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Deriving the total masses of galaxy clusters from observations of theintracluster medium (ICM) generally requires some prior information, inaddition to the assumptions of hydrostatic equilibrium and spherical symmetry.Often, this information takes the form of particular parametrized functionsused to describe the cluster gas density and temperature profiles. In thispaper, we investigate the implicit priors on hydrostatic masses that resultfrom this fully parametric approach, and the implications of such priors forscaling relations formed from those masses. We show that the application ofsuch fully parametric models of the ICM naturally imposes a prior on the slopesof the derived scaling relations, favoring the self-similar model, and arguethat this prior may be influential in practice. In contrast, this bias does notexist for techniques which adopt an explicit prior on the form of the massprofile but describe the ICM non-parametrically. Constraints on the slope ofthe cluster mass--temperature relation in the literature show a separationbased the approach employed, with the results from fully parametric ICMmodeling clustering nearer the self-similar value. Given that a primary goal ofscaling relation analyses is to test the self-similar model, the application ofmethods subject to strong, implicit priors should be avoided. Alternativemethods and best practices are discussed.

Implicit Priors in Galaxy Cluster Mass and Scaling Relation Determinations