IngentaConnect Very Small Array observations of the SunyaevZel'dovich effect in ...

Authors: Lancaster, Katy; Genova-Santos, Ricardo¹; Falcòn, Nelson; Grainge, Keith²; Gutièrrez, Carlos¹; Kneissl, Rüdiger²; Marshall, Phil³; Pooley, Guy²; Rebolo, Rafael; Rubiño-Martin, Jose-Alberto¹; Saunders, Richard D. E.²; Waldram, Elizabeth²; Watson, Robert A.⁴

Source: Monthly Notices of the Royal Astronomical Society, Volume 359, Number 1, May 2005 , pp. 16-30(15)

Publisher: Blackwell Publishing

Abstract:

We present Very Small Array (VSA) observations (centred on ≈34 GHz) on scales ≈20 arcmin towards a complete, X-ray flux-limited sample of seven clusters at redshift z < 0.1 . Four of the clusters have significant Sunyaev–Zel'dovich (SZ) detections in the presence of cosmic microwave background (CMB) primordial anisotropy. For all seven, we use a Bayesian Markov Chain Monte Carlo (MCMC) method for inference from the VSA data, with X-ray priors on cluster positions and temperatures, and radio priors on sources. In this context, the CMB primordial fluctuations are an additional source of Gaussian noise, and are included in the model as a non-diagonal covariance matrix derived from the known angular power spectrum. In addition, we make assumptions of β-model gas distributions and of hydrostatic equilibrium, to evaluate probability densities for the gas mass (M_gas) and total mass (M_r) out to r₂₀₀, the radius at which the average density enclosed is 200 times the critical density at the redshift of the cluster. This is further than has been done before and close to the classical value for a collapsed cluster. Our combined estimate of the gas fraction (f_gas=M_gas/M_r) is 0.08^+0.06_−0.04 h⁻¹ . The random errors are poor (note, however, that the errors are higher than would have been obtained with the usual χ² method on the same data) but the control of bias is good. We have described the MCMC analysis method specifically in terms of SZ but hope the description will be of more general use. We find that the effects of primordial CMB contamination tend to be similar in the estimates of both M_gas and M_r over the narrow range of angular scales we are dealing with, so that there is little effect of primordials on f_gas determination. Using our M_r estimates we find a normalization of the mass–temperature relation based on the profiles from the VSA cluster pressure maps, which is in good agreement with recent M–T determinations from X-ray cluster measurements.

Keywords: galaxies: clusters: general; cosmic microwave background; cosmology: observations; X-rays: galaxies: clusters

Document Type: Research article

DOI: 10.1111/j.1365-2966.2005.08696.x

Affiliations: 1: Instituto de Astrofisíca de Canarias, 38200 La Laguna, Tenerife, Canary Islands, Spain 2: Astrophysics Group, Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE 3: Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, PO Box 20450, MS29, Stanford, CA 94309, USA 4: Jodrell Bank Observatory, University of Manchester, Macclesfield, Cheshire SK11 9DL

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Very Small Array observations of the Sunyaev–Zel'dovich effect in nearby galaxy clusters