Andrés Balaguera-Antolínez
We aim to quantify the capability of the inhomogeneous distribution of galaxy clusters, represented by the two-point statistics in Fourier space, to retrieve information on the underlying scaling relations. As an example, we use the mass-X ray luminosity of galaxy clusters. We define the luminosity-weighted power spectrum and introduce the luminosity power spectrum as a direct assessment of the clustering of X-ray luminosity. Using a suite of halo catalogs extracted from $N$-body simulations and realistic estimates of the mass-X ray luminosity relation, we measure the luminosity-weighted and the luminosity power spectrum of galaxy clusters. By means of a Fisher matrix analysis, we quantify the content of information (by means of a Figure-of Merit) encoded in the amplitude, shape and full-shape of these probes. The full shape of the luminosity power spectrum, when analyzed up to scales of $k~0.2 h/ Mpc$, yields a figure of merit which is only one order of magnitude below the value encoded in X-ray luminosity function estimated from the same sample. This is a significant improvement with respect to the FoM obtained from the estimates of the unweighted power spectrum. We therefore suggest future clustering analysis of galaxy clusters to take advantage of the luminosity power spectrum when aiming at simultaneously constraining cosmological and astrophysical parameters (Abridged)
View original:
http://arxiv.org/abs/1306.1399
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