Today David Spergel (Flatiron) came by to discuss the following question: How much do we know—empirically—about fluctuations or clustering in the dark matter distribution in the Milky Way halo? Spergel's idea is maybe to use old or metal-poor halo stars: Since stars form in the centers of their DM halos (we think), the clustering or fluctuations in phase space of the old stars should always be larger than the clustering or fluctuations in the dark matter. I bet that's true! And it's easy to test in standard simulations, I think.
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