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The formation of globular clusters and their relation to the distribution ofdark matter have long puzzled astronomers. One of the most recently-proposedglobular cluster formation channels ties ancient star clusters to thelarge-scale streaming velocity of baryons relative to dark matter in the earlyUniverse. These streaming velocities affect the global infall of baryons intodark matter halos, the high-redshift halo mass function, and the earliestgenerations of stars. In some cases, streaming velocities may result in denseregions of dark-matter-free gas that becomes Jeans unstable, potentiallyleading to the formation of compact star clusters. We investigate thishypothesis using cosmological hydrodynamical simulations that include a fullchemical network and the formation and destruction of H$_2$, a process crucialfor the formation of the first stars. We find that high-density gas in regionswith significant streaming velocities -- which constitute approximately 1\% ofthe Universe -- is indeed somewhat offset from the centers of dark matterhalos, but this offset is typically significantly smaller than the virialradius. Gas outside of dark matter halos never reaches Jeans-unstable densitiesin our simulations. We postulate that low-level ($Z \approx10^{-3}\,Z_{\odot}$) metal enrichment by Population III supernovae may enablecooling in the extra-virial regions, allowing gas outside of dark matter halosto cool to the CMB temperature and become Jeans-unstable. Follow-up simulationsthat include both streaming velocities and metal enrichment by Population IIIsupernovae are needed to understand if streaming velocities provide one pathfor the formation of globular clusters in the early Universe.

Globular Clusters and Streaming Velocities: Testing the new formation channel in high-resolution cosmological simulations