The same reason, i.e. H$_{inf}$ << m$_{φ}$ also precludes any large trans-Planckian correction. Any such correction would generically go as ( H$_{inf}$$^{/M}$∗ ) 2 ∼ ( m$_{φ}$$^{/M}$∗ ) ≪ 1, where $^{M}$∗ is the scale at which one would expect trans-Planckian effects to kick in [291, 293, 298]. Note that in our case the initial vacuum is the Bunch-Davis and the evolution of the modes is adiabatic. The latter condition is important to make sure that unknown physics at the high scale is less and less sensitive to the low energy world [298, 353]. 

Finally, we also make a comment on the cosmological moduli problem [721–724]. The moduli are generically displaced from their true minimum if their mass is less than the expansion rate during inflation. In our case H$_{inf}$ ≪ m$_{moduli}$ ∼ O (TeV) . This implies that quantum fluctuations cannot displace the moduli from their true minima during the inflationary epoch driven by MSSM flat directions. Moreover, any oscillations of the moduli will be exponentially damped during the inflationary epoch. Therefore, MSSM inflation can naturally address the infamous moduli problem [89]. 

## C. Exciting SM baryons and cold dark matter 

Interesting aspect of MSSM inflaton is that inflation takes place away from the point of enhanced gauge symmetry . Keep in mind that the VEV of the MSSM flat direction inflaton breaks the gauge symmetry spontaneously, for instance udd breaks SU (3)$_{C}$ × U (1)$_{Y}$ while LLe breaks SU (2)$_{W}$ × U (1)$_{Y}$ , therefore, induces a SUSY conserving mass ∼ g 〈 φ ( t ) 〉 to the gauge/gaugino fields in a similar way as the Higgs mechanism, where g is a gauge coupling. When the flat direction goes to its minimum, 〈 φ ( t ) 〉 = 0, the gauge symmetry is restored. In this respect the origin is a point of enhanced symmetry. 

After the end of inflation, the flat direction starts rolling towards its global minimum. At this stage the dominant term in the scalar potential will be: m$_{φ}$φ $^{2}$/ 2. Since the frequency of oscillations is ω ∼ m$_{φ}$ ∼ 10 $^{3}$H$_{inf}$ , the flat direction oscillates a large number of times within the first Hubble time after the end of inflation. Hence the effect of expansion is negligible. Further note that the motion is strictly along the radial direction, i.e. one dimensional. 

In all the examples inflaton has gauge couplings to the gauge/gaugino fields and Yukawa couplings to the Higgs/Higgsino fields. As we will see particles with a larger couplings are 

