  In a previous paper (Paper I) a method was developed to determine the shapes
of dark matter halos of spiral galaxies from the flaring and velocity
dispersion of the gas layer. Here I present the results for the almost edge-on
Scd galaxy NGC 4244 (Paper II Paper III) and preliminary results for the Milky
Way. NGC 4244's dark matter halo is found to be highly flattened with a
shortest-to-longest axis ratio of 0.2 +0.3-0.1. If the dark matter is
disk-like, the vertical velocity dispersion of the dark matter must be ~20%
larger than the measured tangential dispersion in the HI. The flaring of the
Milky Way's gas layer, the local column of identified stars and the total
column within 1.1 kpc from the plane are consistent with a moderately flattened
dark halo (E7-E0) and galactic constants of \RSUN = 7.1 kpc, \VSUN = 180 \kms,
while the stellar disk is ~80% of maximal.
