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    Improving initial conditions for cosmological N -body simulations

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    MNRAS-2016-Garrison-4125-45.pdf
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    Final Published Version
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    Author
    Garrison, Lehman H.
    Eisenstein, Daniel J.
    Ferrer, Douglas
    Metchnik, Marc V.
    Pinto, Philip A.
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2016-10-01
    Keywords
    methods: numerical
    galaxies: haloes
    large-scale structure of Universe
    
    Metadata
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    Publisher
    OXFORD UNIV PRESS
    Citation
    Improving initial conditions for cosmological N -body simulations 2016, 461 (4):4125 Monthly Notices of the Royal Astronomical Society
    Journal
    Monthly Notices of the Royal Astronomical Society
    Rights
    © 2016 The Authors 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
    In cosmological N-body simulations, the representation of dark matter as discrete 'macroparticles' suppresses the growth of structure, such that simulations no longer reproduce linear theory on small scales near k(Nyquist). Marcos et al. demonstrate that this is due to sparse sampling of modes near k(Nyquist) and that the often-assumed continuum growing modes are not proper growing modes of the particle system. We develop initial conditions (ICs) that respect the particle linear theory growing modes and then rescale the mode amplitudes to account for growth suppression. These ICs also allow us to take advantage of our very accurate N-body code ABACUS to implement second-order Lagrangian perturbation theory (2LPT) in configuration space. The combination of 2LPT and rescaling improves the accuracy of the late-time power spectra, halo mass functions, and halo clustering. In particular, we achieve 1 per cent accuracy in the power spectrum down to k(Nyquist), versus k(Nyquist)/4 without rescaling or k(Nyquist)/13 without 2LPT, relative to an oversampled reference simulation. We anticipate that our 2LPT will be useful for large simulations where fast Fourier transforms are expensive and that rescaling will be useful for suites of medium-resolution simulations used in cosmic emulators and galaxy survey mock catalogues. Code to generate ICs is available at https://github.com/lgarrison/zeldovich-PLT.
    ISSN
    0035-8711
    1365-2966
    DOI
    10.1093/mnras/stw1594
    Version
    Final published version
    Sponsors
    National Science Foundation [AST-1313285, 1228509]; US Department of Energy [DE-SC0013718]; FAS Division of Science, Research Computing Group at Harvard University
    Additional Links
    http://mnras.oxfordjournals.org/lookup/doi/10.1093/mnras/stw1594
    ae974a485f413a2113503eed53cd6c53
    10.1093/mnras/stw1594
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