Open AccessThe power spectrum of flux‐limited X‐ray galaxy cluster surveys
Author(s) -
Zandivarez Ariel,
Abadi Mario G.,
Lambas Diego G.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04578.x
Subject(s) - physics , astrophysics , amplitude , spectral density , cluster (spacecraft) , redshift , galaxy cluster , galaxy , spectral index , flux (metallurgy) , power law , range (aeronautics) , spectral line , astronomy , statistics , optics , materials science , mathematics , computer science , metallurgy , composite material , programming language
We compute the redshift space power spectrum of two X‐ray cluster samples: the X‐ray Brightest Abell Cluster Sample (XBACS) and the Brightest Cluster Sample (BCS) using the method developed by Feldman, Kaiser & Peacock. The power spectra derived for these samples are in agreement with determinations of other optical and X‐ray cluster samples. For XBACS we find the largest power spectrum amplitude expected, given the high richness of this sample (R≥2) . In the range 0.05<k<0.4 h Mpc −1 the power spectrum shows a power‐law behaviour P(k)∝k n with an index n≃−1.2 . In a similar range, 0.04<k<0.3 h Mpc −1 , the BCS power spectrum has a smaller amplitude with index n≃−1.0 . We do not find significant evidence for a peak at k≃0.05 h Mpc −1 , suggesting that claims such of feature detections in some cluster samples could rely on artificial inhomogeneities of the data. We compare our results with power spectrum predictions derived by Moscardini et al. within current cosmological models (LCDM and OCDM). For XBACS we find that both models underestimate the amplitude of the power spectrum but for BCS there is reasonably good agreement at k≳0.03 h Mpc −1 for both models.