Hilton, Matt and Romer, A. Kathy and Kay, Scott T. and Mehrtens, Nicola and Lloyd-Davies, E. J. and Thomas, Peter A. and Short, Chris J. and Mayers, Julian A. and Rooney, Philip J. and Stott, John P. and Collins, Chris A. and Harrison, Craig D. and Hoyle, Ben and Liddle, Andrew R. and Mann, Robert G. and Miller, Christopher J. and Sahlén, Martin and Viana, Pedro T P and Davidson, Michael and Hosmer, Mark and Nichol, Robert C. and Sabirli, Kivanc and Stanford, S. A. and West, Michael J. (2012) The XMM Cluster Survey:evidence for energy injection at high redshift from evolution of the X-ray luminosity-temperature relation. Monthly Notices of the Royal Astronomical Society, 424 (3). pp. 2086-2096. ISSN 0035-8711
Full text not available from this repository.Abstract
We measure the evolution of the X-ray luminosity-temperature (L X - T) relation since z ~ 1.5 using a sample of 211 serendipitously detected galaxy clusters with spectroscopic redshifts drawn from the XMM Cluster Survey first data release (XCS-DR1). This is the first study spanning this redshift range using a single, large, homogeneous cluster sample. Using an orthogonal regression technique, we find no evidence for evolution in the slope or intrinsic scatter of the relation since z ~ 1.5, finding both to be consistent with previous measurements at z ~ 0.1. However, the normalization is seen to evolve negatively with respect to the self-similar expectation: we find E -1(z)L X = 10 44.67 ± 0.09(T/5) 3.04 ± 0.16(1 + z) -1.5 ± 0.5, which is within 2σ of the zero evolution case. We see milder, but still negative, evolution with respect to self-similar when using a bisector regression technique. We compare our results to numerical simulations, where we fit simulated cluster samples using the same methods used on the XCS data. Our data favour models in which the majority of the excess entropy required to explain the slope of the L X - T relation is injected at high redshift. Simulations in which active galactic nucleus feedback is implemented using prescriptions from current semi-analytic galaxy formation models predict the positive evolution of the normalization, and differ from our data at more than 5σ. This suggests that more efficient feedback at high redshift may be needed in these models.