I had a call today with Eilers (MIT) and Rix (MPIA) about making self-consistent perturbations to a simple galaxy disk model and interpreting kinematic signatures therein. We have been doing this for months but there are still some conceptual issues that are difficult. Like can we really confine our perturbation to the disk plane, or do we have to give it non-trivial three-dimensional structure. We don't all agree, but we are getting closer. It turns out: Dynamics is hard!
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