Probing the shape of the Milky Way dark matter halo with hypervelocity stars: a new method

We propose a new method to determine the shape of the gravitational potential of the dark matter (DM) halo of the Milky Way (MW) with the galactocentric tangential velocities of a sample of hypervelocity stars (HVSs). We compute the trajectories of different samples of HVSs in a MW where the baryon distribution is axisymmetric and the DM potential either is spherical or is spheroidal or triaxial with radial-dependent axis ratios. We determine the shape of the DM potential with the distribution of the latitudinal velocity $|v_{\vartheta}|$ in axisymmetric Galactic potentials, or with the distribution of $|v_{\vartheta}|$ and of a function $\bar v_{\varphi}$ of the azimuthal velocity in non-axisymmetric Galactic potentials. We recover the correct shape of the DM potential by comparing the distribution of $|v_{\vartheta}|$ and $\bar v_{\varphi}$ against the corresponding distributions of mock samples of HVSs that traveled in DM halos of different shapes. We use the largest possible sample of $\sim 800$ HVSs of $4~M_\odot$ ejected with the Hills mechanism at a rate $\sim 10^{-4}$ yr$^{-1}$, currently outgoing, and located at more than 10 kpc from the Galactic center. In the ideal case of galactocentric velocities with null uncertainties, our method recovers the correct shape of the DM potential with a success rate $S\gtrsim 89\%$ in axisymmetric Galactic potentials, and $S > 96\%$ in the explored non-axisymmetric cases. The unsuccessful cases yield axis ratios of the DM potential that are off by $\pm 0.1$. The success rate decreases with decreasing sample size: for $\sim 80$ HVSs, close to the current number of HVS candidates, $S$ is in the range $\sim 40\%-60\%$, depending on the actual shape of the DM halo. A robust determination of the shape of the DM potential thus requires increasing by a factor $\sim 10$ the size of the sample of genuine HVSs with measured galactocentric velocity.