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ationary trajectories. Graceful exit and particle creation occurs in the non-linear part of the X eld. Right panel: WMAP5 cosmological
constraints (yellow region) in the rnSplane. For no- ne-tuned minimal in
ation models the green and red area show our predictions for
both cases of a stable (concave) potential and unstable (convex) potential. The Planck satellite will be able to provide signi cantly tigther
constraints on rand especially nS(at the<0:5% level) thus further constraining our model. The dashed line is the limit in rthat can be
achieved with an ideal CMB polarization experiment [14]
These are bonuses which come directly from the observa-
tions of the initial density perturbations from WMAP data
[11]. The fact that the in
aton is lighter than the gravitino
may have interesting low-energy phenomenological impli-
cations. Furthermore in this simple model it is easy to
obtain sucient number of efoldings with moderate values
of theparameter.
To explore our proposal in more detail, it is important
to construct an explicit model, even if not very realistic,
in order to understand in more detail the end of in
ation,
the reheating mechanisms, and also the ne structure of
the in
aton potential. We hope to report on this in the
near future [25].
Acknowledgements
We would like to thank G. Dvali, G. Giudice, J. Les-
gourgues, S. Matarrese, G. Ross, Nathan Seiberg, M.A.
V azquez Mozo, and L. Verde for useful discussion. C.G.
and R.J. would like to thank the CERN Theory Group for
hospitality while part of this work was done.References
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