The effect of a disc on the population of cuspy and cored dark matter substructures in Milky Way-like galaxies

Raphaël Errani, Jorge Penarrubia, Chervin F. P. Laporte, Facundo Gomez

Research output: Contribution to journalArticlepeer-review

Abstract / Description of output

We use high-resolution N-body simulations to study the effect of a galactic disc on the dynamical evolution of dark matter substructures with orbits and structural parameters extracted from the Aquarius A-2 merger tree. Satellites are modelled as equilibrium N-body realizations of generalized Hernquist profiles with 2 × 106 particles and injected in the analytical evolving host potential at zinfall, defined by the peak of their mass evolution. We select all substructures with M200(zinfall) > 108 M⊙ and first pericentric distances rp < r200. Motivated by observations of Milky Way dwarf spheroidal galaxies, we also explore satellite models with cored dark matter profiles with a fixed core size rc = 0.8 as, where as is the Hernquist scale radius. We find that models with cuspy satellites have twice as many surviving substructures at z = 0 than their cored counterparts, and four times as many if we only consider those on orbits with rp < 0.1 r200. For a given profile, adding an evolving disc potential reduces the number of surviving substructures further by a factor of &lt2 for satellites on orbits which penetrate the disc (rp < 20 kpc). For large rp, where tidal forces and the effect of the disc become negligible, the number of satellites per pericentre bin converges to similar values for all four models.
Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society: Letters
DOIs
Publication statusPublished - 16 Nov 2016

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