2003/05/31 by Takashi Hamana, Issha Kayo, Naoki Yoshida +2
Environmental Science · Physics and Astronomy · #Galaxies: Formation, Evolution, Phenomena #Plant Water Relations and Carbon Dynamics #Remote Sensing in Agriculture #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2003.06787.x
published as Mon.Not.Roy.Astron.Soc. 343 (2003) 1312; Erratum-ibid. 357 (2005) 1407 · This paper was published in MNRAS, 343, 1312 (2003). Owing to an error in numerical computations, some incorrect results were presented there. Erratum is to be published in MNRAS. Conclusions of the original version are unaffected by the correction. This version supersedes the original version
openalex publication_date 2003/08/21 · arxiv created 2004/12/06 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We present a simple model that accurately describes various statistical properties of peculiar velocities of dark matter haloes. We pay particular attention to the following two effects. First, the evolution of the halo peculiar velocity depends on the local matter density, instead of the global density. Secondly, dark matter haloes are biased tracers of the underlying mass distribution, thus haloes tend to be located preferentially at high density regions. For the former, we develop an empirical model calibrated with N-body simulations while, for the latter, we use a conventional halo bias model based on the extended Press–Schechter model combined with an empirical lognormal probability distribution function of the mass density distribution. We find that, compared with linear theory, the present model significantly improves the accuracy of predictions of statistical properties of the halo peculiar velocity field including the velocity dispersion, the probability distribution function, and the pairwise velocity dispersion at large separations. Thus, our model predictions may be useful in analysing future observations of the peculiar velocities of galaxy clusters.