Using 21 cm H i observations from the Parkes Radio Telescope ’ s Galactic All-Sky Survey , we measure 255 H i clouds in the lower Galactic halo that are located near the tangent points at 16.9 \arcdeg \leq l \leq 35.3 \arcdeg and |b| \lesssim 20 \arcdeg .
The clouds have a median mass of 700 M _ { \odot } and a median distance from the Galactic plane of 660 pc .
This first Galactic quadrant ( QI ) region is symmetric to a region of the fourth quadrant ( QIV ) studied previously using the same data set and measurement criteria .
The properties of the individual clouds in the two quadrants are quite similar suggesting that they belong to the same population , and both populations have a line of sight cloud-cloud velocity dispersion of \sigma _ { cc } \approx 16 km s ^ { -1 } .
However , there are three times as many disk-halo clouds at the QI tangent points and their scale height , at h = 800 pc , is twice as large as in QIV .
Thus the observed line of sight random cloud motions are not connected to the cloud scale height or its variation around the Galaxy .
The surface density of clouds is nearly constant over the QI tangent point region but is peaked near R \sim 4 kpc in QIV .
We ascribe all of these differences to the coincidental location of the QI region at the tip of the Milky Way ’ s bar , where it merges with a major spiral arm .
The QIV tangent point region , in contrast , covers only a segment of a minor spiral arm .
The disk-halo H i cloud population is thus likely tied to and driven by large-scale star formation processes , possibly through the mechanism of supershells and feedback .