Implications of a contracted dark matter halo for the Milky Way’s inferred virial mass

We investigate how reliably the global properties of Milky Way–mass dark matter haloes can be recovered from dynamical data from a limited range of radii, particular ≲ 30kpc where observations are most sensitive but baryonic processes modify the halo structure. Using the ARTEMIS simulations, which produce varying degrees of baryon-induced contraction, we fit dark matter profiles over restricted radial ranges using commonly adopted parametric models. Assuming negligible observational uncertainties allows the systematic errors from these choices to be isolated. When fits are confined to inner radii, an NFW profile underestimates the virial mass by a factor of ≈2 on average (≈4 for some systems), and the concentration by a factor of ≈2. Einasto and generalised-NFW models provide excellent local fits but retain similar global biases. In contrast, a contracted halo prescription yields stable extrapolations and recovers unbiased halo mass estimates over all radii. The inferred mass improves systematically with increasing radial coverage, and tracers beyond ≳ 50 kpc largely eliminate the mean bias for all models. The local dark matter density at the Solar radius is recovered to within ≲ 5% for all profiles other than NFW. These biases are sufficient to reconcile recent low Milky Way mass estimates derived from inner rotation-curve analyses with the canonical ≈1012M⊙. We additionally find a halo-to-halo scatter of ≳ 0.1 dex (≈25%) persists even under idealised conditions, setting a likely lower limit for the precision of halo mass estimates.