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The core mass of galaxy clusters is an important probe of structureformation. Here, we evaluate the use of a Single-Halo model (SHM) as anefficient method to estimate the strong lensing cluster core mass, testing itwith ray-traced images from the `Outer Rim' simulation. Unlike detailed lensmodels, the SHM represents the cluster mass distribution with a single halo andcan be automatically generated from the measured lensing constraints. We findthat the projected core mass estimated with this method, M$_{\rm SHM}$, has ascatter of $8.52\%$ and a bias of $0.90\%$ compared to the "true" mass withinthe same aperture. Our analysis shows no systematic correlation between thescatter or bias and the lens-source system properties. The bias and scatter canbe reduced to $3.26\%$ and $0.34\%$, respectively, by excluding models thatfail a visual inspection test. We find that the SHM success depends on thelensing geometry, with single giant arc configurations accounting for most ofthe failed cases due to their limiting constraining power. When excluding suchcases, we measure a scatter and bias of $3.88\%$ and $0.84\%$, respectively.Finally, we find that when the source redshift is unknown, the model-predictedredshifts are overestimated, and the M$_{\rm SHM}$ is underestimated by a fewpercent, highlighting the importance of securing spectroscopic redshifts ofbackground sources. Our analysis provides a quantitative characterization ofM$_{\rm SHM}$, enabling its efficient use as a tool to estimate the stronglensing cluster core masses in the large samples, expected from current andfuture surveys.

Core Mass Estimates in Strong Lensing Galaxy Clusters Using a Single-Halo Lens Model