  Motivated by BICEP2 results on the CMB polarization B-mode which imply
primordial gravitational waves are produced when the Universe has the expansion
rate of about $H \approx 10^{14}$ GeV, and by deviations from a smooth
power-law behaviour for multipoles $\ell <50$ in the CMB temperature anisotropy
power spectrum found in the WMAP and Planck experiments, we have expanded our
class of large field inflationary models that fit both the BICEP2 and Planck
CMB observations consistently. These best-fitted large field models are found
to have a transition from a faster roll to the slow roll $V(\phi)=m^2 \phi^2/2$
inflation at a field value around 14.6~${\rm M_{Pl}}$ and thus a potential
energy of $V(\phi) \sim (10^{16}\,{\rm GeV})^4$. In general this transition
with sharp features in the inflaton potential produces not only suppression of
scalars relative to tensor modes at small $k$ but also introduces wiggles in
the primordial perturbation spectrum. These wiggles are shown to be useful to
explain some localized features in the CMB angular power spectrum and can also
have other observational consequences. Thus, primordial GW can be used now to
make a tomography of inflation determining its fine structure. The resulting
Wiggly Whipped Inflation scenario is described in details and the anticipated
perturbation power spectra, CMB power spectra, non-Gaussianity and other
observational consequences are calculated and compared to existing and
forthcoming observations.
