  We introduce a method for measuring the slopes of mass profiles within dwarf
spheroidal (dSph) galaxies directly from stellar spectroscopic data and without
adopting a dark matter halo model. Our method combines two recent results: 1)
spherically symmetric, equilibrium Jeans models imply that the product of
halflight radius and (squared) stellar velocity dispersion provides an estimate
of the mass enclosed within the halflight radius of a dSph stellar component,
and 2) some dSphs have chemo-dynamically distinct stellar
\textit{sub}components that independently trace the same gravitational
potential. We devise a statistical method that uses measurements of stellar
positions, velocities and spectral indices to distinguish two dSph stellar
subcomponents and to estimate their individual halflight radii and velocity
dispersions. For a dSph with two detected stellar subcomponents, we obtain
estimates of masses enclosed at two discrete points in the same mass profile,
immediately defining a slope. Applied to published spectroscopic data, our
method distinguishes stellar subcomponents in the Fornax and Sculptor dSphs,
for which we measure slopes $\Gamma\equiv \Delta \log M / \Delta \log
r=2.61_{-0.37}^{+0.43}$ and $\Gamma=2.95_{-0.39}^{+0.51}$, respectively. These
values are consistent with 'cores' of constant density within the central
few-hundred parsecs of each galaxy and rule out `cuspy' Navarro-Frenk-White
(NFW) profiles ($d\log M/d\log r \leq 2$ at all radii) with significance $\ga
96%$ and $\ga 99%$, respectively. Tests with synthetic data indicate that our
method tends systematically to overestimate the mass of the inner stellar
subcomponent to a greater degree than that of the outer stellar subcomponent,
and therefore to underestimate the slope $\Gamma$ (implying that the stated NFW
exclusion levels are conservative).
