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

By A. Schneider, Rowan J. Smith, A. Macciò, B. Moore. 2011

220 citations recorded by the source corpus.

The dark energy dominated warm dark matter (WDM) model is a promising alternative cosmological scenario. We explore large-scale structure formation in this paradigm. We do this in two different ways: with the halo model approach and with the help of an ensemble of high-resolution N-body simulations. Combining these quasi-independent approaches leads to a physical understanding of the important processes which shape the formation of structures. We take a detailed look at the halo mass function, the concentrations and the linear halo bias of WDM. In all cases we find interesting deviations with respect to cold dark matter (CDM). In particular, the concentration-mass relation displays a turnover for group scale dark matter haloes, for the case of WDM particles with masses of the order of mWDM˜ 0.25 keV. This may be interpreted as a hint for top-down structure formation on small scales. We implement our results into the halo model and find much better agreement with simulations. On small scales, the WDM halo model now performs as well as its CDM counterpart.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6cbc7e57aa2438310b514749208e2337f771abb0

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Citations in the corpus

The properties of warm dark matter haloes (2013, background): “3 case can be fit with the functional form given by Schneider et al. (2012): nWDM/nCDM = (1 +MhmM −1)β, (7) where Mhm is the mass associated with the scale at which the WDM matter power spectrum is suppressed by 50 percent relative to the CDM power spectrum, M is subhalo mass and β is a free…”
Matter power spectrum and the challenge of percent accuracy (2015, background): “3, can be explained in terms of analytical considerations: experiments with the halo model show that clusters significantly contribute to the power spectrum, while the presence of small haloes below 1011 h−1M have a negligible effect (Schneider et al. 2012; van Daalen & Schaye 2015).”
Is there a "too big to fail" problem in the field? (2014, methodology): “5 using each time the appropriate medianc-Mvir relation (Schneider et al. 2012, Eqn.”
The stellar mass-halo mass relation of isolated field dwarfs : a critical test of ΛCDM at the edge of galaxy formation (2016, unknown): “We use the formulae in Schneider et al. (2012) to transform MNRAS 000, 000–000 (0000) the Bolshoi halo mass function, derived for ΛCDM, to one in ΛWDM5: dN dM ∣∣∣∣ WDM = dN dM ∣∣∣∣ CDM ( 1 + Mhm M )−β (14) where Mhm = 4/3πρcrit(λhm/2) 3 is the ‘half mode mass’; β = 1.16; λhm is the ‘half mode’…”
Gravitational probes of dark matter physics (2017, background): “For the most frequently encountered (thermal relic warm dark matter) transfer functions, kcut ∼ 10 khm, or Mhm ∼ (a few) × 10(3)Mcut, where Mcut is the halo mass corresponding to kcut [170].”
CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847 (2013, background): “For example, it has been found that thecMr has opposite slopes in Cold and Hot DM cosmologies (Wang & White 2009), while in dark-energydominated Warm DM models thecMr is not monotonous but characterized by a turnover point at group mass scales (Schneider et al. 2012).”
Quantifying baryon effects on the matter power spectrum and the weak lensing shear correlation (2018, background): “At redshift zero the power spectrum is strongly influenced by haloes hosting galaxy groups and small clusters, while Milky-Way sized haloes do not affect the signal below k ∼ 10 h/Mpc [61, 62].”
Constraints on Dark Matter Microphysics from the Milky Way Satellite Population (2019, methodology): “We generate linear matter power spectra as a function of σ0 and mχ, and we compare these to WDM power spectra using the transfer function in Schneider et al. (2012) by matching the half-mode scale khm, i.e., the wavenumber at which the transfer function T (k) = (Pcollisional(k)/PCDM(k))1/2 is equal…”
Halo mass function and the free streaming scale (2013, methodology): “In the simulation outputs these artefacts are most visible in cosmic filaments, where they form equally spaced clumps that are strongly resolution dependent (Wang & White 2007; Schneider et al. 2012).”
Cores in warm dark matter haloes: a Catch 22 problem (2012, methodology): “Numerical N-body simulations have been used to better understand the properties of virialized objects in the Warm Dark Matter scenarios (e.g. Bode et al. 2001; Knebe et al. 2003; Wang & White 2007; Zavala et al. 2009; Tikhonov et al. 2009; Schneider et al. 2011).”
Small-Scale Challenges to the ΛCDM Paradigm (2017, background): “The half-mode wavelength λhm is approximately fourteen times larger than the free-streaming length (Schneider et al. 2012), meaning that structure below ∼ 5× 1010 M is significantly different from CDM in a 1 keV thermal dark matter model: Mhm = 5.5× 1010 (mWDM 1 keV )−3.33 M .”
The mass–concentration–redshift relation of cold and warm dark matter haloes (2016, background): “The resulting c(M) relation, however, is non-monotonic: concentrations reach a maximum at a halo mass about two decades above the truncation scale but decline gradually towards larger and smaller masses (see also e.g. Schneider et al. 2012; Macciò et al. 2013).”
The warm dark matter halo mass function below the cut-off scale (2013, methodology): “For our choice of cosmological parameters and WDM particle mass: α = 0.26 h−1Mpc, which translates into a freestreaming mass-scale Mfs = 4π 3 ρ̄ (α/2)3 ≃ 7× 108 h−1M⊙ (3) and a half-mode mass-scale (cf. Coĺın et al. 2008; Schneider et al. 2012) Mhm ≃ 4.3× 10 3 Mfs ≃ 3.0× 10 12 h−1M⊙.”