  The leading tensions to the collisionless cold dark matter (CDM) paradigm are
the "small-scale controversies", discrepancies between observations at the
dwarf-galactic scale and their simulational counterparts. In this work we
consider methods to infer 3D morphological information on Local Group dwarf
spheroidals, and test the fitness of CDM+hydrodynamics simulations to the
observed galaxy shapes. We find that the subpopulation of dwarf galaxies with
mass-to-light ratio $\gtrsim 100 M_\odot/L_\odot$ reflects an oblate
morphology. This is discrepant with the dwarf galaxies with mass-to-light ratio
$\lesssim 100 M_\odot/L_\odot$, which reflect prolate morphologies, and more
importantly with simulations of CDM-sourced galaxies which are explicitly
prolate. Although more simulations and data are called for, if evidence of
oblate pressure-supported stellar distributions persists, we argue that an
underlying oblate non-CDM dark matter halo may be required, and present this as
motivation for future studies.
