 = 100km s −1 Mpc −1 . The dimensionless Hubble parameters are defined as h X =H 0 /(X km s −1 Mpc −1 ). All coordinates are given at equinox J2000.