NOVel Adaptive softening for collisionless N-body simulations : Eliminating spurious haloes
(2016) In Monthly Notices of the Royal Astronomical Society 458(1). p.468-479- Abstract
We describe a NOVel form of Adaptive softening (NOVA) for collisionless N-body simulations, implemented in the RAMSES adaptive mesh refinement code. In RAMSES - that we refer to as a 'standard N-body method' - cells are only split if they containmore than eight particles (amass refinement criterion). Here, we introduce an additional criterion that the particle distribution within each cell be sufficiently isotropic, as measured by the ratio of the maximum to minimum eigenvalues of its moment of inertia tensor: n = λmax/λmin. In this way, collapse is only refined if it occurs along all three axes, ensuring that the softening ε is always of order twice the largest interparticle spacing in a cell. This more... (More)
We describe a NOVel form of Adaptive softening (NOVA) for collisionless N-body simulations, implemented in the RAMSES adaptive mesh refinement code. In RAMSES - that we refer to as a 'standard N-body method' - cells are only split if they containmore than eight particles (amass refinement criterion). Here, we introduce an additional criterion that the particle distribution within each cell be sufficiently isotropic, as measured by the ratio of the maximum to minimum eigenvalues of its moment of inertia tensor: n = λmax/λmin. In this way, collapse is only refined if it occurs along all three axes, ensuring that the softening ε is always of order twice the largest interparticle spacing in a cell. This more conservative force softening criterion is designed to minimize spurious two-body effects, while maintaining high force resolution in collapsed regions of the flow. We test NOVA using an antisymmetric perturbed plane wave collapse ('Valinia' test) before applying it to warm dark matter (WDM) simulations. For the Valinia test, we show that - unlike the standard N-body method - NOVA produces no numerical fragmentation while still being able to correctly capture fine caustics and shells around the collapsing regions. For theWDM simulations, we find that NOVA converges significantly more rapidly than standard N-body, producing little or no spurious haloes on small scales. We will use NOVA in forthcoming papers to study the issue of halo formation below the free-streaming mass Mfs; filament stability; and to obtain new constraints on the temperature of dark matter.
(Less)
- author
- Hobbs, Alexander ; Read, Justin I. ; Agertz, Oscar LU ; Iannuzzi, Francesca and Power, Chris
- publishing date
- 2016-02-22
- type
- Contribution to journal
- publication status
- published
- keywords
- Dark matter, Large-scale structure of universe, Methods: numerical
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 458
- issue
- 1
- pages
- 12 pages
- publisher
- Oxford University Press
- external identifiers
-
- scopus:84963758890
- ISSN
- 0035-8711
- DOI
- 10.1093/mnras/stw251
- language
- English
- LU publication?
- no
- id
- 24583f16-8194-4131-b8fb-4d9caadfa428
- date added to LUP
- 2019-02-07 11:15:33
- date last changed
- 2022-03-02 19:50:22
@article{24583f16-8194-4131-b8fb-4d9caadfa428,
abstract = {{<p>We describe a NOVel form of Adaptive softening (NOVA) for collisionless N-body simulations, implemented in the RAMSES adaptive mesh refinement code. In RAMSES - that we refer to as a 'standard N-body method' - cells are only split if they containmore than eight particles (amass refinement criterion). Here, we introduce an additional criterion that the particle distribution within each cell be sufficiently isotropic, as measured by the ratio of the maximum to minimum eigenvalues of its moment of inertia tensor: n = λ<sub>max</sub>/λ<sub>min</sub>. In this way, collapse is only refined if it occurs along all three axes, ensuring that the softening ε is always of order twice the largest interparticle spacing in a cell. This more conservative force softening criterion is designed to minimize spurious two-body effects, while maintaining high force resolution in collapsed regions of the flow. We test NOVA using an antisymmetric perturbed plane wave collapse ('Valinia' test) before applying it to warm dark matter (WDM) simulations. For the Valinia test, we show that - unlike the standard N-body method - NOVA produces no numerical fragmentation while still being able to correctly capture fine caustics and shells around the collapsing regions. For theWDM simulations, we find that NOVA converges significantly more rapidly than standard N-body, producing little or no spurious haloes on small scales. We will use NOVA in forthcoming papers to study the issue of halo formation below the free-streaming mass Mfs; filament stability; and to obtain new constraints on the temperature of dark matter.</p>}},
author = {{Hobbs, Alexander and Read, Justin I. and Agertz, Oscar and Iannuzzi, Francesca and Power, Chris}},
issn = {{0035-8711}},
keywords = {{Dark matter; Large-scale structure of universe; Methods: numerical}},
language = {{eng}},
month = {{02}},
number = {{1}},
pages = {{468--479}},
publisher = {{Oxford University Press}},
series = {{Monthly Notices of the Royal Astronomical Society}},
title = {{NOVel Adaptive softening for collisionless N-body simulations : Eliminating spurious haloes}},
url = {{http://dx.doi.org/10.1093/mnras/stw251}},
doi = {{10.1093/mnras/stw251}},
volume = {{458}},
year = {{2016}},
}