Prof Michael Jones: Publications

Deep optical imaging of the field of PC 1643+4631A&B – II. Estimating the colours and redshifts of faint galaxies

Monthly Notices of the Royal Astronomical Society 91̽�� University Press (OUP) 334:2 (2002) 283-296

Authors:

Garret Cotter, Toby Haynes, Joanne C Baker, Michael E Jones, Richard Saunders

Observations of the Sunyaev–Zel'dovich effect in the z=0.78 cluster MS 1137.5+6625

Monthly Notices of the Royal Astronomical Society 91̽�� University Press (OUP) 334:2 (2002) 323-326

Authors:

Garret Cotter, Helen J Buttery, Rhiju Das, Michael E Jones, Keith Grainge, GG Pooley, Richard Saunders

Deep optical imaging of the field of PC 1643+4631A&B - I. Spatial distributions and the counts of faint galaxies

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 334:2 (2002) 262-282

Authors:

T Haynes, G Cotter, JC Baker, S Eales, ME Jones, S Rawlings, R Saunders

Detection of a cosmic microwave background decrement towards a cluster of mJy radio sources

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 331:1 (2002) 1-6

Authors:

G Cotter, HJ Buttery, S Rawlings, S Croft, GJ Hill, P Gay, R Das, N Drory, K Grainge, WF Grainger, ME Jones, GG Pooley, R Saunders

Surveying the sky with the Arcminute Microkelvin Imager: Expected constraints on galaxy cluster evolution and cosmology

Monthly Notices of the Royal Astronomical Society 328:3 (2001) 783-794

Authors:

R Kneissl, ME Jones, R Saunders, VR Eke, AN Lasenby, K Grainge, G Cotter

Abstract:

We discuss prospects for cluster detection via the Sunyaev-Zel'dovich (SZ) effect in a blank field survey with the interferometer array, the Arcminute MicroKelvin Imager (AMI). Clusters of galaxies selected in the SZ effect probe cosmology and structure formation with little observational bias, because the effect measures integrated gas pressure directly, and does so independently of cluster redshift. We use hydrodynamical simulations in combination with the Press-Schechter expression to simulate SZ cluster sky maps. These are used with simulations of the observation process to gauge the expected SZ cluster counts. Even with a very conservative choice of parameters we find that AMI will discover at least several tens of clusters every year with Mtot ≥ 1014M⊙; the numbers depend on factors such as the mean matter density, the density fluctuation power spectrum and cluster gas evolution. The AMI survey itself can distinguish between these to some degree, and parameter degeneracies are largely eliminated given optical and X-ray follow-up of these clusters; this will also permit direct investigation of cluster physics and what drives the evolution.

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