I will show how the current data (from WMAP+PLANCK+BICEP) and the future data on CMB can discriminate super-Planckian VEV models of inflation with a sub-Planckian VEV models of inflation. I will reconstruct the inflationary potential for a sub-Planckian excursion of a single inflaton field from WMAP+PLANCL+BICEP data, and embed such sub-Planckian VEV model of inflation within SUSY flat directions of MSSM with Supergravity corrections.

Inflation is not only responsible for creating the seed perturbations for the cosmic microwave background (CMB) radiation, but also responsible for creating all the observed matter after the end of inflation. It is high time that the community understands the importance that inflation is not just to explain CMB data, but also to explain how and why we observe the current dark matter abundance and the baryonic abundance. Especially, the latter is well constrained from Big Bang Nucleosynthesis (BBN). Typically, if inflation occurs in the hidden sector then it is extremely challenging to explain NATURALLY the correct abundance of dark matter and baryonic asymmetry, one requires ad-hoc assumptions which may or many not arise naturally. On the other hand a sub-Planckian VEV model of inflation can in principle be embedded within MSSM while taking into account of Supergravity corrections, and such a model can explain all the CMB data including the large tensor to scalar ratio arising from the current BICEP data.