We have analyzed the archival data of FUV observations for the region of GSH 006-15+7 , a large shell-like structure discovered by Moss et al .
( 30 ) from the H i velocity maps .
FUV emission is seen to be enhanced in the lower supershell region .
The FUV emission is considered to come mainly from the scattering of interstellar photons by dust grains .
A corresponding Monte Carlo simulation indicates that the distance to the supershell is 1300 \pm 800 pc , which is similar to the previous estimation of 1500 \pm 500 pc based on kinematic considerations .
The spectrum at lower Galactic latitudes of the supershell exhibits molecular hydrogen fluorescence lines ; a simulation model for this candidate photodissociation region ( PDR ) yields an H _ { 2 } column density of N ( H _ { 2 } ) = 10 ^ { 18.0 - 20.0 } cm ^ { -2 } with a rather high total hydrogen density of n _ { H } \sim 30 cm ^ { -3 } .