In a variety of inflation models the motion of the inflaton may trigger the production of some noninflaton particles during inflation, for example, via parametric resonance or a phase transition. Particle production during inflation leads to observables in the cosmological fluctuations, such as features in the primordial power spectrum and also non-Gaussianities. Here we focus on a prototype scenario with inflaton, $\varphi$, and isoinflaton, $\chi$, fields interacting during inflation via the coupling $g^2(\varphi -{\varphi }_0{)}^2{\chi }^2$. Since several previous investigations have hinted at the presence of localized “glitches” in the observed primordial power spectrum, which are inconsistent with the simplest power-law model, it is interesting to determine the extent to which such anomalies can be explained by this simple and microscopically well-motivated inflation model. Our prototype scenario predicts a bumplike feature in the primordial power spectrum, rather than an oscillatory “ringing” pattern as has previously been assumed. We discuss the observational constraints on such features using a variety of cosmological data sets. We find that bumps with amplitudes as large as $\mathcal{O}(10\%)$ of the usual scale-invariant fluctuations from inflation, corresponding to $g^2\sim 0.01$, are allowed on scales relevant for cosmic microwave background experiments. Our results imply an upper limit on the coupling $g^2$ (for a given ${\varphi }_0$) which is crucial for assessing the detectability of the non-Gaussianity produced by inflationary particle production. We also discuss more complicated features that result from superposing multiple instances of particle production. Finally, we point to a number of microscopic realizations of this scenario in string theory and supersymmetry and discuss the implications of our constraints for the popular brane/axion monodromy inflation models.

• Received 29 September 2009

DOI:https://doi.org/10.1103/PhysRevD.80.126018