The XMM Cluster Survey: forecasting cosmological and cluster scaling-relation parameter constraints

Sahlén, Martin, Viana, Pedro T P, Liddle, Andrew R, Romer, A Kathy, Davidson, Michael, Hosmer, Mark, Lloyd-Davies, E J, Sabirli, Kivanc, Collins, Chris A, Freeman, Peter E, Hilton, Matt, Hoyle, Ben, Kay, Scott T, Mann, Robert G, Mehrtens, Nicola, Stanford, S Adam and West, Michael J (2009) The XMM Cluster Survey: forecasting cosmological and cluster scaling-relation parameter constraints. Monthly Notices of the Royal Astronomical Society, 397 (2). pp. 577-607. ISSN 0035-8711

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We forecast the constraints on the values of s8, Om and cluster scaling-relation parameters which we expect to obtain from the XMM Cluster Survey (XCS). We assume a flat cold dark matter Universe and perform a Monte Carlo Markov Chain analysis of the evolution of the number density of galaxy clusters that takes into account a detailed simulated selection function. Comparing our current observed number of clusters shows good agreement with predictions. We determine the expected degradation of the constraints as a result of self-calibrating the luminositytemperature relation (with scatter), including temperature measurement errors, and relying on photometric methods for the estimation of galaxy cluster redshifts. We examine the effects of systematic errors in scaling relation and measurement error assumptions. Using only (T, z) self-calibration, we expect to measure Om to 0.03 (and O to the same accuracy assuming flatness), and s8 to 0.05, also constraining the normalization and slope of the luminositytemperature relation to 6 and 13 per cent (at 1s), respectively, in the process. Self-calibration fails to jointly constrain the scatter and redshift evolution of the luminositytemperature relation significantly. Additional archival and/or follow-up data will improve on this. We do not expect measurement errors or imperfect knowledge of their distribution to degrade constraints significantly. Scaling-relation systematics can easily lead to cosmological constraints 2s or more away from the fiducial model. Our treatment is the first exact treatment to this level of detail, and introduces a new `smoothed ML (Maximum Likelihood) estimate of expected constraints.

Item Type: Article
Additional Information: The XCS Collaboration
Schools and Departments: School of Mathematical and Physical Sciences > Physics and Astronomy
Subjects: Q Science > QB Astronomy
Depositing User: Nils Jean Nikolaj Martin Sahlen
Date Deposited: 06 Feb 2012 19:51
Last Modified: 07 Mar 2017 05:46

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