Refinement of the standard halo model for dark matter searches in light of the Gaia Sausage

Evans, N. W.; O’Hare, Ciaran A. J.; McCabe, Christopher

doi:10.1103/physrevd.99.023012

Cited by 178 publications

(179 citation statements)

References 191 publications

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“…Our results are in good agreement with the literature (e.g. Evans et al 2019;Bozorgnia et al 2019), and predict that the DM particles have a preference for radial orbits, with β = 0.14 +0.07 −0.03 , and that the SHM overpredicts the high velocity tail of the velocity distribution. Furthermore, by using multiple action distributions, we have characterised the halo-to-halo scatter in the velocity distribution, which is important for understanding how robust are the constraints inferred from direct DM detection experiments.…”

Section: Discussionsupporting

confidence: 92%

The orbital phase space of contracted dark matter haloes

Callingham

Cautun

Deason

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the orbital phase-space of dark matter (DM) halos in the auriga suite of cosmological hydrodynamics simulations of Milky Way analogues. We characterise halos by their spherical action distribution, F (J r , L), a function of the specific angular momentum, L, and the radial action, J r , of the DM particles. By comparing DM-only and hydrodynamical simulations of the same halos, we investigate the contraction of DM halos caused by the accumulation of baryons at the centre. We find a small systematic suppression of the radial action in the DM halos of the hydrodynamical simulations, suggesting that the commonly used adiabatic contraction approximation can result in an underestimate of the density by ∼ 8%. We apply an iterative algorithm to contract the auriga DM halos given a baryon density profile and halo mass, recovering the true contracted DM profiles with an accuracy of ∼ 15%, that reflects halo-to-halo variation. Using this algorithm, we infer the total mass profile of the Milky Way's contracted DM halo. We derive updated values for the key astrophysical inputs to DM direct detection experiments: the DM density and velocity distribution in the Solar neighbourhood.

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Section: Discussionsupporting

confidence: 92%

The orbital phase space of contracted dark matter haloes

Callingham

Cautun

Deason

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Most of the millisecond binary pulsars observed to date are located in ∼ 2 kpc neighbourhood of the Solar System. The Milky Way halo models give DM density in this regionρ DM ∼ 0.3 ÷ 0.6 GeV/cm 3 [49][50][51]. In our numerical estimates we will use a conservative proxȳ ρ DM = 0.3 GeV/cm 3 .…”

Section: Ultralight Dark Matter In the Halomentioning

confidence: 99%

“…The former are due to the oscillating contribution in Φ 2 /2, see Eq. (51), and appear if m Φ is close to N ω b /2. They are the same as for linear coupling.…”

Section: Evolution Of the Orbital Elements: Quadratic Couplingmentioning

confidence: 99%

Secular effects of ultralight dark matter on binary pulsars

2020

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Dark matter (DM) can consist of very light bosons behaving as a classical scalar field that experiences coherent oscillations. The presence of this DM field would perturb the dynamics of celestial bodies, either because the (oscillating) DM stress tensor modifies the gravitational potentials of the galaxy, or if DM is directly coupled to the constituents of the body. We study secular variations of the orbital parameters of binary systems induced by such perturbations. Two classes of effects are identified. Effects of the first class appear if the frequency of DM oscillations is in resonance with the orbital motion; these exist for general DM couplings including the case of purely gravitational interaction. Effects of the second class arise if DM is coupled quadratically to the masses of the binary system members and do not require any resonant condition. The exquisite precision of binary pulsar timing can be used to constrain these effects. Current observations are not sensitive to oscillations in the galactic gravitational field, though a discovery of pulsars in regions of high DM density may improve the situation. For DM with direct coupling to ordinary matter, the current timing data are already competitive with other existing constraints in the range of DM masses ∼ 10 −22 − 10 −18 eV. Future observations are expected to increase the sensitivity and probe new regions of parameters.

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“…Another promising avenue to look for interesting signatures of DM substructure are axion searches and directional detection experiments as discussed in refs. [37][38][39]. The main drawback of the aforementioned analyses is the underlying assumption of a near perfect stellar-DM velocity correlation.…”

Section: Introductionmentioning

confidence: 99%

Implications of the Gaia sausage for dark matter nuclear interactions

2020

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The advent of the Gaia era has led to potentially revolutionary understanding of dark matter (DM) dynamics in our galaxy, which has important consequences for direct detection (DD) experiments. In this paper, we study how the empirical DM velocity distribution inferred from Gaia-Sausage, a dominant substructure in the solar neighborhood, affects the interpretation of DD data. We survey different classes of operators in the non-relativistic effective field theory that could arise from several relativistic benchmark models and emphasize that the Gaia velocity distribution could modify both the total number of events as well as the shape of the differential recoil spectra, the two primary observables in DD experiments. Employing the euclideanized signal method, we investigate the effects of the Gaia distribution on reconstructing DM model parameters and identifying the correct DM model given a positive signal at future DD experiments. We find that for light DM with mass ∼ 10 GeV, the Gaia distribution poses an additional challenge for characterizing DM interactions with ordinary matter, which may be addressed by combining complementary DD experiments with different targets and lowering the detection threshold. Meanwhile, for heavy DM with mass above ∼ 30 GeV, depending on the type of DM model, there could be a (moderate) improvement in the sensitivity at future DD experiments.

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Refinement of the standard halo model for dark matter searches in light of the Gaia Sausage

Cited by 178 publications

References 191 publications

The orbital phase space of contracted dark matter haloes

The orbital phase space of contracted dark matter haloes

Secular effects of ultralight dark matter on binary pulsars

Implications of the Gaia sausage for dark matter nuclear interactions

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