I had an absolutely great meeting this morning with Danny Horta-Darrington (Flatiron) and Adrian Price-Whelan (Flatiron), in which Horta showed us plots of various stellar surface abundances as a function of dynamical quasi-invariants in the Milky Way. That is, abundance gradients! But abundance gradients get stronger and more informative when they are plotted in terms of dynamical invariants than when they are plotted versus position (say), because positions of stars change with time. There is so much information for us to use here!
One thing we discussed is what units or transformations of the dynamical invariants we should plot. We're leaning towards the transformations that have units of length, which are guiding radius, z-max, and radial span.
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