Spatial clustering of dark matter haloes: secondary bias, neighbour bias, and the influence of massive neighbours on halo properties
Author
Salcedo, Andrés NMaller, Ariyeh H
Berlind, Andreas A
Sinha, Manodeep
McBride, Cameron K
Behroozi, Peter S
Wechsler, Risa H
Weinberg, David H
Affiliation
Univ Arizona, Steward ObservIssue Date
2018-04-21Keywords
methods: numericalgalaxies: formation
galaxies: haloes
dark matter
large-scale structure of Universe
cosmology: theory
Metadata
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OXFORD UNIV PRESSCitation
Andrés N Salcedo, Ariyeh H Maller, Andreas A Berlind, Manodeep Sinha, Cameron K McBride, Peter S Behroozi, Risa H Wechsler, David H Weinberg; Spatial clustering of dark matter haloes: secondary bias, neighbour bias, and the influence of massive neighbours on halo properties, Monthly Notices of the Royal Astronomical Society, Volume 475, Issue 4, 21 April 2018, Pages 4411–4423, https://doi.org/10.1093/mnras/sty109Rights
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We explore the phenomenon commonly known as halo assembly bias, whereby dark matter haloes of the same mass are found to be more or less clustered when a second halo property is considered, for haloes in the mass range 3.7 x 10(11)-5.0 x 10(13) h(-1)M(circle dot). Using the Large Suite of Dark Matter Simulations (LasDamas) we consider nine commonly used halo properties and find that a clustering bias exists if haloes are binned by mass or by any other halo property. This secondary bias implies that no single halo property encompasses all the spatial clustering information of the halo population. The mean values of some halo properties depend on their halo's distance to a more massive neighbour. Halo samples selected by having high values of one of these properties therefore inherit a neighbour bias such that they are much more likely to be close to a much more massive neighbour. This neighbour bias largely accounts for the secondary bias seen in haloes binned by mass and split by concentration or age. However, haloes binned by other mass-like properties still show a secondary bias even when the neighbour bias is removed. The secondary bias of haloes selected by their spin behaves differently than that for other halo properties, suggesting that the origin of the spin bias is different than of other secondary biases.ISSN
0035-87111365-2966
Version
Final published versionSponsors
Department of Energy Computational Science Graduate Fellowship Program of the Office of Science; National Nuclear Security Administration in the Department of Energy [DE-FG02-97ER25308]; NSF Career Award [AST-1151650]; Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) [CE170100013]; NSF [AST-1516997]; [NSF-REU 1263045]Additional Links
https://academic.oup.com/mnras/article/475/4/4411/4810556ae974a485f413a2113503eed53cd6c53
10.1093/mnras/sty109