Evaluating Tests of Virialization and Substructure Using Galaxy Clusters
  in the ORELSE Survey
  We evaluated the effectiveness of different indicators of cluster
virialization using 12 large-scale structures in the ORELSE survey spanning
from $0.7<z<1.3$. We located diffuse X-ray emission from 16 galaxy clusters
using Chandra observations. We studied the properties of these clusters and
their members, using Chandra data in conjunction with optical and near-IR
imaging and spectroscopy. We measured X-ray luminosities and gas temperatures
of each cluster, as well as velocity dispersions of their member galaxies. We
compared these results to scaling relations derived from virialized clusters,
finding significant offsets of up to 3-4$\sigma$ for some clusters, which could
indicate they are disturbed or still forming. We explored if other properties
of the clusters correlated with these offsets by performing a set of tests of
virialization and substructure on our sample, including Dressler-Schectman
tests, power ratios, analyses of the velocity distributions of galaxy
populations, and centroiding differences. For comparison to a wide range of
studies, we used two sets of tests: ones that did and did not use spectral
energy distribution fitting to obtain rest-frame colours, stellar masses, and
photometric redshifts of galaxies. Our results indicated that the difference
between the stellar mass or light mean-weighted center and the X-ray center, as
well as the projected offset of the most-massive/brightest cluster galaxy from
other cluster centroids had the strongest correlations with scaling relation
offsets, implying they are the most robust indicators of cluster virialization
and can be used for this purpose when X-ray data is insufficiently deep for
reliable $L_X$ and $T_X$ measurements.
