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How to Build an Empirical Speed Distribution for Dark Matter in the Solar Neighborhood

  • Authors: Tal Shpigel, Dylan Folsom, Mariangela Lisanti, Lina Necib, Mark Vogelsberger, Lars Hernquist

Tal Shpigel et al 2026 The Astrophysical Journal 1003 .

  • Provider: AAS Journals

Caption: Figure B2.

Boost factor Δσ as a function of the infall time for all Traceable mergers (circles). GSE-like mergers are highlighted separately (stars). Mergers with earlier infall times tend to show smaller dispersion offsets. Those with infall times greater than 11 Gyr have a median offset of ﹩{9}_{-5}^{+2}\,\,\rm{km}\,\,{\,\rm{s}\,}^{-1}﹩, while those with infall times less than 11 Gyr have a median offset of ﹩1{5}_{-7}^{+6}\,\,\rm{km}\,\,{\,\rm{s}\,}^{-1}﹩. This trend is consistent with the mechanism highlighted in Figure B1. When mergers fall in earlier, both their DM and stars are deposited at smaller radii because the MW itself was smaller, reducing the difference in potential energies and thus the dispersion offset.

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