We analyze the HI absorption profile for TeV Supernova Remnant ( SNR ) G349.7+0.2 based on updated knowledge of the inner Galaxy ’ s structure .
We significantly revise its kinematic distance from the previous \sim 22 kpc to \sim 11.5 kpc , indicating it is in the far 3 kpc arm of the Galactic center .
We give a revised age of \sim 1800 year for G349.7+0.2 which has a low explosion energy of \sim 2.5 \times 10 ^ { 50 } ergs .
This removes G349.7+0.2 from the set of brightest SNRs in radio and X-ray to \gamma -ray wavebands and helps us to better understand \gamma -ray emission originating from this remnant .
However , one needs to use caution when discussing old kinematic distances of Galactic objects ( e.g. , SNRs , pulsars and HII regions ) in the range of -12 ^ { 0 } \leq l \leq 12 ^ { 0 } with distance estimates of \geq 5.5 kpc .