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The spin and orientation of dark matter halos within cosmic filaments | | Youcai Zhang
; Xiaohu Yang
; Andreas Faltenbacher
; Volker Springel
; Weipeng Lin
; Huiyuan Wang
; | | Date: |
9 Jun 2009 | | Abstract: | Clusters, filaments, sheets and voids are the building blocks of the cosmic
web. In this study, we present and compare two distinct algorithms for finding
cosmic filaments and sheets, a task which is far less well established than the
identification of dark matter halos or voids. One method is based on the
smoothed dark matter density field, the other uses the halo distributions
directly. We apply both techniques to one high resolution N-body simulation and
reconstruct the filamentary/sheet like network of the dark matter density
field. We focus on investigating the properties of the dark matter halos inside
these structures, in particular on the directions of their spins and the
orientation of their shapes with respect to the directions of the filaments and
sheets. We find that both the spin and the major axes of filament-halos with
masses <= 10^{13} M_sun/h are preferentially aligned with the direction of the
filaments. The spins and major axes of halos in sheets tend to lie parallel to
the sheets. There is an opposite mass dependence of the alignment strengths for
the spin (negative) and major (positive) axes, i.e. with increasing halo mass
the major axis tends to be more strongly aligned with the direction of the
filament whereas the alignment between halo spin and filament becomes weaker
with increasing halo mass. The alignment strengths are stronger for halos in
the neighborhood of massive cluster halos. Overall, the two algorithms for
filament/sheet identification investigated here agree well with each other. The
method based on halos alone can be easily adapted for use with observational
data sets. | | Source: | arXiv, 0906.1654 | | Services: | Forum | Review | PDF | Favorites | |
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