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 \rightarrow \infty and infinite equation of state parameter , w \rightarrow \infty .
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 q \rightarrow - 1 ,w \rightarrow - 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 .