Mass of clusters in simulations

Andrea Maccio, Giuseppe Murante, Silvio P. Bonometto

Research output: Contribution to journalArticle

Abstract

We show that dark matter halos in N-body simulations have a boundary layer (BL), which neatly separates dynamically bound mass from unbound materials. We define T(r) and W(r) as the differential kinetic and potential energy of halos and evaluate them in spherical shells. We notice that in simulated halos such differential quantities fulfill the following properties: (1) the differential virial ratio ℛ = -2T/W has at least one persistent (resolution-independent) minimum r̄, such that, close to r̄, (2) the function w = -d log W/d log r has a maximum, while (3) the relation ℛ(r̄) ≃ w(r̄) holds. BLs are set where these three properties are fulfilled, in halos found in simulations of "tilted" Einstein-de Sitter and ACDM models, run ad hoc, using the ART and GADGET codes; their presence is confirmed in larger simulations of the same models with a lower level of resolution. Here we find that ∼97% of the ∼300 clusters (per model) we have with M > 4.2 × 1014 h-1 M own a BL. Those clusters that appear not to have a BL are seen to be undergoing major merging processes and to grossly violate spherical symmetry. The radius r̄ ≡ rc has significant properties. First of all, the mass Mc it encloses almost coincides with the mass Mdyn evaluated from the velocities of all particles within rc, according to the virial theorem. Also, materials at r > rc are shown not be in virial equilibrium. Using rc we can then determine an individual density contrast Δc for each virialized halo, which we compare with the "virial" density contrast Δv ≃ 178Ωm0.45 (where Ωm is the matter density parameter) obtained assuming a spherically symmetric and unperturbed fluctuation growth. As expected, for each mass scale, Δv is within the range of values Δc. However, the spread in Δc is wide, while the average Δc is ∼25% smaller than the corresponding Δv. We argue that the matching of properties derived under the assumption of spherical symmetry must be a consequence of an approximate sphericity, after violent relaxation destroyed features related to ellipsoidal nonlinear growth. On the contrary, the spread of the final Δc is an imprint of the different initial three-dimensional geometries of fluctuations and of the variable environment during their collapse, as suggested by a comparison of our results with the Sheth & Tormen analysis.

Original languageEnglish (US)
Pages (from-to)35-49
Number of pages15
JournalAstrophysical Journal
Volume588
Issue number1 I
DOIs
StatePublished - May 1 2003

Fingerprint

halos
boundary layer
boundary layers
simulation
symmetry
potential energy
virial theorem
kinetic energy
spherical shells
shell
dark matter
geometry
radii
material

Keywords

  • Cosmology: theory
  • Dark matter
  • Galaxies: clusters: general
  • Large-scale structure of universe
  • Methods: N-body simulations

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Maccio, A., Murante, G., & Bonometto, S. P. (2003). Mass of clusters in simulations. Astrophysical Journal, 588(1 I), 35-49. https://doi.org/10.1086/373944

Mass of clusters in simulations. / Maccio, Andrea; Murante, Giuseppe; Bonometto, Silvio P.

In: Astrophysical Journal, Vol. 588, No. 1 I, 01.05.2003, p. 35-49.

Research output: Contribution to journalArticle

Maccio, A, Murante, G & Bonometto, SP 2003, 'Mass of clusters in simulations', Astrophysical Journal, vol. 588, no. 1 I, pp. 35-49. https://doi.org/10.1086/373944
Maccio, Andrea ; Murante, Giuseppe ; Bonometto, Silvio P. / Mass of clusters in simulations. In: Astrophysical Journal. 2003 ; Vol. 588, No. 1 I. pp. 35-49.
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