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Dynamics of pairwise motions in the Cosmic Web

Published online by Cambridge University Press:  12 October 2016

Wojciech A. Hellwing
Wojciech A. Hellwing*
Affiliation:
Interdisciplinary Center for Mathematical and computational modelling (ICM), University of Warsaw, ul. Pawińskiego 2a, 02-186 Warsaw, Poland email: [email protected] Institute for Computational Cosmology, University of Durham, Science Site, South Road, DH1-3LE Durham, UK
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Abstract

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We present results of analysis of the dark matter (DM) pairwise velocity statistics in different Cosmic Web environments. We use the DM velocity and density field from the Millennium 2 simulation together with the NEXUS+ algorithm to segment the simulation volume into voxels uniquely identifying one of the four possible environments: nodes, filaments, walls or cosmic voids. We show that the PDFs of the mean infall velocities v12 as well as its spatial dependence together with the perpendicular and parallel velocity dispersions bear a significant signal of the large-scale structure environment in which DM particle pairs are embedded. The pairwise flows are notably colder and have smaller mean magnitude in wall and voids, when compared to much denser environments of filaments and nodes. We discuss on our results, indicating that they are consistent with a simple theoretical predictions for pairwise motions as induced by gravitational instability mechanism. Our results indicate that the Cosmic Web elements are coherent dynamical entities rather than just temporal geometrical associations. In addition it should be possible to observationally test various Cosmic Web finding algorithms by segmenting available peculiar velocity data and studying resulting pairwise velocity statistics.

Keywords

cosmic webpairwise velocitylarge-scale structuredark matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 322 - 327
Copyright
Copyright © International Astronomical Union 2016 

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