  We have examined the distribution of the position angle (PA) of the Galactic
center filaments with lengths $L > 66''$ and $ < 66''$ as well as their length
distribution as a function of PA. We find bimodal PA distributions of the
filaments, long and short populations of radio filaments. Our PA study shows
the evidence for a distinct population of short filaments with PA close to the
Galactic plane. Mainly thermal short radio filaments ($<66''$) have PAs
concentrated close to the Galactic plane within $60^\circ < \rm PA <120^\circ$.
Remarkably, the short filament PAs are radial with respect to the Galactic
center at $l <0^\circ$, and extend in the direction toward Sgr A*. On a smaller
scale, the prominent Sgr E HII complex G358.7-0.0 provides a vivid example of
the nearly radial distribution of short filaments. The bimodal PA distribution
suggests different origin for two distinct filament populations. We argue that
alignment of the short filament population results from the ram pressure of a
degree-scale outflow from Sgr A* that exceeds the internal filament pressure,
and aligns them along the Galactic plane. The ram pressure is estimated to be
2$\times10^6\,$ cm$^{-3}\,$ K at a distance of 300pc, requiring biconical mass
outflow rate $10^{-4}$ \msol\, yr$^{-1}$ with an opening angle of
$\sim40^\circ$. This outflow aligns not only the magnetized filaments along the
Galactic plane but also accelerates thermal material associated with embedded
or partially embedded clouds. This places an estimate of $\sim$6 Myr as the age
of the outflow.
