Inflationary power spectra with quantum holonomy corrections
  In this paper we study slow-roll inflation with holonomy corrections from
loop quantum cosmology. Both tensor and scalar power spectra of primordial
perturbations 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 a
critical energy density (expected to be of the order of the Planck energy
density). Possible normalizations of modes at short scales are discussed. In
case the normalization is performed with use of the Wronskian condition applied
to adiabatic vacuum, the tensor and scalar spectral indices are not quantum
corrected in the leading order. However, by choosing an alternative method of
normalization one can obtain quantum corrections in the leading order.
Furthermore, we show that the holonomy-corrected equation of motion for tensor
modes can be derived from an effective background metric. This allows us to
prove that the Wronskian normalization condition for the tensor modes preserves
the classical form.
