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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 731856.0, MPI für Astronomie / Publikationen_mpia
Effects of coupled dark energy on the Milky Way and its satellites
Authors:Penzo, C.; Macciò, A. V.; Baldi, M.; Casarini, L.; Oñorbe, J.; Dutton, A. A.
Date of Publication (YYYY-MM-DD):2016
Title of Journal:Monthly Notices of the Royal Astronomical Society
Issue / Number:3
Start Page:2490
End Page:2501
Audience:Not Specified
Abstract / Description:We present the first numerical simulations in coupled dark energy cosmologies with high enough resolution to investigate the effects of the coupling on galactic and subgalactic scales. We choose two constant couplings and a time-varying coupling function and we run simulations of three Milky Way-sized haloes (˜1012 M), a lower mass halo (6 × 1011 M) and a dwarf galaxy halo (5 × 109 M). We resolve each halo with several million dark matter particles. On all scales, the coupling causes lower halo concentrations and a reduced number of substructures with respect to Λ cold dark matter (ΛCDM). We show that the reduced concentrations are not due to different formation times. We ascribe them to the extra terms that appear in the equations describing the gravitational dynamics. On the scale of the Milky Way satellites, we show that the lower concentrations can help in reconciling observed and simulated rotation curves, but the coupling values necessary to have a significant difference from ΛCDM are outside the current observational constraints. On the other hand, if other modifications to the standard model allowing a higher coupling (e.g. massive neutrinos) are considered, coupled dark energy can become an interesting scenario to alleviate the small-scale issues of the ΛCDM model.
Free Keywords:methods: numerical; galaxies: evolution; galaxies: formation; galaxies: haloes; dark energy; dark matter
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 %R 10.1093/mnras/stw1502
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