We investigate interstellar absorption from molecular hydrogen ( H _ { 2 } ) and metals in an intermediate-velocity cloud ( IVC ) in the direction of the LMC star Sk -68 80 ( HD 36521 ) , based on data from the Far Ultraviolet Spectroscopic Explorer ( FUSE ) satellite .
H _ { 2 } absorption from the Lyman- and Werner bands is detected in 30 lines at radial velocities v _ { LSR } \approx + 50 km s ^ { -1 } in this IVC that is presumably located in the Milky Way halo .
We obtain a total logarithmic H _ { 2 } column density of log N ( H _ { 2 } ) = 16.6 \pm 0.5 
along with a very low Doppler parameter of b = 1.5 ^ { +0.8 } _ { -0.2 } km s ^ { -1 } .
The presence of molecular material in this cloud is suprising , given the fact that the O i column density ( log N ( O i ) = 14.8 \pm 0.1 ) implies a very low neutral gas column density of \sim 10 ^ { 18 } cm ^ { -2 } ( assuming a solar oxygen abundance ) .
If the H _ { 2 } column density represents its abundance in a formation-dissociation equilibrium , the data imply that the molecular gas resides in a small , dense filament at a volume density of \sim 800 cm ^ { -3 } and a thickness of only 41 Astronomical Units ( AU ) .
The molecular filament possibly corresponds to the tiny-scale atomic structures ( TSAS ) in the diffuse interstellar medium observed in high-resolution optical data , H i 
21cm absorption , and in CO emission .