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Several independent measurements have confirmed the existence of fluctuations($\delta F_{\rm obs}\approx 0.1 \rm nW/m^{2}/sr$ at $3.6 \rm \mu m$) up todegree angular scales in the source-subtracted Near InfraRed Background (NIRB)whose origin is unknown. By combining high resolution cosmologicalN-body/hydrodynamical simulations with an analytical model, and by matchinggalaxy Luminosity Functions (LFs) and the constraints on reionizationsimultaneously, we predict the NIRB absolute flux and fluctuation amplitudeproduced by high-$z$ ($z > 5$) galaxies (some of which harboring Pop III stars,shown to provide a negligible contribution). This strategy also allows us tomake an empirical determination of the evolution of ionizing photon escapefraction: we find $f_{\rm esc} = 1$ at $z \ge 11$, decreasing to $\approx 0.05$at $z = 5$. In the wavelength range $1.0-4.5 \rm \mu m$, the predictedcumulative flux is $F =0.2-0.04 \rm nW/m^2/sr$. However, we find that theradiation from high-$z$ galaxies (including those undetected by currentsurveys) is insufficient to explain the amplitude of the observed fluctuations:at $l=2000$, the fluctuation level due to $z > 5$ galaxies is $\delta F =0.01-0.002 \rm nW/m^2/sr$, with a relative wavelength-independent amplitude$\delta F/F = 4$%. The source of the missing power remains unknown. This mightindicate that an unknown component/foreground, with a clustering signal verysimilar to that of high-$z$ galaxies, dominates the source-subtracted NIRBfluctuation signal.

The contribution of high redshift galaxies to the Near-Infrared Background