The Halo Density Profiles with Non-Standard N-body Simulations

Abstract

We propose a new numerical procedure to simulate a single dark halo of any size and mass in a hierarchical framework coupling the extended Press-Schechter formalism (EPSF) to N-body simulations. The procedure consists of assigning cosmological initial conditions to the particles of a single halo with a EPSF technique and following only the dynamical evolution using a serial N-body code. The computational box is fixed with a side of $0.5h^{-1}$ Mpc. This allows to simulate galaxy cluster halos using appropriate scaling relations, to ensure savings in computing time and code speed. The code can describe the properties of halos composed of collisionless or collisional dark matter. For collisionless Cold Dark Matter (CDM) particles the NFW profile is reproduced for galactic halos as well as galaxy cluster halos. Using this numerical technique we study some characteristics of halos assumed to be isolated or placed in a cosmological context in presence of weak self-interacting dark matter: the soft core formation and the core collapse. The self-interacting dark matter cross section per unit mass is assumed to be inversely proportional to the particle collision velocity: $\sigma /m_x\propto 1/v$.

Accepted for publication in MNRAS (2 figures added)

References in corpus (6)

• Concentrations of Dark Halos from their Assembly Histories
• H alpha rotation curves of Low Surface Brightness galaxies
• Orbital perturbations on transiting planets: A possible method to measure stellar quadrupoles and to detect Earth-mass planets
• Halpha rotation curves: the soft core question
• Chandra Observations of the Lensing Cluster EMSS 1358+6245: Implications for Self-Interacting Dark Matter
• Observational Constraints on the Self Interacting Dark Matter Scenario and the Growth of Supermassive Black Holes

Cited by in corpus (7)

• Subhaloes in Self-Interacting Galactic Dark Matter Haloes
• Gravothermal collapse of isolated self-interacting dark matter haloes: N-body simulation versus the fluid model
• Probing Dark Energy at Galactic and Cluster Scales
• The Failure of Self-Interacting Dark Matter to solve the Overabundance of Dark Satellites and the Soft Core Question
• The role of baryons in self-interacting dark matter mergers
• The Dark Halo of NGC 5963 as a Constraint on Dark Matter Self-Interaction at the Low Velocity Regime
• Cusped Mass Density Profiles and Magnification Ratios of Double Image Gravitational Lenses