The mass–concentration–redshift relation of cold and warm dark matter haloes

Ludlow, Aaron D.; Bose, Sownak; Angulo, Raúl E.; Wang, Lan; Hellwing, Wojciech A.; Navarro, Julio F.; Cole, Shaun; Frenk, Carlos S.

doi:10.1093/mnras/stw1046

Cited by 335 publications

(514 citation statements)

References 79 publications

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“…We estimate the scatter that would be induced by using a different concentration-mass relation, comparing the models of Duffy et al (2008), Meneghetti et al (2014) and Zhao et al (2009). time t 0.04 at which the main halo progenitor assembled 4 per cent of its mass needed by the Zhang et al (2009) concentration-mass model. The WDM trend is opposite to the CDM one, because in WDM models the concentration peaks at intermediate masses and decreases both at the high and low mass end, behaving similarly to the WDM power-spectrum (Ludlow et al 2016). The contours show the effect of choosing a concentration 1 or 2σ away from the average concentration.…”

Section: Discussionmentioning

confidence: 90%

Modelling the line-of-sight contribution in substructure lensing

Despali

Vegetti

White

et al. 2018

Monthly Notices of the Royal Astronomical Society

120

165

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We investigate how Einstein rings and magnified arcs are affected by small-mass dark-matter haloes placed along the line-of-sight to gravitational lens systems. By comparing the gravitational signature of line-of-sight haloes with that of substructures within the lensing galaxy, we derive a mass-redshift relation that allows us to rescale the detection threshold (i.e. lowest detectable mass) for substructures to a detection threshold for line-of-sight haloes at any redshift. We then quantify the line-of-sight contribution to the total number density of low-mass objects that can be detected through strong gravitational lensing. Finally, we assess the degeneracy between substructures and line-of-sight haloes of different mass and redshift to provide a statistical interpretation of current and future detections, with the aim of distinguishing between CDM and WDM. We find that line-of-sight haloes statistically dominate with respect to substructures, by an amount that strongly depends on the source and lens redshifts, and on the chosen dark matter model. Substructures represent about 30 percent of the total number of perturbers for low lens and source redshifts (as for the SLACS lenses), but less than 10 per cent for high redshift systems. We also find that for data with high enough signal-to-noise ratio and angular resolution, the non-linear effects arising from a double-lens-plane configuration are such that one is able to observationally recover the line-of-sight halo redshift with an absolute error precision of 0.15 at the 68 per cent confidence level.

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Section: Discussionmentioning

confidence: 90%

Modelling the line-of-sight contribution in substructure lensing

Despali

Vegetti

White

et al. 2018

Monthly Notices of the Royal Astronomical Society

120

165

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“…The measured concentration, c200 = 6.3 ± 1.2, as estimated in the reference regression, is slightly higher than but still consistent with predictions. Recent theoretical estimates based on N -body simulations of dark matter halos (Bhattacharya et al 2013;Dutton & Macciò 2014;Ludlow et al 2016) graze the 68.3 per cent confidence region, see Fig. 11.…”

Section: Mass and Concentrationmentioning

confidence: 92%

CLUMP-3D: three-dimensional lensing and multi-probe analysis of MACS J1206.2−0847, a remarkably regular cluster

Sereno

Ettori

Meneghetti

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Multi-wavelength techniques can probe the distribution and the physical properties of baryons and dark matter in galaxy clusters from the inner regions out to the peripheries. We present a full three-dimensional analysis combining strong and weak lensing, X-ray surface brightness and temperature, and the Sunyaev-Zel'dovich effect. The method is applied to MACS J1206.2-0847, a remarkably regular, face-on, massive, M 200 = (1.1 ± 0.2) × 10 15 M /h, cluster at z = 0.44. The measured concentration, c 200 = 6.3 ± 1.2, and the triaxial shape are common to halos formed in a ΛCDM scenario. The gas has settled in and follows the shape of the gravitational potential, which is evidence of pressure equilibrium via the shape theorem. There is no evidence for significant non-thermal pressure and the equilibrium is hydrostatic.

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“…Though halo concentration correlates with halo mass, there is significant scatter (∼ 0.1 dex) about the median at fixed Mvir (Jing 2000;Bullock et al 2001). Some fraction of this scatter is driven by the variation in halo mass accretion history (Wechsler et al 2002;Ludlow et al 2016), with early-forming halos having higher concentrations at fixed final virial mass. The dependence of halo profile on a mass-dependent concentration parameter and the correlation between formation time and concentration at fixed virial mass are caused by the hierarchical build-up of halos in ΛCDM: low-mass halos assemble earlier, when the mean density of the Universe is higher, and therefore have higher concentrations than high-mass halos (e.g., Navarro, Frenk & White 1997;Wechsler et al 2002).…”

Section: Substructure Is Abundant and Almost Self-similar [Figure 5]mentioning

confidence: 98%

Small-Scale Challenges to the ΛCDM Paradigm

Bullock

Boylan-Kolchin

2017

Annu. Rev. Astron. Astrophys.

1,318

1,017

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The dark energy plus cold dark matter (ΛCDM) cosmological model has been a demonstrably successful framework for predicting and explaining the large-scale structure of Universe and its evolution with time. Yet on length scales smaller than ∼ 1 Mpc and mass scales smaller than ∼ 10 11 M , the theory faces a number of challenges. For example, the observed cores of many dark-matter dominated galaxies are both less dense and less cuspy than naively predicted in ΛCDM. The number of small galaxies and dwarf satellites in the Local Group is also far below the predicted count of low-mass dark matter halos and subhalos within similar volumes. These issues underlie the most well-documented problems with ΛCDM: Cusp/Core, Missing Satellites, and Too-Big-to-Fail. The key question is whether a better understanding of baryon physics, dark matter physics, or both will be required to meet these challenges. Other anomalies, including the observed planar and orbital configurations of Local Group satellites and the tight baryonic/dark matter scaling relations obeyed by the galaxy population, have been less thoroughly explored in the context of ΛCDM theory. Future surveys to discover faint, distant dwarf galaxies and to precisely measure their masses and density structure hold promising avenues for testing possible solutions to the small-scale challenges going forward. Observational programs to constrain or discover and characterize the number of truly dark low-mass halos are among the most important, and achievable, goals in this field over then next decade. These efforts will either further verify the ΛCDM paradigm or demand a substantial revision in our understanding of the nature of dark matter.

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The mass–concentration–redshift relation of cold and warm dark matter haloes

Cited by 335 publications

References 79 publications

Modelling the line-of-sight contribution in substructure lensing

Modelling the line-of-sight contribution in substructure lensing

CLUMP-3D: three-dimensional lensing and multi-probe analysis of MACS J1206.2−0847, a remarkably regular cluster

Small-Scale Challenges to the ΛCDM Paradigm

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