Presentation #311.06 in the session The Milky Way.
The recent discovery of a spiral pattern in the vertical kinematic structure in the solar neighborhood provides a prime opportunity to study non-equilibrium dynamics in the Milky Way from local stellar kinematics. Furthermore, results from simulations indicate that even in a limited volume, differences in stellar orbital histories allow us to trace variations in the initial perturbation across large regions of the disk. I will introduce , a novel algorithm we developed for studying these variations in both simulated and observed data sets. automatically extracts key quantities from the structure of a given phase spiral, including the time since perturbation and the perturbation mode. We have demonstrated ’s performance on simulated data where we show that it is capable of accurately recovering information about the time since the perturbation occurred as well as subtle differences in phase spiral morphology due to stellar location in the disk at the time of perturbation. Applying to kinematic data from data release 3 of the Gaia mission in bins of guiding radius, we show that similar structural differences in morphology occur in the Gaia phase spirals as a function of stellar orbital history. These results indicate that the phase spirals are the product of a complex dynamical response in the disk with large-scale coupling between different regions of phase space.