The evolution of large-scale structure in a universe dominated by cold dark matter

Davis, Marc; Efstathiou, G.; Frenk, Carlos S.; White, Simon D. M.

doi:10.1086/163168

Cited by 3,286 publications

(2,929 citation statements)

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“…Groups of particles are identified in our simulations by applying the Friends-of-Friends (FoF) algorithm with linking length 0.2 to the dark matter particles (Davis et al 1985). The mass M crit 200 and the radius r crit 200 of the groups are assigned using a spherical overdensity algorithm centred on the minimum of the gravitational potential, as implemented in SUBFIND (Springel et al 2001;Dolag et al 2009).…”

Section: Halo and Subhalo Definitionmentioning

confidence: 99%

The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations

Velliscig

Cacciato

Schaye

et al. 2015

Mon. Not. R. Astron. Soc.

142

170

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(2015) 'The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations.', Monthly notices of the Royal Astronomical Society., 453 (1). pp. 721-738. Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details.

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Section: Halo and Subhalo Definitionmentioning

confidence: 99%

The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations

Velliscig

Cacciato

Schaye

et al. 2015

Mon. Not. R. Astron. Soc.

142

170

View full text Add to dashboard Cite

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“…For each output snapshot, dark matter haloes are identified using a Friends-Of-Friends (FOF) algorithm (Davis et al 1985) with a linking length of b = 0.2 in units of the mean inter-particle separation. Then the SUB-FIND algorithm (Springel et al 2001) is applied to identify self-bound and locally over-dense substructures within each FOF halo.…”

Section: Simulationsmentioning

confidence: 99%

The galaxy population in cold and warm dark matter cosmologies

Wang

González-Pérez²,

Xie

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use a pair of high resolution N-body simulations implementing two dark matter models, namely the standard cold dark matter (CDM) cosmogony and a warm dark matter (WDM) alternative where the dark matter particle is a 1.5 keV thermal relic. We combine these simulations with the GALFORM semi-analytical galaxy formation model in order to explore differences between the resulting galaxy populations. We use GALFORM model variants for CDM and WDM that result in the same z = 0 galaxy stellar mass function by construction. We find that most of the studied galaxy properties have the same values in these two models, indicating that both dark matter scenarios match current observational data equally well. Even in under-dense regions, where discrepancies in structure formation between CDM and WDM are expected to be most pronounced, the galaxy properties are only slightly different. The only significant difference in the local universe we find is in the galaxy populations of "Local Volumes", regions of radius 1 to 8Mpc around simulated Milky Way analogues. In such regions our WDM model provides a better match to observed local galaxy number counts and is five times more likely than the CDM model to predict subregions within them that are as empty as the observed Local Void. Thus, a highly complete census of the Local Volume and future surveys of void regions could provide constraints on the nature of dark matter.

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“…The mass of a simulation particle is 5.67 × 10 5 h −1 M sun and the gravitational softening length is 1 h −1 kpc. We run a friends-of-friends (FoF) group finder (Davis et al 1985) to locate groups of galaxies. We also identify substructures (subhalos) in each FoF group using SUB-FIND algorithm developed by Springel et al (2001).…”

Section: Numerical Simulationsmentioning

confidence: 99%

Structure of dark matter halos in warm dark matter models and in models with long-lived charged massive particles

Kamada

Yoshida

Kohri

et al. 2013

J. Cosmol. Astropart. Phys.

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We study the formation of non-linear structures in Warm Dark Matter (WDM) models and in a Long-Lived Charged Massive Particle (CHAMP) model. CHAMPs with a decay lifetime of about 1 yr induce characteristic suppression in the matter power spectrum at subgalactic scales through acoustic oscillations in the thermal background. We explore structure formation in such a model. We also study three WDM models, where the dark matter particles are produced through the following mechanisms: i) WDM particles are produced in the thermal background and then kinematically decoupled; ii) WDM particles are fermions produced by the decay of thermal heavy bosons; and iii) WDM particles are produced by the decay of non-relativistic heavy particles. We show that the linear matter power spectra for the three models are all characterised by the comoving Jeans scale at the matter-radiation equality. Furthermore, we can also describe the linear matter power spectrum for the Long-Lived CHAMP model in terms of a suitably defined characteristic cut-off scale k Ch , similarly to the WDM models. We perform large cosmological N -body simulations to study the non-linear growth of structures in these four models. We compare the halo mass functions, the subhalo mass functions, and the radial distributions of subhalos in simulated Milky Way-size halos. For the characteristic cut-off scale k cut = 51 h Mpc −1 , the subhalo abundance -2 -(∼ 10 9 M sun ) is suppressed by a factor of ∼ 10 compared with the standard ΛCDM model. We then study the models with k cut ≃ 51, 410, 820 h Mpc −1 , and confirm that the halo and the subhalo abundances and the radial distributions of subhalos are indeed similar between the different WDM models and the Long-Lived CHAMP model. The result suggests that the cut-off scale k cut not only characterises the linear power spectra but also can be used to predict the non-linear clustering properties. The radial distribution of subhalos in Milky Way-size halos is consistent with the observed distribution for k cut ∼ 50 − 800 h Mpc −1 ; such models resolve the so-called "missing satellite problem".

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The evolution of large-scale structure in a universe dominated by cold dark matter

Cited by 3,286 publications

References 0 publications

The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations

The alignment and shape of dark matter, stellar, and hot gas distributions in the EAGLE and cosmo-OWLS simulations

The galaxy population in cold and warm dark matter cosmologies

Structure of dark matter halos in warm dark matter models and in models with long-lived charged massive particles

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