paper

Mass of clusters in simulations

arXiv:astro-ph/0301247 · doi:10.1086/373944

Abstract

We show that DM halos, in n--body simulations, have a boundary layer (BL), separating bound from unbound mass. Let T(r) and W(r) be the kinetic and potential energies in shells of halos. We find that, in almost all halos: (i) The virial ratio R=-2T/W has at least one persistent (i.e. resolution independent) minimum r_c, such that, close to it, (ii) the function w=-d log W/d log r has a maximum and (iii) the relation R(r_c)=w(r_c) is almost exactly fulfilled. The radius r_c is the position of BL's, in halos found in simulations of TCDM and LCDM models, run using ART and GADGET codes at various resolutions. We find that 97% of the ~300 halos (per model) with M>4.2 10^14 M_s h^-1 owns a BL. Those with no BL are undergoing major mergings. The mass M_c enclosed in r_c almost coincides with the mass evaluated from velocities, according to virial theorem. Particles at r>r_c are not in virial equilibrium. Using r_c we have a density contrast Δ_c for each halo. For each mass scale, Δ_v=178 Omega_m^0.45 is within the range of Δ_c's, but the spread in Δ_c is wide and the average Δ_c is ~25% smaller than the corresponding Δ_v. The matching of properties derived under the assumption of spherical symmetry is a consequence of violent relaxation destroying features related to previous ellipsoidal non-linear growth. In turn, the spread of final Δ_c's is an imprint of the different 3-D geometries and of the variable environment during collapses, as suggested by a comparison with Sheth & Tormen analysis.

19 Pages, 15 figures, ApJ in press

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