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We derive new constraints on the non-gravitational baryon-dark-matterscattering (BDMS) by evaluating the mass thresholds of dark matter (DM) haloesin which primordial gas can cool efficiently to form Population III (Pop III)stars, based on the timing of the observed 21-cm absorption signal. We focus onthe BDMS model with interaction cross-section $\sigma=\sigma_{1}[v/(1\\mathrm{km\ s^{-1}})]^{-4}$, where $v$ is the relative velocity of theencounter. Our results rule out the region in parameter space with$\sigma_{1}\gtrsim 10^{-19}\ \mathrm{cm^{2}}$ and DM particle mass$m_{\chi}c^{2}\lesssim 3\times 10^{-2}\ \mathrm{GeV}$, where the cosmic numberdensity of Pop III hosts at redshift $z\sim 20$ is at least three orders ofmagnitude smaller than in the standard Lambda cold DM ($\Lambda$CDM) case. Inthese BDMS models, the formation of Pop III stars is significantly suppressedfor $z\gtrsim 20$, inconsistent with the timing of the observed global 21-cmabsorption signal. For the fiducial BDMS model with $m_{\chi}c^{2}=0.3$ GeV and$\sigma_{1}=8\times 10^{-20}\ \mathrm{cm^{2}}$, capable of accommodating themeasured absorption depth, the number density of Pop III hosts is reduced by afactor of $3-10$ at $z\sim 15-20$, when the 21-cm signal is imprinted, comparedwith the $\Lambda$CDM model. The confluence of future detailed cosmologicalsimulations with improved 21-cm observations promises to probe theparticle-physics nature of DM at the small-scale frontier of early structureformation.

Constraining the non-gravitational scattering of baryons and dark matter with early cosmic structure formation