  The flatness of an accelerating universe model (characterized by a dark
energy scalar field $\chi$) is mimicked from a curved model that is filled
with, apart from the cold dark matter component, a quintessencelike scalar
field $Q$. In this process, we characterize the original scalar potential
$V(Q)$ and the mimicked scalar potential $V(\chi)$ associated to the scalar
fields $Q$ and $\chi$, respectively. The parameters of the original model are
fixed through the mimicked quantities that we relate to the present
astronomical data, such that the equation state parameter $w_{_{\chi}}$ and the
dark energy density parameter $\Omega_{\chi}$.
