The properties of warm dark matter haloes

Lovell, Mark R.; Frenk, Carlos S.; Eke, V. R.; Jenkins, Adrian; Gao, Liang; Theuns, Tom

doi:10.1093/mnras/stt2431

Cited by 466 publications

(661 citation statements)

References 68 publications

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“…• We present a method to estimate the number of substructures in a host halo, and show that it agrees very well with warm DM simulations from Lovell et al (2014). Based on this, we provide approximative constraints on mixed DM models by comparing the expected number of substructures to the observed number of Milky-Way satellites.…”

Section: Discussionmentioning

confidence: 59%

“…Number of predicted Milky-Way satellites with mass above 10 8 h −1 M from the model (Eq. 17) and from simulations by Lovell et al (2014). For the case of CDM the perfect agreement is by construction, since the model is calibrated to this number.…”

Section: Estimating the Number Of Dwarf Satellitesmentioning

confidence: 87%

“…We therefore apply a postprocessing scheme similar to the one presented by Lovell et al (2014), which filters out artefacts based on both protohalo sphericity and overlap between two simulations with the same density field but different resolution.…”

Section: Discussionmentioning

confidence: 99%

“…the volume spanned by all particles ending up in a halo) as well as their overlap between realisations with different resolution. In a first step, Lovell et al (2014) measured the sphericity of proto-haloes, removing all objects that are unusually elongated. This selection criterion is based on the observation that artefacts originate from the collapse of larger modes to walls and filaments, pushing already aligned particles together until they cluster into non-physical clumps.…”

Section: Removing Artefactsmentioning

confidence: 99%

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Structure formation with suppressed small-scale perturbations

Schneider

2015

Monthly Notices of the Royal Astronomical Society

140

215

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All commonly considered dark matter scenarios are based on hypothetical particles with small but non-zero thermal velocities and tiny interaction cross-sections. A generic consequence of these attributes is the suppression of small-scale matter perturbations either due to free-streaming or due to interactions with the primordial plasma. The suppression scale can vary over many orders of magnitude depending on particle candidate and production mechanism in the early Universe.While nonlinear structure formation has been explored in great detail well above the suppression scale, the range around suppressed perturbations is still poorly understood. In this paper we study structure formation in the regime of suppressed perturbations using both analytical techniques and numerical simulations. We develop simple and theoretically motivated recipes for the halo mass function, the expected number of satellites, and the halo concentrations, which are designed to work for power spectra with suppression at arbitrary scale and of arbitrary shape. As case studies, we explore warm and mixed dark matter scenarios where effects are most distinctive. Additionally, we examine the standard dark matter scenario based on weakly interacting massive particles (WIMP) and compare it to pure cold dark matter with zero primordial temperature. We find that our analytically motivated recipes are in good agreement with simulations for all investigated dark matter scenarios, and we therefore conclude that they can be used for generic cases with arbitrarily suppressed small-scale perturbations.

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Section: Discussionmentioning

confidence: 59%

Section: Estimating the Number Of Dwarf Satellitesmentioning

confidence: 87%

Section: Discussionmentioning

confidence: 99%

Section: Removing Artefactsmentioning

confidence: 99%

See 2 more Smart Citations

Structure formation with suppressed small-scale perturbations

Schneider

2015

Monthly Notices of the Royal Astronomical Society

140

215

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“…Historically, cosmological WDM simulations, and hence semi-analytic galaxy formation models built on them, have suffered from uncertainties introduced by spurious selfbound DM clumps arising from numerical discreetness effects (Wang & White 2007). These spurious haloes have been carefully removed from the halo catalogue on which our GALFORM model is based by applying the procedure of Lovell et al (2014), which improves the reliability of comparisons between our results and observations. We note that hydrodynamical simulations by Gao & Theuns (2007) and Gao et al (2015) have demonstrated a novel star formation mechanism in WDM, which occurs in filaments rather than in collapsed dark matter haloes.…”

Section: Introductionmentioning

confidence: 98%

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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2023

Collective Phenomena in Plasmas and Elsewhere

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The properties of warm dark matter haloes

Cited by 466 publications

References 68 publications

Structure formation with suppressed small-scale perturbations

Structure formation with suppressed small-scale perturbations

The galaxy population in cold and warm dark matter cosmologies

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