Galaxy cluster X-ray luminosity scaling relations from a representative local sample (REXCESS)

By G. Pratt, Judith Croston, M. Arnaud, H. Böhringer. 2008

493 citations recorded by the source corpus.

We examine the X-ray luminosity scaling relations of 31 nearby galaxy clusters from the Representative XMM-Newton Cluster Structure Survey (REXCESS). The objects are selected only in X-ray luminosity, optimally sampling the cluster luminosity function. Temperatures range from 2 to 9 keV, and there is no bias toward any particular morphological type. To reduce measurement scatter we extract pertinent values in an aperture corresponding to R500, estimated using the tight correlation between YX (the product of gas mass and temperature) and total mass. The data exhibit power law relations between bolometric X-ray luminosity and temperature, YX and total mass, all with slopes that are significantly steeper than self-similar expectations. We examine the possible causes for the steepening, finding that structural variations have little effect and that the primary driver appears to be a systematic variation of the gas content with mass. Scatter about the relations is dominated in all cases by the presence of cool cores. The natural logarithmic scatter about the raw X-ray luminosity-temperature relation is about 70 per cent, and about the X-ray luminosity-YX relation it is 40 per cent. Systems with more morphological substructure show similar scatter about scaling relations than clusters with less substructure, due to the preponderance of cool core systems in the regular cluster subsample. Cool core and morphologically disturbed systems occupy distinct regions in the residual space with respect to the best fitting mean relation, the former lying systematically at the high luminosity side, the latter lying systematically at the low luminosity side. Simple exclusion of the central regions serves to reduce the scatter about the scaling relations by more than a factor of two. The scatter reduces by a similar amount with the use of the central gas density as a third parameter. Using YX as a total mass proxy, we derive a Malmquist bias-corrected local luminosity-mass relation and compare with other recent determinations. Our results indicate that luminosity can be a reliable mass proxy with controllable scatter, which has important implications for upcoming all-sky cluster surveys, such as those to be undertaken with Planck and eROSITA ,a nd ultimately for the use of the cluster population for cosmological purposes.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/309436b9844f14f1757390817fe1abe441f3ac5b

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Citations in the corpus

The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths (2012, methodology): “For each cluster observed in X-rays, the predicted SZ flux Y500 is given by the combination of the LX-M relation of Pratt et al. (2009) and the M-Y relation of Arnaud et al. (2010).”
A SUNYAEV–ZEL'DOVICH-SELECTED SAMPLE OF THE MOST MASSIVE GALAXY CLUSTERS IN THE 2500 deg2 SOUTH POLE TELESCOPE SURVEY (2011, result): “…42 http://cxc.harvard.edu/toolkit/pimms.jsp 43 http://heasarc.nasa.gov/xanadu/xspec/xspec11/index.html 12 Williamson et al. tions from Pratt et al. (2009), Vikhlinin et al. (2009a), and Mantz et al. (2010), to compare our results with other X-ray cluster studies.”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “Melin et al. (2010) used the 5-year WMAP data and a bigger sample of 893 clusters and a scaling relation between r500 and the X-ray luminosity taken from Pratt et al. (2009); Arnaud et al. (2010).”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, unknown): “Recent work by Pratt et al. (2009) have derived a similar slope for the LX − T relation for clusters as Markevitch (2002).”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, background): “…of Vikhlinin et al. (2006) and Sun et al. (2009) (where the gas fraction fg is defined as the gas mass divided by total mass within R500), and the ‘universal’ electron pressure profile measured by Arnaud et al. (2010) from the REXCESS cluster sample (Böhringer et al. 2007; Pratt et al. 2009).”
Planck intermediate results: V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (2012, unknown): “At R 500 , the measurement of f gas for massive clusters presented by Pratt et al. (2009) ( see also Giodini et al. 2009, for massive clusters with (4–10) × 10 14 M ⊙ ) is lower by a factor 1.3 with respect to our estimate (although compatible within ± 2 σ ). re-ported We can also compare our…”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “Some authors have included corrections for the expected Malmquist bias given a flux limit or selection function (Pacaud et al. 2007; Pratt et al. 2009; Vikhlinin et al. 2009a), but most analyses of scaling relations in the literature employs least-squares regression without detailed consideration…”
The MCXC: a meta-catalogue of x-ray detected clusters of galaxies (2010, methodology): “The temperature dependence of this conversion is taken into account by either using measured temperatures when available in the input catalogue, or by iteration about the the non-core-excised luminositytemperature relation of Pratt et al. (2009), assuming an abudance of 0.3.”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, methodology): “Furthermore we note that the scaling relation determined by Pratt et al. (2009) is based on three different samples of groups and clusters: this should reduce the potential bias produced by sample selection.”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, methodology): “…relation between Y500 and M500, and the data points utilized after correction of the Malmquist bias. adapted from that described in Vikhlinin et al. (2009a) and Pratt et al. (2009), where each data point is rescaled by the mean bias for its flux, and the relation refitted using the rescaled points.”
The Observed Growth of Massive Galaxy Clusters II: X-ray Scaling Relations (2009, methodology): “Pratt et al. (2009) and Vikhlinin et al. (2009a) found luminosity– mass (0.1–2.4 keV band) slopes ∼1.6 using a procedure in which the luminosity data are corrected for the expected Malmquist bias, given a flux limit or full selection function.”
X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories (2009, background): “15−1×r500 as the most reliable single observable mass proxy for clusters (e.g. Arnaud et al. 2005; Pratt et al. 2009).”