In a previous paper ( Olling 1995 ) a method was developed to determine the shapes of dark matter halos of spiral galaxies from an accurate determination of the rotation curve , the flaring of the gas layer and the velocity dispersion in the H I .
Here I report the results for the almost edge-on Scd galaxy NGC 4244 ( Olling 1996a , 1996b ) .

The observed flaring of the H I beyond the optical disk puts significant constraints on the shape of the dark matter halo , which are almost independent of the stellar mass-to-light ratio .
NGC 4244 ’ s dark matter halo is found to be highly flattened with a shortest-to-longest axis ratio of 0.2 _ { -0.1 } ^ { +0.3 } .
If the dark matter is disk-like , the data presented in this paper imply that the vertical velocity dispersion of the dark matter must be 10 % - 30 % larger than the measured tangential dispersion in the H I .