A Robust Mass Estimator for Dark Matter Subhalo Perturbations in Strong Gravitational Lenses

Minor, Quinn E.; Kaplinghat, Manoj; Li, Nan

doi:10.3847/1538-4357/aa7fee

Cited by 35 publications

(46 citation statements)

References 64 publications

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“…The values obtained are degenerate, as already found in simulations investigated in Minor et al (2017), Sluse et al (2017), and Vegetti & Vogelsberger (2014). The model-independent approach derived in this work explains these degeneracies from a more general viewpoint, especially the fact that the degeneracy between the perturber and the main lens is not only a degeneracy between different classes of lens models, but a modelindependent degeneracy already contained in the general lensing equations.…”

supporting

confidence: 72%

“…Vegetti & Koopmans 2009;Vegetti & Vogelsberger 2014), and other ansatzes to describe perturbers, (e.g. Minor et al 2017). Thus, coupling the modelindependent equations, Eqs.…”

Section: General Estimatesmentioning

confidence: 99%

“…Existing approaches for some of these applications were developed in Habara & Yamamoto (2011), Koopmans (2005), Minor et al (2017), Suyu et al (2017), and Vegetti & Koopmans (2009). They employ parametric models or a combination of Article number, page 1 of 11 arXiv:1705.07195v3 [astro-ph.CO] 13 Jun 2018 A&A proofs: manuscript no.…”

Section: Introductionmentioning

confidence: 99%

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Generalised model-independent characterisation of strong gravitational lenses

Wagner

2018

A&A

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In galaxy-galaxy strong gravitational lensing, Einstein rings are generated when the lensing galaxy has an axisymmetric lensing potential and the source galaxy is aligned with its symmetry centre along the line of sight. Using a Taylor expansion around the Einstein radius and eliminating the unknown source, I derive a set of analytic equations that determine differences of the deflection angle of the perturber weighted by the convergence of the axisymmetric lens and ratios of the convergences at the positions of the arcs from the measurable thickness of the arcs. In the same manner, asymmetries in the brightness distributions along an arc determine differences in the deflection angle of the perturber if the source has a symmetric brightness profile and is oriented parallel to or orthogonal to the caustic. These equations are the only model-independent information retrievable from observations to leading order in the Taylor expansion. General constraints on the derivatives of the perturbing lens are derived such that the perturbation does not change the number of critical curves. To infer physical properties such as the mass of the perturber or its position, models need to be inserted. The same conclusions about the scale of detectable masses (of the order of 10 8 M ) and model-dependent degeneracies as in other approaches are then found and supported by analysing B1938+666 as an example. Yet, the model-independent equations show that there is a fundamental degeneracy between the main lens and the perturber that can only be broken if their relative position is known. This explains the degeneracies between lens models already found in simulations from a more general viewpoint. Hence, apart from the radii and brightness distributions of the arcs, independent information on the axisymmetric lens or the perturber has to be employed to disentangle the axisymmetric lens and the perturber. Depending on the properties of the pertuber, this degeneracy can be broken by characterising the surrounding of the lens or by measuring the time delay between quasar images embedded in the perturbed Einstein ring of the host galaxy.

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supporting

confidence: 72%

“…Vegetti & Koopmans 2009;Vegetti & Vogelsberger 2014), and other ansatzes to describe perturbers, (e.g. Minor et al 2017). Thus, coupling the modelindependent equations, Eqs.…”

Section: General Estimatesmentioning

confidence: 99%

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Generalised model-independent characterisation of strong gravitational lenses

Wagner

2018

A&A

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“…However, Despali et al (2018) have shown that assuming a constant mass-concentration relation from Duffy et al (2008) plays only a secondary effect and leads to an error on the inferred mass of 5 per cent for subhaloes with masses of 10 5−6 M and 20 per cent for masses of 10 9 M . These errors are significantly smaller than the de-projection errors on the total mass of pseudo-Jaffe profiles (Minor et al 2017;Despali et al 2018) and it leads to an error on the expected number of substructures of the order of 10 per cent.…”

Section: Small Mass Haloes As Analytical Mass Componentsmentioning

confidence: 91%

Low-mass halo perturbations in strong gravitational lenses at redshift z ∼ 0.5 are consistent with CDM

Ritondale

Vegetti

Despali

et al. 2019

Monthly Notices of the Royal Astronomical Society

123

114

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We use a sample of 17 strong gravitational lens systems from the BELLS GALLERY survey to quantify the amount of low-mass dark matter haloes within the lensing galaxies and along their lines of sight, and to constrain the properties of dark matter. Based on a detection criterion of 10σ, we report no significant detection in any of the lenses. Using the sensitivity function at the 10-σ level, we have calculated the predicted number of detectable cold dark matter (CDM) line-of-sight haloes to be µ l = 1.17 ± 1.08, in agreement with our null detection. Assuming a detection sensitivity that improved to the level implied by a 5-σ threshold, the expected number of detectable line-of-sight haloes rises to µ l = 9.0 ± 3.0. Whilst the current data find zero detections at this sensitivity level (which has a probability of P 5σ CDM (n det = 0)=0.0001 and would be in strong tension with the CDM framework), we find that such a low detection threshold leads to many spurious detections and non-detections and therefore the current lack of detections is unreliable and requires data with improved sensitivity. Combining this sample with a subsample of 11 SLACS lenses, we constrain the half-mode mass to be log(M hm ) < 12.26 at the 2-σ level. The latter is consistent with resonantly produced sterile neutrino masses m s < 0.8 keV at any value of the lepton asymmetry at the 2-σ level.

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“…On these scales, such substructures would be completely dark matter dominated, and contain too few stars to be observed directly. A number of strategies have been proposed to indirectly probe low mass dark matter halos, including analyses of the impact on Lyα forest observations [14][15][16][17][18][19][20] and perturbations of strong gravitational lenses [21][22][23][24][25][26][27][28][29].…”

Section: Introductionmentioning

confidence: 99%

Probing the nature of dark matter particles with stellar streams

Banik

Bertone

Bovy

et al. 2018

J. Cosmol. Astropart. Phys.

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A key prediction of the standard cosmological model -which relies on the assumption that dark matter is cold, i.e. non-relativistic at the epoch of structure formationis the existence of a large number of dark matter substructures on sub-galactic scales. This assumption can be tested by studying the perturbations induced by dark matter substructures on cold stellar streams. Here, we study the prospects for discriminating cold from warm dark matter by generating mock data for upcoming astronomical surveys such as the Large Synoptic Survey Telescope (LSST), and reconstructing the properties of the dark matter particle from the perturbations induced on the stellar density profile of a stream. We discuss the statistical and systematic uncertainties, and show that the method should allow to set stringent constraints on the mass of thermal dark matter relics, and possibly to yield an actual measurement of the dark matter particle mass if it is in the O(1) keV range.

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A Robust Mass Estimator for Dark Matter Subhalo Perturbations in Strong Gravitational Lenses

Cited by 35 publications

References 64 publications

Generalised model-independent characterisation of strong gravitational lenses

Generalised model-independent characterisation of strong gravitational lenses

Low-mass halo perturbations in strong gravitational lenses at redshift z ∼ 0.5 are consistent with CDM

Probing the nature of dark matter particles with stellar streams

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