  Gauss-Bonnet-scalar interaction has been found to play a crucial role from
the beginning till the late time of cosmological evolution. A cosmological
model has been constructed where the Universe starts with exponential expansion
but with infinite deceleration (q), and infinite equation of state (w)
parameters. During evolution it passes through the stiff fluid era, q=2, w=1,
the radiation dominated era, q=1, w=1/3 and the matter dominated era, q=1/2,
w=0. Finally, deceleration halts, q=0, w=-1/3, and it then encounters a
transition to the accelerating phase. Asymptotically the Universe reaches yet
another inflationary phase as q and w go over to -1. Such evolution is
independent of the form of the potential and the sign of the kinetic energy
term ie., even a noncanonical kinetic energy is unable to phantomize (w<-1) the
model.
