N-body simulations for coupled dark energy: halo mass function and density profiles
We present the results of a series of N-body simulations in cosmologies where dark matter (DM) is coupled to dark energy (DE), so easing the cosmic coincidence problem. The dark-dark coupling introduces two novel effects in N-body dynamics: (i) DM particle masses vary with time; (ii) gravity between...
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| Main Authors: | , |
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| Format: | Article (Journal) Chapter/Article |
| Language: | English |
| Published: |
2003
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| In: |
Arxiv
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| Online Access: | Verlag, kostenfrei, Volltext: http://arxiv.org/abs/astro-ph/0309671
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| Author Notes: | A.V. Macciò, C. Quercellini, R. Mainini, L. Amendola & S.A. Bonometto |
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| 100 | 1 | |a Macciò, Andrea V. |d 1975- |e VerfasserIn |0 (DE-588)1125037520 |0 (DE-627)1772230561 |0 (DE-576)483289434 |4 aut | |
| 245 | 1 | 0 | |a N-body simulations for coupled dark energy |b halo mass function and density profiles |c A.V. Macciò, C. Quercellini, R. Mainini, L. Amendola & S.A. Bonometto |
| 264 | 1 | |c 2003 | |
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| 520 | |a We present the results of a series of N-body simulations in cosmologies where dark matter (DM) is coupled to dark energy (DE), so easing the cosmic coincidence problem. The dark-dark coupling introduces two novel effects in N-body dynamics: (i) DM particle masses vary with time; (ii) gravity between DM particles is ruled by a constant $G^{*}$, greater than Newton's constant $G$, holding in other 2-body interactions. As a consequence, baryons and DM particle distributions develop a large scale bias. Here we investigate DE models with Ratra-Peebles (RP) potentials; the dark-dark coupling is set in a parametric range compatible with observations, for as concern background and linear perturbation properties. We study the halo mass function, the halo density profile and the behavior of the non-linear bias. We find that non-linear dynamics puts additional constraints to the coupling parameter. They mostly arise from density profiles, that we find to yield higher concentrations, in coupled RP models, with respect to (uncoupled) dynamical DE cosmologies. Such enhancement, although being a strong effect in some coupling parameter range, is just a minor change for smaller but significant values of the coupling parameter. With these further restrictions, coupled DE models with RP potential are consistent with non-linear observables. | ||
| 650 | 4 | |a Astrophysics | |
| 700 | 1 | |a Amendola, Luca |d 1963- |e VerfasserIn |0 (DE-588)1029171270 |0 (DE-627)732547482 |0 (DE-576)377045128 |4 aut | |
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