### Abstract

We study the properties of dark matter (DM) halos in several models in which we have included dark energy (DE). We consider both dynamical DE, due to a scalar field self-interacting through Ratra-Peebles or supergravity potentials, and DE with constant negative w = p/p > -1. We find that at zero redshift, both the nonlinear power spectrum of DM and the mass function of halos do not depend appreciably on the state equation of DE, which implies that both statistics are almost indistinguishable from those of Λ-dominated cold dark matter (ΛCDM). This result is consistent with the nonlinear treatment in the accompanying paper and is also a welcome feature, because ΛCDM fits a large variety of data. On the other hand, DE halos differ from ΛCDM halos in that they are denser in their central parts, because DE halos collapsed earlier. Neverthe-less, such differences are not so large. For example, the density at 10 kpc of a ∼10^{13} M_{⊙} DE halo is only 50% denser than the ΛCDM halo. This means that DE does not ease the problem with cuspy DM profiles. Addressing another cosmological problem, the abundance of subhalos, we find that the number of satellites of halos in various DE models does not change with respect to ΛCDM when normalized to the same circular velocity as the parent halo. Most of the above similarities are related to choosing for all models the same normalization factor σ_{8} at z = 0. At high redshifts, different DE and ΛCDM models have different amplitudes of fluctuations, which causes substantial deviations of halo properties to occur. Therefore, the way to find which DE equation of state gives the best fit to the observed universe is to look at the evolution of halo properties. For example, the abundance of galaxy groups with mass larger than 10^{13} h^{-1} M_{⊙} at z ≳ 2 can be used to discriminate between the models and thus to constrain the nature of DE.

Original language | English (US) |
---|---|

Pages (from-to) | 31-37 |

Number of pages | 7 |

Journal | Astrophysical Journal |

Volume | 599 |

Issue number | 1 I |

DOIs | |

State | Published - Dec 10 2003 |

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### Keywords

- Cosmology: theory
- Dark matter
- Galaxies: clusters: general
- Galaxies: halos
- Methods: analytical
- Methods: numerical

### ASJC Scopus subject areas

- Space and Planetary Science
- Nuclear and High Energy Physics

### Cite this

*Astrophysical Journal*,

*599*(1 I), 31-37. https://doi.org/10.1086/379237

**Halo properties in models with dynamical dark energy.** / Klypin, A.; Maccio, Andrea; Mainini, R.; Bonometto, S. A.

Research output: Contribution to journal › Article

*Astrophysical Journal*, vol. 599, no. 1 I, pp. 31-37. https://doi.org/10.1086/379237

}

TY - JOUR

T1 - Halo properties in models with dynamical dark energy

AU - Klypin, A.

AU - Maccio, Andrea

AU - Mainini, R.

AU - Bonometto, S. A.

PY - 2003/12/10

Y1 - 2003/12/10

N2 - We study the properties of dark matter (DM) halos in several models in which we have included dark energy (DE). We consider both dynamical DE, due to a scalar field self-interacting through Ratra-Peebles or supergravity potentials, and DE with constant negative w = p/p > -1. We find that at zero redshift, both the nonlinear power spectrum of DM and the mass function of halos do not depend appreciably on the state equation of DE, which implies that both statistics are almost indistinguishable from those of Λ-dominated cold dark matter (ΛCDM). This result is consistent with the nonlinear treatment in the accompanying paper and is also a welcome feature, because ΛCDM fits a large variety of data. On the other hand, DE halos differ from ΛCDM halos in that they are denser in their central parts, because DE halos collapsed earlier. Neverthe-less, such differences are not so large. For example, the density at 10 kpc of a ∼1013 M⊙ DE halo is only 50% denser than the ΛCDM halo. This means that DE does not ease the problem with cuspy DM profiles. Addressing another cosmological problem, the abundance of subhalos, we find that the number of satellites of halos in various DE models does not change with respect to ΛCDM when normalized to the same circular velocity as the parent halo. Most of the above similarities are related to choosing for all models the same normalization factor σ8 at z = 0. At high redshifts, different DE and ΛCDM models have different amplitudes of fluctuations, which causes substantial deviations of halo properties to occur. Therefore, the way to find which DE equation of state gives the best fit to the observed universe is to look at the evolution of halo properties. For example, the abundance of galaxy groups with mass larger than 1013 h-1 M⊙ at z ≳ 2 can be used to discriminate between the models and thus to constrain the nature of DE.

AB - We study the properties of dark matter (DM) halos in several models in which we have included dark energy (DE). We consider both dynamical DE, due to a scalar field self-interacting through Ratra-Peebles or supergravity potentials, and DE with constant negative w = p/p > -1. We find that at zero redshift, both the nonlinear power spectrum of DM and the mass function of halos do not depend appreciably on the state equation of DE, which implies that both statistics are almost indistinguishable from those of Λ-dominated cold dark matter (ΛCDM). This result is consistent with the nonlinear treatment in the accompanying paper and is also a welcome feature, because ΛCDM fits a large variety of data. On the other hand, DE halos differ from ΛCDM halos in that they are denser in their central parts, because DE halos collapsed earlier. Neverthe-less, such differences are not so large. For example, the density at 10 kpc of a ∼1013 M⊙ DE halo is only 50% denser than the ΛCDM halo. This means that DE does not ease the problem with cuspy DM profiles. Addressing another cosmological problem, the abundance of subhalos, we find that the number of satellites of halos in various DE models does not change with respect to ΛCDM when normalized to the same circular velocity as the parent halo. Most of the above similarities are related to choosing for all models the same normalization factor σ8 at z = 0. At high redshifts, different DE and ΛCDM models have different amplitudes of fluctuations, which causes substantial deviations of halo properties to occur. Therefore, the way to find which DE equation of state gives the best fit to the observed universe is to look at the evolution of halo properties. For example, the abundance of galaxy groups with mass larger than 1013 h-1 M⊙ at z ≳ 2 can be used to discriminate between the models and thus to constrain the nature of DE.

KW - Cosmology: theory

KW - Dark matter

KW - Galaxies: clusters: general

KW - Galaxies: halos

KW - Methods: analytical

KW - Methods: numerical

UR - http://www.scopus.com/inward/record.url?scp=0347460670&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0347460670&partnerID=8YFLogxK

U2 - 10.1086/379237

DO - 10.1086/379237

M3 - Article

AN - SCOPUS:0347460670

VL - 599

SP - 31

EP - 37

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 I

ER -