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Quasi-single field inflation predicts a peculiar momentum dependence in thesqueezed limit of the primordial bispectrum which smoothly interpolates betweenthe local and equilateral models. This dependence is directly related to themass of the isocurvatons in the theory which is determined by thesupersymmetry. Therefore, in the event of detection of a non-zero primordialbispectrum, additional constraints on the parameter controlling themomentum-dependence in the squeezed limit becomes an important question. Weexplore the effects of these non-Gaussian initial conditions on large-scalestructure and the cosmic microwave background, with particular attention to thegalaxy power spectrum at large scales and scale-dependence corrections togalaxy bias. We determine the simultaneous constraints on the two parametersdescribing the QSF bispectrum that we can expect from upcoming large-scalestructure and cosmic microwave background observations. We find that forrelatively large values of the non-Gaussian amplitude parameters, but stillwell within current uncertainties, galaxy power spectrum measurements will beable to distinguish the QSF scenario from the predictions of the local model. ACMB likelihood analysis, as well as Fisher matrix analysis, shows that there isalso a range of parameter values for which Planck data may be able distinguishbetween QSF models and the related local and equilateral shapes. Given thedifferent observational weightings of the CMB and LSS results, degeneracies canbe significantly reduced in a joint analysis.

Effects and Detectability of Quasi-Single Field Inflation in the Large-Scale Structure and Cosmic Microwave Background