  We present direct images in the H$\alpha$ and [SII]$\lambda \lambda$6717,6731
$\text{\AA}$ lines of the Galactic Supernova Remnant G109.1-1.0 (CTB 109). We
confirm that the filaments detected are the optical counterpart of the X-ray
and radio supernova remnant due to their high [SII]/H$\alpha$ line-ratios. We
study for the first time the kinematics of the optical counterpart of SNR CTB
109 using the UNAM scanning Fabry-Perot interferometer PUMA. We estimate a
systemic velocity of V$_{LSR}$=-50$\pm$6 km s$^{-1}$ for this remnant and an
expansion velocity of V$_{exp}$=230$\pm$5 km s$^{-1}$. From this velocity value
and taking into account previous studies about the kinematics of objects at
that Galactic longitude we derive a distance to the SNR CTB 109 of 3.1$\pm$0.2
kpc, locating it in the Perseus arm. Using the
[SII]$\lambda$6717/[SII]$\lambda$6731 line-ratio we find an electronic density
value around n$_e$= 580 cm$^{-3}$. Considering that this remnant is evolving in
a low density medium with higher density cloudlets responsible of the optical
emission, we determine the age and energy deposited in the ISM by the supernova
explosion (E$_0$) in both the Sedov-Taylor phase and the radiative phase. For
both cases the age is of thousands of years and the E$_0$ is rather typical of
SNRs containing simple pulsars so that, the energy released to the ISM cannot
be used to distinguish between supernova remnants hosting typical pulsars from
those hosting powerful magnetars as in the case of CTB 109.
