The lensing properties of subhaloes in massive elliptical galaxies in sterile neutrino cosmologies

Despali, Giulia; Lovell, Mark R.; Vegetti, Simona; Crain, Robert A.; Oppenheimer, Benjamin D.

doi:10.1093/mnras/stz3068

Cited by 29 publications

(33 citation statements)

References 99 publications

(192 reference statements)

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“…For example, the normalized radial density of M 0 = [10 7.5 , 10 8.0 ] M WDM subhaloes at 30 kpc is twice that in CDM at radii <70 kpc, and in the [10 7.0 , 10 7.5 ] bin the normalized abundance is a factor of five times the CDM equivalent. 1 We thus recover the intriguing results found in Bose et al (2017) and Despali et al (2020).…”

Section: Radial Distributionssupporting

confidence: 77%

“…Initial published constraints using stream gaps have made the assumption that the spatial distribution of subhaloes is the same in WDM as in CDM. While this assumption appears to work well for massive, luminous satellites (Newton et al 2020), it breaks down for dark, lower mass haloes as shown above and in Despali et al (2020). We investigate the implications of this result by comparing the CDM and WDM subhalo populations in the halo region where stellar stream gaps are analysed versus the population of all subhaloes out to 300 kpc.…”

Section: Radial Distribution: Implications For the Number Of Stream Perturbersmentioning

confidence: 87%

“…A second effect is the change in the internal properties of WDM haloes close to the mass cut-off scale, which are characterized by lower densities (Colín, Avila-Reese & Valenzuela 2000;Lovell et al 2012) and thus can potentially experience faster mass loss and disruption when orbiting around a more massive host such as the MW. However, it has been shown that the switch from one model to the other also affects the radial distribution of low mass subhaloes, both in MW-analogue haloes (Lovell et al 2014;Bose et al 2017) and in ∼10 13 M haloes that are used for lensing constraints (Despali et al 2020). In both cases, the radial distribution of subhaloes with masses below the WDM characteristic half-mode mass, M hm , is steeper in WDM than in CDM, which can be seen as a change in the radial distribution of satellite galaxies if the halfmode mass is high enough.…”

mentioning

confidence: 99%

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The spatial distribution of Milky Way satellites, gaps in streams, and the nature of dark matter

Lovell

Cautun

Frenk

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The spatial distribution of Milky Way (MW) subhaloes provides an important set of observables for testing cosmological models. These include the radial distribution of luminous satellites, planar configurations, and the abundance of dark subhaloes whose existence or absence is key to distinguishing amongst dark matter models. We use the coco N-body simulations of cold dark matter (CDM) and 3.3 keV thermal relic warm dark matter (WDM) to predict the satellite spatial distribution in the limit that the impact of baryonic physics is minimal. We demonstrate that the radial distributions of CDM and 3.3 keV-WDM luminous satellites are identical if the minimum pre-infall halo mass to form a galaxy is >108.5 ${\, \rm M_\odot }$. The distribution of dark subhaloes is significantly more concentrated in WDM due to the absence of low mass, recently accreted substructures that typically inhabit the outer parts of a MW halo in CDM. We show that subhaloes of mass [107, 108] ${\, \rm M_\odot }$ and within 30 kpc of the centre are the stripped remnants of larger haloes in both models. Therefore their abundance in WDM is 3 × higher than one would anticipate from the overall WDM subhalo population. We estimate that differences between CDM and WDM concentration–mass relations can be probed for subhalo–stream impact parameters <2 kpc. Finally, we find that the impact of WDM on planes of satellites is likely negligible. Comprehensive comparisons with observations will require further work with high resolution, self-consistent hydrodynamical simulations.

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Section: Radial Distributionssupporting

confidence: 77%

Section: Radial Distribution: Implications For the Number Of Stream Perturbersmentioning

confidence: 87%

mentioning

confidence: 99%

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The spatial distribution of Milky Way satellites, gaps in streams, and the nature of dark matter

Lovell

Cautun

Frenk

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Our four Ns Boltzmann-derived power spectra have shallower 1 An alternative, public algorithm for calculating these momentum distributions was presented by Venumadhav et al (2016). It was shown briefly in Despali et al (2019) slopes than their V05 counterparts, and this difference correlates with L6. The V05 fit overestimates the power of the LA12 model for k < k hm by up to 10 per cent and the LA8 model by 20 per cent.…”

Section: Methods and Resultsmentioning

confidence: 90%

“…originally with β = −1.3 and γ = 2.7. Despali et al (2019) refit γ = 0.35 for LA8; this model has M hm = 1.28 × 10 8 M⊙. We compute our results for the top-hat measure of halo mass, MTH, as this is the measure computed by EPS.…”

Section: Methods and Resultsmentioning

confidence: 99%

The halo mass function in alternative dark matter models

Lovell

2020

Monthly Notices of the Royal Astronomical Society: Letters

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The claimed detection of large amounts of substructure in lensing flux anomalies, and in Milky Way stellar stream gaps statistics, has lead to a step change in constraints on simple warm dark matter models. In this study we compute predictions for the halo mass function both for these simple models and also for comprehensive particle physics models of sterile neutrinos and dark acoustic oscillations. We show that the mass function fit of Lovell et al. underestimates the number of haloes less massive than the half-mode mass, M hm by a factor of 2, relative to the extended Press-Schechter (EPS) method. The alternative approach of applying EPS to the Viel et al. matter power spectrum fit instead suggests good agreement at M hm relative to the comprehensive model matter power spectra results, although the number of haloes with mass < M hm is still suppressed due to the absence of small scale power in the fitting function. Overall, we find that the number of dark matter haloes with masses < 10 8 M ⊙ predicted by competitive particle physics models is underestimated by a factor of ∼ 2 when applying popular fitting functions, although careful studies that follow the stripping and destruction of subhaloes will be required in order to draw robust conclusions.

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Strong Gravitational Lensing as a Probe of Dark Matter

Vegetti,

Birrer,

Despali

et al. 2024

Space Sci Rev

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Dark matter structures within strong gravitational lens galaxies and along their lines of sight leave a gravitational imprint on the multiple images of lensed sources. Strong gravitational lensing provides, therefore, a key test of different dark matter models. In this article, we describe how galaxy-scale strong gravitational lensing observations are sensitive to the physical nature of dark matter. We provide an historical perspective of the field, and review its current status. We discuss the challenges and advances in terms of data, treatment of systematic errors and theoretical predictions, that will enable one to deliver a stringent and robust test of different dark matter models in the next decade. With the advent of the next generation of sky surveys, the number of known strong gravitational lens systems is expected to increase by several orders of magnitude. Coupled with high-resolution follow-up observations, these data will provide a key opportunity to constrain the properties of dark matter with strong gravitational lensing.

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The lensing properties of subhaloes in massive elliptical galaxies in sterile neutrino cosmologies

Abstract: The version presented here may differ from the published version or from the version of the record. Please see the repository URL above for details on accessing the published version and note that access may require a subscription.

Cited by 29 publications

References 99 publications

The spatial distribution of Milky Way satellites, gaps in streams, and the nature of dark matter

The spatial distribution of Milky Way satellites, gaps in streams, and the nature of dark matter

The halo mass function in alternative dark matter models

Strong Gravitational Lensing as a Probe of Dark Matter

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