Discussions continued at Flatiron about Galactic dynamics and actions. We laid out uses for actions and then discussed more results from Beane (Flatiron) on the inconsistency of actions when you have wrong coordinate systems or potential.
Stars meeting featured various interesting discussions. But during a discussion led by Kreidberg (Harvard) about temperature-mapping hot rocky planets, I had an idea: We could use the strong absorption lines in stellar spectra to increase the planet-to-star brightness ratio. If we have full-phase coverage with high-resolution spectroscopy, we can look for the hot planet to “fill in” some of the absorption lines at full phases, and the amount it fills in for lines at different wavelengths would tell you the temperature (or low-resolution spectrum) of the planet! I want to do this with our HARPS data and our wobble pipeline!
In the afternoon, Boris Leistedt (NYU) and I made a plan with David Blei (Columbia) and Andrew Miller (Columbia) to build our 3-d dust model out of dust measurements. There are many problems to solve! But we are starting by assuming that Leistedt's data-driven dust measurements are correct and have Gaussian noise, the stellar positions are well known, and the dust field can be represented by a Gaussian process. In terms of challenges, we are starting by working on the scaling problem: How to make things run on millions or hundreds of millions of stars at a time? One dispute we had is about what line-of-sight integral of the dust corresponds to the extinction?
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