The Square Kilometre Array (SKA)

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Searching for clusters of galaxies with SUMSS

NEW ERA IN COSMOLOGY 283 (2002) 245-246

Authors:

HJ Buttery, G Cotter, RW Hunstead, EM Sadler

The Power of Jets: New Clues from Radio Circular Polarization and X-Rays

Chapter in Lighthouses of the Universe: The Most Luminous Celestial Objects and Their Use for Cosmology, Springer Nature (2002) 428-435

Authors:

Heino Falcke, Thomas Beckert, Sera Markoff, Elmar Körding, Geoffrey C Bower, Rob Fender

The death of FR II radio sources and their connection with radio relics

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 336:2 (2002) 649-658

Authors:

CR Kaiser, G Cotter

The very small array

EXPERIMENTAL COSMOLOGY AT MILLIMETRE WAVELENGTHS 616 (2002) 72-78

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.