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In this paper we study slow-roll inflation with holonomy corrections fromloop quantum cosmology. Both tensor and scalar power spectra of primordialperturbations are computed up to the first order in slow-roll parameters and$V/\rho_{c}$, where $V$ is a potential of the scalar field and $\rho_{c}$ is acritical energy density (expected to be of the order of the Planck energydensity). Possible normalizations of modes at short scales are discussed. Incase the normalization is performed with use of the Wronskian condition appliedto adiabatic vacuum, the tensor and scalar spectral indices are not quantumcorrected in the leading order. However, by choosing an alternative method ofnormalization one can obtain quantum corrections in the leading order.Furthermore, we show that the holonomy-corrected equation of motion for tensormodes can be derived from an effective background metric. This allows us toprove that the Wronskian normalization condition for the tensor modes preservesthe classical form.

Inflationary power spectra with quantum holonomy corrections