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tokens: a method to infer the slope of the underlying DM halo at the average half-light radius , finding that both the Fornax and the Sculptor dSph must be embedded in DM haloes with constant-density cores, in conflict with the centrally divergent density cusps of haloes in DM-only simulations (the cusp/core problem ). Laporte, Walker Peñarrubia ( 2013 ) subsequently showed that also for triaxial DM haloes, the Walker Peñarrubia ( 2011 ) method gives reliable lower limits on the slope Γ. Sawala et al. ( 2015 ) use halo masses derived by Peñarrubia et al. ( 2008a ) for Milky Way dSphs using the Walker et al. ( 2009c ) estimator to motivate their corrections to stellar mass–halo mass relations obtained from abundance matching based on DM-only simulations. More recently, Fattahi et al. ( 2018 ) make use of the Wolf et al. ( 2010 ) estimator to study the tidal evolution DM haloes of the apostle simulations compatible with the observed kinematics of Milky Way dSphs. In this contribution, we study a virial mass estimator which is minimally affected by our ignorance on two key parameters: (i) the shape of the inner DM halo profile, and (ii) the spatial segregation of the stellar tracers within the DM halo. The use of the projected spherical virial theorem has several advantages over Jeans analysis for the construction of mass estimators: The virial theorem does not contain any functional dependence on β( r ) and thereby avoids the mass–anisotropy degeneracy. Also systematic biases of inferred enclosed masses and slopes Γ follow directly from the assumptions made on the DM and stellar density profiles and are independent of sample size. Furthermore, the average squared dispersion is a sum over all stars and does not require any binning of data. This makes mass estimators based on the virial theorem applicable also to systems with only few stellar tracers – carefully factoring in the uncertainties due to sample size on the measured squared velocity dispersion as pointed out by Laporte, Agnello Navarro ( 2018 ). This paper is structured as follows: in Section 2 we introduce the spherical virial theorem and discuss the systematics of mass estimators for dwarf galaxies consisting of a stellar tracer population embedded inside a DM halo. In Section 3 , we construct a mass estimator which is tailored to minimize the uncertainty introduced by our ignorance on the central slope of the underlying DM profile as well as on how deeply embedded the stellar component is within the DM halo. We do test this mass estimator on a catalogue of N -body mocks. Section 4 discusses how to obtain the total halo masses of dwarf galaxies, breaking the degeneracy between structural parameters constrained by use of the virial theorem with the help of controlled cosmological simulations. In Section 5 , we estimate the masses of Milky Way dwarf galaxies using the methods introduced in the previous sections, and discuss implications of the derived stellar mass–halo mass relation for