value is very very tiny, we arrive at the constraint condition

$$\label{const2} 
(1+\sqrt{3})\left[\frac{A a e^{-a \tilde t_0}}
{-\frac{3}{2 \tilde t_0}+h'(\tilde 
t_0)}+f(\tilde 
{s}_0)\right]=2 
\tilde s_0 f'(\tilde {s}_0).$$

The constraint (\[const2\]) puts restrictions on the parameters and choice of the functions $h$ and $f$. Imposing this constraint condition allows the scalar potential of the hidden sector to be written as,

$$\label{scalarpot2}
V_{h0}=\frac{1}{M_p^2}\frac{e^{h}}{16 \tilde s_0 \tilde t_0^3} \times \frac{1}{( h''(\tilde t_0)+
\frac{3}{4 \tilde t_0^2})}f^2(\tilde s_0) \left(\frac{3}{2 \tilde t_0}-h'(\tilde t_0)\right)^2.$$

where $V_{h0}$ is the VEV of the scalar potential(\[scalarpot\]). Thus the nature of the minimum depends entirely on the choice of the function $h(\tilde t)$. In the following section an example has been presented in this regard. For a value of $f(\tilde{s}) \sim 10^{25} ~\rm GeV^3$ at VEV, vacuum energy $V_{h_0} \sim -10^{12} ~\rm GeV^4$ can be produced provided all the dimensionless quantities are of $O(1)$. This, together with the contributions from the observable sector in the scalar potential $V_{obs} \sim 10^{12} ~\rm GeV^4$ may conspire to produce a small but positive cosmological constant.

The above analysis implies that the parameter $A \sim \Lambda_N^3$ should have a mass scale with $\Lambda_N \simeq 10^{14} ~\rm GeV$ to produce viable soft breaking terms. This will be 