Non-linear evolution of cosmological structures in warm dark matter models

Schneider, Aurel; Smith, R. E.; Macciò, Andrea V.; Moore, Ben

doi:10.1111/j.1365-2966.2012.21252.x

Cited by 303 publications

(453 citation statements)

References 82 publications

(156 reference statements)

Supporting

Mentioning

430

Contrasting

Order By: Relevance

“…The Bullock-model approximately works for pure CDM, but it breaks down for the case of WDM where it predicts the concentration-mass relation to become constant instead of the observed downturn towards small masses (Eke et al 2001;Schneider et al 2012). The reason for this failure comes from an inaccuracy in the estimation of the redshift of collapse.…”

Section: Concentration-mass Relationmentioning

confidence: 99%

“…In a pure CDM scenario, halo concentrations are slightly mass dependent, decreasing on average towards larger halo masses with an important scatter between individual haloes. In WDM scenarios, halo concentrations have been reported to increase, turn over, and decrease on average towards large masses (Bode et al 2001;Avila-Reese et al 2001;Schneider et al 2012).…”

Section: Concentration-mass Relationmentioning

confidence: 99%

See 1 more Smart Citation

Structure formation with suppressed small-scale perturbations

Schneider

2015

Monthly Notices of the Royal Astronomical Society

Self Cite

143

215

View full text Add to dashboard Cite

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.

show abstract

Section: Concentration-mass Relationmentioning

confidence: 99%

Section: Concentration-mass Relationmentioning

confidence: 99%

Structure formation with suppressed small-scale perturbations

Schneider

2015

Monthly Notices of the Royal Astronomical Society

Self Cite

143

215

View full text Add to dashboard Cite

show abstract

“…On large scales unaffected by the free streaming cut-off, structure formation is very similar in CDM and sterile neutrino cosmologies (and in WDM in general), but on scales comparable to or smaller than the cut-off, structure formation proceeds in a fundamentally different way in the two cases. No haloes form below a certain mass scale determined by the cut-off and the formation of small haloes above the cut-off is delayed (see Colín et al 2000;Bode et al 2001;Avila-Reese et al 2001;Viel et al 2005;Lovell et al 2012;Schneider et al 2012;Bose et al 2016b,a) For a 7 keV sterile neutrino, the cut-off mass is ∼ 10 9 M . Thus, potentially observable differences from CDM would emerge on subgalactic scales and at high redshifts when the delayed onset of structure formation might become apparent.…”

Section: Introductionmentioning

confidence: 99%

Reionization in sterile neutrino cosmologies

Bose¹,

Frenk²,

Hou³

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The 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. ABSTRACTWe investigate the process of reionisation in a model in which the dark matter is a warm elementary particle such as a sterile neutrino. We focus on models that are consistent with the dark matter decay interpretation of the recently detected line at 3.5 keV in the X-ray spectra of galaxies and clusters. In warm dark matter models the primordial spectrum of density perturbations has a cut-off on the scale of dwarf galaxies. Structure formation therefore begins later than in the standard cold dark matter (CDM) model and very few objects form below the cut-off mass scale. To calculate the number of ionising photons, we use the Durham semianalytic model of galaxy formation, GALFORM. We find that even the most extreme 7 keV sterile neutrino we consider is able to reionise the Universe early enough to be compatible with the bounds on the epoch of reionisation from Planck. This, perhaps surprising, result arises from the rapid build-up of high redshift galaxies in the sterile neutrino models which is also reflected in a faster evolution of their far-UV luminosity function between 10 > z > 7 than in CDM. The dominant sources of ionising photons are systematically more massive in the sterile neutrino models than in CDM. As a consistency check on the models, we calculate the present-day luminosity function of satellites of Milky Way-like galaxies. When the satellites recently discovered in the DES survey are taken into account, strong constraints are placed on viable sterile neutrino models.

show abstract

“…In the past decade, many papers have modelled WDM structure formation (e.g Bode et al 2001;Knebe et al 2002Knebe et al , 2003Busha et al 2007;Colín et al 2008;Zavala et al 2009;Smith & Markovic 2011;Schneider et al 2012;Lovell et al 2012;Destri et al 2013;Angulo et al 2013;Benson et al 2013;Kamada et al 2013;Lovell et al 2014;Bose et al 2016;Ludlow et al 2016;Li et al 2016a,b). In the WDM model, the dark matter particles have intrinsic thermal velocities, and these velocities influence the small scale structure formation of the Universe mainly in two different ways.…”

Section: Introductionmentioning

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

View full text Add to dashboard Cite

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.

show abstract

Non-linear evolution of cosmological structures in warm dark matter models

Cited by 303 publications

References 82 publications

Structure formation with suppressed small-scale perturbations

Structure formation with suppressed small-scale perturbations

Reionization in sterile neutrino cosmologies

The galaxy population in cold and warm dark matter cosmologies

Contact Info

Product

Resources

About