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 $\bar v_φ$ 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 $\bar v_φ$ 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 our ideal case of galactocentric velocities with null uncertainties and no observational limitations, 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 example, for a spherical DM halo, $S$ drops from $\sim 98\%$ to $\sim 38\%$ when the sample size decreases from $\sim 800$ to $\sim 40$ HVSs. A robust determination of the shape of the DM potential thus requires the measure of the galactocentric velocity of a few hundred genuine HVSs.