A Chandra Study of the Image Power Spectra of 41 Cool Core and Non-Cool
  Core Galaxy Clusters
  In this work we propose a new diagnostic to segregate cool core (CC) clusters
from non-cool core (NCC) clusters by studying the two-dimensional power spectra
of the X-ray images observed with the Chandra X-ray observatory. Our sample
contains 41 members ($z=0.01\sim 0.54$), which are selected from the Chandra
archive when a high photon count, an adequate angular resolution, a relatively
complete detector coverage, and coincident CC-NCC classifications derived with
three traditional diagnostics are simultaneously guaranteed. We find that in
the log-log space the derived image power spectra can be well represented by a
constant model component at large wavenumbers, while at small wavenumbers a
power excess beyond the constant component appears in all clusters, with a
clear tendency that the excess is stronger in CC clusters. By introducing a new
CC diagnostic parameter, i.e., the power excess index (PEI), we classify the
clusters in our sample and compare the results with those obtained with three
traditional CC diagnostics. We find that the results agree with each other very
well. By calculating the PEI values of the simulated clusters, we find that the
new diagnostic works well at redshifts up to 0.5 for intermediately sized and
massive clusters with a typical Chandra or XMM pointing observation. The new CC
diagnostic has several advantages over its counterparts, e.g., it is free of
the effects of the commonly seen centroid shift of the X-ray halo caused by
merger event, and the corresponding calculation is straightforward, almost
irrelevant to the complicated spectral analysis.
