VLA D-configuration mosaics of relatively small fields of Galactic H I emission
reveal complicated filaments and structures on all angular
scales. With an ultra-compact antenna configuration it will be possible
to survey H I in large parts of the Galactic plane with an angular
resolution of 
and a velocity resolution of 0.5 km/s in a very short
time. A survey covering one quadrant and 10 degrees of Galactic
latitude would take only 120 hour of observing to complete. A high
resolution, fully sampled survey of Galactic H I would provide an
important data base for: i) modeling gas dynamics in the Galaxy; ii)
comparing H I with molecular gas, allowing detailed modeling of the
conversion between atomic and molecular gas in molecular clouds or
photodissociation regions; iii) comparison with continuum emission,
possibly allowing a distance determination to continuum features if an
H I/continuum correlation is found; iv) the study of the interaction
between violent events in the disk - SNR, disk blowout events, H II
regions - and H I.
Technical requirements include: