Siebert, A.; Famaey, B.; Binney, J.; Burnett, B.; Faure, C.; Minchev, I.; Williams, M. E. K.; Bienayme, O.; Bland-Hawthorn, J.; Boeche, C.; Gibson, Brad K.
Abstract:
Using the Radial Velocity Experiment (RAVE) survey, we recently brought to light a gradient in the mean galactocentric radial velocity of stars in the extended solar neighbourhood. This gradient likely originates from non-axisymmetric perturbations of the potential, among which a perturbation by spiral arms is a possible explanation. Here, we apply the traditional density wave theory and analytically model the radial component of the two-dimensional velocity field. Provided that the radial velocity gradient is caused by relatively long-lived spiral arms that can affect stars substantially above the plane, this analytic model provides new independent estimates for the parameters of the Milky Way spiral structure. Our analysis favours a two-armed perturbation with the Sun close to the inner ultra-harmonic 4:1 resonance, with a pattern speed Ωp = 18.6+0.3 −0.2 km s−1 kpc−1 and a small amplitude A = 0.55+0.02 −0.02 per cent of the background potential (14 per cent of the background density). This model can serve as a basis for numerical simulations in three dimensions, additionally including a possible influence of the Galactic bar and/or other non-axisymmetric modes.