Abstract
The degree of dark matter clustering on small scales presents a strong constraint on its physical nature. One of the most promising avenues for determining the clustering of dark matter on the smallest scales employs narrow stellar streams in the halo of the Milky Way. In this contribution, I review recent progress in modeling the effect of dark matter substructure on the structure of stellar streams and recent constraints on the amount of small (\({\approx }10^7\,M_\odot \)) dark matter substructure in the inner Milky Way halo. The next few years will likely see a large amount of progress both in the modeling of stellar streams and in the quantity and quality of the available data and I discuss future challenges and opportunities in this area.
Published Version
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