  We have succeeded in establishing a cosmological model with a non-minimally
coupled scalar field $\phi$ that can account not only for the spatial
periodicity or the picket-fence structure exhibited by the galaxy $N$-$z$
relation of the 2dF survey, but also for the spatial power spectrum of the
cosmic microwave background radiation (CMB) temperature anisotropy observed by
the WMAP satellite. The scalar field of our model universe starts from an
extremely small value at around the nucleosynthesis epoch, remains in that
state for sufficiently long periods, allowing sufficient time for the CMB
temperature anisotropy to form, and then starts to grow in magnitude at the
redshift $z$ of $\sim 1$, followed by a damping oscillation which is required
to reproduce the observed picket-fence structure of the $N$-$z$ relation. To
realize such behavior of the scalar field, we have found it necessary to
introduce a new form of potential $V(\phi)\propto \phi^2\exp(-q\phi^2)$, with
$q$ being a constant. Through this parameter $q$, we can control the epoch at
which the scalar field starts growing.
