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In the era of large surveys, yielding thousands of galaxy clusters, efficientmass proxies at all scales are necessary in order to fully utilize clusters ascosmological probes. At the cores of strong lensing clusters, the Einsteinradius can be turned into a mass estimate. This efficient method has beenroutinely used in literature, in lieu of detailed mass models; however, itsscatter, assumed to be $\sim30\%$, has not yet been quantified. Here, we assessthis method by testing it against ray-traced images of cluster-scale halos fromthe Outer Rim N-body cosmological simulation. We measure a scatter of $13.9\%$and a positive bias of $8.8\%$ in $M(<\theta_E)$, with no systematiccorrelation with total cluster mass, concentration, or lens or sourceredshifts. We find that increased deviation from spherical symmetry increasesthe scatter; conversely, where the lens produces arcs that cover a largefraction of its Einstein circle, both the scatter and the bias decrease. Whilespectroscopic redshifts of the lensed sources are critical for accuratemagnifications and time delays, we show that for the purpose of estimating thetotal enclosed mass, the scatter introduced by source redshift uncertainty isnegligible compared to other sources of error. Finally, we derive and apply anempirical correction that eliminates the bias, and reduces the scatter to$10.1\%$ without introducing new correlations with mass, redshifts, orconcentration. Our analysis provides the first quantitative assessment of theuncertainties in $M(<\theta_E)$, and enables its effective use as a core massestimator of strong lensing galaxy clusters.

Efficient Mass Estimate at the Core of Strong Lensing Galaxy Clusters Using the Einstein Radius