Kinematics of the Galactic Supernova Remnant G109.1-1.0 (CTB 109)

We present direct images in the H alpha and [S II] lambda lambda 6717,6731 angstrom lines of the Galactic supernova remnant (SNR) G109.1-1.0 (CTB 109). We confirm that the filaments detected are the optical counterpart of the X-ray and radio SNR due to their high [S II]/H alpha line ratios. We study for the first time the kinematics of the optical counterpart of SNR CTB 109 using the Universidad Nacional Autonoma de Mexico scanning Fabry-Perot interferometer PUMA. We estimate a systemic velocity of V-LSR = - 50 +/- 6 km s(-1) for this remnant and an expansion velocity of V-exp = 230 +/- 5 km s(-1). From this velocity and taking into account previous studies of the kinematics of objects at that Galactic longitude, we derive a distance to SNR CTB 109 of 3.1 +/- 0.2 kpc, locating it in the Perseus arm. Using the [S II] lambda 6717/[S II] 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 for 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 thousands of years and E-0 is rather typical of SNRs containing simple pulsars, so that the energy released to the ISM cannot be used to distinguish between SNRs hosting typical pulsars from those hosting powerful magnetars, like CTB 109.