  New HI images from the VLA Galactic Plane Survey show prominent absorption
features associated with the supernovae remnant G23.3-0.3 (SNR W41). We
highlight the HI absorption spectra and the $^{13}$CO emission spectra of eight
small regions on the face of W41, including four HII regions, three non-thermal
emission regions and one unclassified region. The maximum velocity of
absorption for W41 is 78$\pm$2 km/s and the CO cloud at radial velocity
95$\pm$5 km/s is behind W41. Because an extended TeV source, a diffuse X-ray
enhancement and a large molecular cloud at radial velocity 77$\pm$5 km/s are
also projected at the center of W41, these yield the kinematic distance of 3.9
to 4.5 kpc for W41. For HII regions, our analyses reveal that both G23.42-0.21
and G23.07+0.25 are at the far kinematic distances ($\sim$9.9 kpc and $\sim$
10.6 kpc respectively) of their recombination-line velocities (103$\pm$0.5 km/s
and 89.6$\pm$2.1 km/s respectively), G23.07-0.37 is at the near kinematic
distance (4.4$\pm$0.3 kpc) of its recombination-line velocity (82.7$\pm$2.0
km/s), and G23.27-0.27 is probably at the near kinematic distance (4.1$\pm$0.3
kpc) of its recombination-line velocity (76.1$\pm$0.6 km/s).
