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Strong gravitationally lensed arcs produced by galaxy clusters have beenobservationally detected for several decades now. These strong lensingconstraints provided high-fidelity mass models for cluster lenses that includesubstructure down to $10^{9-10}\,\mathrm{M}_\odot$. Optimizing lens models,where the cluster mass distribution is modeled by a smooth component andsubhalos associated with the locations of individual cluster galaxies, hasenabled deriving the subhalo mass function, providing important constraints onthe nature and granularity of dark matter. In this work, we explore and presenta novel method to detect and measure individual perturbers (subhalos,line-of-sight halos, and wandering supermassive black holes) by exploitingtheir proximity to highly distorted lensed arcs in galaxy clusters, and bymodeling the local lensing distortions with curved arc bases. This methodoffers the possibility of detecting individual low-mass perturber subhalos inclusters and halos along the line-of-sight down to a mass resolution of$10^8\,\mathrm{M}_\odot$. We quantify our sensitivity to low-mass perturbers($M\sim 10^{7-9}\,\mathrm{M}_\odot$) in clusters ($M\sim10^{14-15}\mathrm{M}_\odot$), by creating realistic mock data. Using threelensed images of a background galaxy in the cluster SMACS J0723, taken by the$\textit{James Webb Space Telescope}$, we study the retrieval of the propertiesof potential perturbers with masses $M=10^{7-9}\,\mathrm{M}_\odot$. From thederived posterior probability distributions for the perturber, we constrain itsconcentration, redshift, and ellipticity. By allowing us to probe lower-masssubstructures, the use of curved arc bases can lead to powerful constraints onthe nature of dark matter as discrimination between dark matter models appearson smaller scales.

Detecting Low-Mass Perturbers in Cluster Lenses using Curved Arc Bases