Measuring the slopes of mass profiles for dwarf spheroidals in triaxial
  CDM potentials
  We generate stellar distribution functions (DFs) in triaxial haloes in order
to examine the reliability of slopes $\Gamma\equiv \Delta {\rm log} M / \Delta
{\rm log} r$ inferred by applying mass estimators of the form $M\propto
R_e\sigma^2$ (i.e. assuming spherical symmetry, where $R_e$ and $\sigma$ are
luminous effective radius and global velocity dispersion, respectively) to two
stellar sub-populations independently tracing the same gravitational potential.
The DFs take the form $f(E)$, are dynamically stable, and are generated within
triaxial potentials corresponding directly to subhaloes formed in cosmological
dark-matter-only simulations of Milky Way and galaxy cluster haloes.
Additionally, we consider the effect of different tracer number density
profiles (cuspy and cored) on the inferred slopes of mass profiles. For the
isotropic DFs considered here, we find that halo triaxiality tends to introduce
an anti-correlation between $R_e$ and $\sigma$ when estimated for a variety of
viewing angles. The net effect is a negligible contribution to the systematic
error associated with the slope of the mass profile, which continues to be
dominated by a bias toward greater overestimation of masses for
more-concentrated tracer populations. We demonstrate that simple mass estimates
for two distinct tracer populations can give reliable (and cosmologically
meaningful) lower limits for $\Gamma$, irrespective of the degree of
triaxiality or shape of the tracer number density profile.
