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If the dark matter halos of galaxies contain large numbers of subhalos aspredicted by the $\Lambda$CDM model, these subhalos are expected to appear instrong galaxy--galaxy lens systems as small--scale perturbations in individualimages. We simulate observations of multiply--lensed sub--mm galaxies at$z\sim2$ as a probe of the dark matter halo of a lens galaxy at $z\sim0.5$. Wepresent detection limits for dark substructures based on a visibility planeanalysis of simulated Atacama Large Millimeter/submillimeter Array (ALMA) datain bands 7, 8 and 9. We explore two effects: local surface brightness anomalieson angular scales similar to the Einstein radius and the astrometric shift ofmacroimages. This improves the sensitivity of our lens modeling to the mass ofthe lens perturber. We investigate the sensitivity of the detection oflow--mass subhalos to the projected position of the subhalo on the image planeas well as the source structure and inner density profile of the lens. Wedemonstrate that, using the most extended ALMA configuration, pseudo-Jaffesubhalos can be detected with 99% confidence down to $M = 10^7 M_\odot$. Weshow how the detection threshold for the three ALMA bands depends on theprojected position of the subhalo with respect to the lensed images andconclude that, despite the highest nominal angular resolution, band 9 providesthe poorest sensitivity due to observational noise. All simulations use the\emph{ALMA Full ops most extended} ALMA configuration setup in CASA.

Probing cold dark matter subhalos with simulated ALMA observations of macrolensed sub-mm galaxies