Hilton, M. and Collins, C. and De Propris, R. and Baldry, I.K. and Baugh, C.M. and Bland-Hawthorn, J. and Bridges, T. and Cannon, R. and Cole, S. and Colless, M. and Couch, W.J. and Dalton, G.B. and Driver, S.P. and Efstathiou, G. and Ellis, R.S. and Frenk, C.S. and Glazebrook, K. and Jackson, C.A. and Lahav, O. and Lewis, I. and Lumsden, S. and Maddox, S.J. and Madgwick, D. and Norberg, P. and Peacock, J.A. and Peterson, B.A. and Sutherland, W. and Taylor, K. (2005) 'The 2dF Galaxy Redshift Survey : correlation with the ROSAT-ESO flux-limited X-ray galaxy cluster survey.', Monthly notices of the Royal Astronomical Society., 363 (2). pp. 661-674.
The ROSAT-European Southern Observatory (ESO) flux-limited X-ray (REFLEX) galaxy cluster survey and the Two-degree Field Galaxy Redshift Survey (2dFGRS), respectively, comprise the largest, homogeneous X-ray selected cluster catalogue and completed galaxy redshift survey. In this work, we combine these two outstanding data sets in order to study the effect of the large-scale cluster environment, as traced by X-ray luminosity, on the properties of the cluster member galaxies. We measure the LX−σr relation from the correlated data set and find it to be consistent with recent results found in the literature. Using a sample of 19 clusters with LX≥ 0.36 × 1044 erg s−1 in the 0.1–2.4 keV band, and 49 clusters with lower X-ray luminosity, we find that the fraction of early spectral type (η=−1.4), passively evolving galaxies is significantly higher in the high-LX sample within R200. We extend the investigation to include composite bJ cluster luminosity functions, and find that the characteristic magnitude of the Schechter-function fit to the early-type luminosity function is fainter for the high-LX sample compared to the low-LX sample (ΔM*= 0.58 ± 0.14). This seems to be driven by a deficit of such galaxies with MbJ∼−21. In contrast, we find no significant differences between the luminosity functions of star-forming, late-type galaxies. We believe these results are consistent with a scenario in which the high-LX clusters are more dynamically evolved systems than the low-LX clusters.
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|Publisher Web site:||http://dx.doi.org/10.1111/j.1365-2966.2005.09470.x|
|Publisher statement:||This article has been accepted for publication in Monthly notices of the Royal Astronomical Society ©: 2005 RAS Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.|
|Date accepted:||No date available|
|Date deposited:||15 August 2016|
|Date of first online publication:||October 2005|
|Date first made open access:||No date available|
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