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We evaluated the effectiveness of different indicators of clustervirialization using 12 large-scale structures in the ORELSE survey spanningfrom $0.7<z<1.3$. We located diffuse X-ray emission from 16 galaxy clustersusing Chandra observations. We studied the properties of these clusters andtheir members, using Chandra data in conjunction with optical and near-IRimaging and spectroscopy. We measured X-ray luminosities and gas temperaturesof each cluster, as well as velocity dispersions of their member galaxies. Wecompared these results to scaling relations derived from virialized clusters,finding significant offsets of up to 3-4$\sigma$ for some clusters, which couldindicate they are disturbed or still forming. We explored if other propertiesof the clusters correlated with these offsets by performing a set of tests ofvirialization and substructure on our sample, including Dressler-Schectmantests, power ratios, analyses of the velocity distributions of galaxypopulations, and centroiding differences. For comparison to a wide range ofstudies, we used two sets of tests: ones that did and did not use spectralenergy distribution fitting to obtain rest-frame colours, stellar masses, andphotometric redshifts of galaxies. Our results indicated that the differencebetween the stellar mass or light mean-weighted center and the X-ray center, aswell as the projected offset of the most-massive/brightest cluster galaxy fromother cluster centroids had the strongest correlations with scaling relationoffsets, implying they are the most robust indicators of cluster virializationand can be used for this purpose when X-ray data is insufficiently deep forreliable $L_X$ and $T_X$ measurements.

Evaluating Tests of Virialization and Substructure Using Galaxy Clusters in the ORELSE Survey