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The primordial matter power spectrum quantifies fluctuations in thedistribution of dark matter immediately following inflation. Over cosmic time,over-dense regions of the primordial density field grow and collapse into darkmatter halos, whose abundance and density profiles retain memory of the initialconditions. By analyzing the image magnifications in eleven strongly-lensed andquadruply-imaged quasars, we infer the abundance and concentrations of low-masshalos, and cast the measurement in terms of the amplitude of the primordialmatter power spectrum. We anchor the power spectrum on large scales, isolatingthe effect of small-scale deviations from the $\Lambda$CDM prediction. Assumingan analytic model for the power spectrum and accounting for several sources ofpotential systematic uncertainty, including three different models for the halomass function, we obtain correlated inferences of $\log_{10}\left(P /P_{\Lambda \rm{CDM}}\right)$, the power spectrum amplitude relative to thepredictions of the concordance cosmological model, of $0.0_{-0.4}^{+0.5}$,$0.1_{-0.6}^{+0.7}$, and $0.2_{-0.9}^{+1.0}$ at k = 10, 25 and 50$\rm{Mpc^{-1}}$ at $68 \%$ confidence, consistent with cold dark matter andsingle-field slow-roll inflation.

The primordial matter power spectrum on sub-galactic scales