To be or not to be oblate: the shape of the dark matter halo in the
  polar ring galaxies
  With the aim to determine the spatial distribution of the dark matter halo,
we investigate two polar ring galaxies NGC 4262 and SPRC-7. For both galaxies
the stellar kinematics data for the central galaxy were obtained from optical
spectroscopy at the 6-m telescope of the Special Astrophysical Observatory of
the Russian Academy of Sciences. The information about polar gaseous components
was taken from the optical 3D-spectroscopic observations of ionized gas (for
SPRC-7) and H {\sc i} radio observations (for NGC 4262). SPRC-7 is the system
with a relative angle $\delta=73^{\circ}$ towards the central galaxy and a
quite massive stellar-gaseous polar component. Meanwhile NGC 4262 is the
classic polar case with $\delta=88^{\circ}$ where the polar ring mainly
consists of neutral gas with a negligible stellar contribution to the mass. We
are hence dealing with two different systems and the results are quite diverse
too. The observed properties of both galaxies were compared with the results of
self consistent simulations of velocity fields of the polar component along
with the rotation curve of the central lenticular galaxy. For SPRC-7 we have
found a slightly flattened halo towards the polar plane with the axis ratio
$c/a \simeq 1.7 \pm 0.2$ for the isothermal halo model and $c/a \simeq 1.5 \pm
0.2$ for the NFW model. The case of NGC 4262 is more unusual, the shape of the
dark matter distribution varies strongly with radius. Namely, the dark matter
halo is fattened in the vicinity of the galactic disc ($c/a \approx 0.4 \pm
0.1$), however it is prolate far beyond the central galaxy ($c/a \approx 1.7$
for the isothermal halo and $c/a \approx 2.3$ for NFW).
