2023MNRAS.524.3596D

Using data from the Gaia satellite's Radial Velocity Spectrometer Data Release 3 (RVS, DR3), we find a new and robust feature in the phase-space distribution of halo stars. It is a prominent ridge at constant energy and with angular momentum L_z > 0. We run test particle simulations of a stellar halo-like distribution of particles in a realistic Milky Way potential with a rotating bar. We observe similar structures generated in the simulations from the trapping of particles in resonances with the bar, particularly at the corotation resonance. Many of the orbits trapped at the resonances are halo like, with large vertical excursions from the disc. The location of the observed structure in energy space is consistent with a bar pattern speed in the range Ω_b ≈ 35-40 km s^–1 kpc^–1. Overall, the effect of the resonances is to give the inner stellar halo a mild, net spin in the direction of the bar's rotation. As the distribution of the angular momentum becomes asymmetric, a population of stars with positive mean L_z and low vertical action is created. The variation of the average rotational velocity of the simulated stellar halo with radius is similar to the behaviour of metal-poor stars in data from the APOGEE survey. Though the effects of bar resonances have long been known in the Galactic disc, this is strong evidence that the bar can drive changes even in the diffuse and extended stellar halo through its resonances.