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(ABRIDGED)The rise of cosmic structure depends upon the statisticaldistribution of initial density fluctuations generated by inflation. While thesimplest models predict an almost perfectly Gaussian distribution, more-generalmodels predict a level of primordial non-Gaussianity (PNG) that observationsmight yet be sensitive enough to detect. Recent Planck Collaborationmeasurements of the CMB temperature anisotropy bispectrum significantly tightenthe observational limits, but they are still far from the PNG level predictedby the simplest models of inflation. Probing levels below CMB sensitivitieswill require other methods, such as searching for the statistical imprint ofPNG on galactic halo clustering. During the epoch of reionization (EoR), thefirst stars and galaxies released radiation into the intergalactic medium (IGM)that created ionized patches whose large-scale geometry and evolution reflectedthe underlying abundance and large-scale clustering of the star-forminggalaxies. This statistical connection between ionized patches in the IGM andgalactic halos suggests that observing reionization may be another way toconstrain PNG. We employ the linear perturbation theory of reionization andsemi-analytic models based on the excursion-set formalism to model the effectsof PNG on the EoR. We quantify the effects of PNG on the large-scale structureof reionization by deriving the ionized density bias, i.e. ratio of ionizedatomic to total matter overdensities in Fourier space, at small wavenumber.Just as previous studies found that PNG creates a scale-dependent signature inthe halo bias, so, too, we find a scale-dependent signature in the ionizeddensity bias. Our results, which differ significantly from previous attempts inthe literature to characterize this PNG signature, will be applied elsewhere topredict its observable consequences, e.g. in the cosmic 21cm background.

The scale-dependent signature of primordial non-Gaussianity in the large-scale structure of cosmic reionization