Kavli Affiliate: Mark Vogelsberger
| First 5 Authors: William Lake, Claire E. Williams, Smadar Naoz, Federico Marinacci, Blakesley Burkhart
| Summary:
At high redshifts ($zgtrsim12$), the relative velocity between baryons and
dark matter (the so-called streaming velocity) significantly affects star
formation in low-mass objects. Streaming substantially reduces the abundance of
low-mass gas objects while simultaneously allowing for the formation of
supersonically-induced gas objects (SIGOs) and their associated star clusters
outside of dark matter halos. Here, we present a study of the population-level
effects of streaming on star formation within both halos and SIGOs in a set of
simulations with and without streaming. Notably, we find that streaming
actually enhances star formation within individual halos of all masses at
redshifts between $z=12$ and $z=20$. This is demonstrated both as an increased
star formation rate per object as well as an enhancement of the
Kennicutt-Schmidt relation for objects with streaming. We find that our
simulations are consistent with some observations at high redshift, but on a
population level, they continue to under-predict star formation relative to the
majority of observations. However, simulations of overdense regions (both with
and without streaming) agree with observations, suggesting a strategy for
extracting information about the overdensity and streaming velocity in a given
survey volume in future observations.
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