Integrating out astrophysical uncertainties

Fox, Patrick J.; Liu, Jia; Weiner, Neal

doi:10.1103/physrevd.83.103514

Cited by 162 publications

(233 citation statements)

References 58 publications

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“…For example, the direct detection limits rely on an assumption about the local dark matter density and velocity distributions, the latter of which is expected to vary from the standard assumptions used in the experimental results [59][60][61][62][63][64][65]. While it is possible to some degree to disentangle the astrophysical uncertainties to place limits on the fundamental parameters [66][67][68][69][70][71], we cannot lose sight of the assumptions that went into the analysis. Similarly, the parameters that are required to obtain a thermal relic abundance can be changed significantly if additional particles (beyond the minimal set in our benchmark simplified models) are present in the spectrum, or if the flavor-universal assumption for the coupling g v is lifted.…”

Section: Non-collider Boundsmentioning

confidence: 99%

Scalar simplified models for dark matter

2015

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We introduce a set of minimal simplified models for dark matter interactions with the Standard Model, connecting the two sectors via either a scalar or pseudoscalar particle. These models have a wider regime of validity for dark matter searches at the LHC than the effective field theory approach, while still allowing straightforward comparison to results from non-collider dark matter detection experiments. Such models also motivate dark matter searches in multiple correlated channels. In this paper, we constrain scalar and pseudoscalar simplified models with direct and indirect detection experiments, as well as from existing LHC searches with missing energy plus tops, bottoms, or jets, using the exact loop-induced coupling with gluons. This calculation significantly affects key differential cross sections at the LHC, and must be properly included. We make connections with the Higgs sector, and conclude with a discussion of future searches at the LHC.

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Section: Non-collider Boundsmentioning

confidence: 99%

Scalar simplified models for dark matter

2015

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“…On the assumption that there is no dark form factor, the event distributions (once we have compensated for the different target nuclei) with respect to v min should be the same for each of the experiments [26][27][28][29][30][31] -any disagreement indicates the presence of some extra effect. For a dark form factor, since q(v min ) = 2µ XN v min , changing µ XN by changing m N will change the range of F X (q) that we sample (significantly so if the DM mass is larger than those of the SM target nuclei).…”

Section: Jhep07(2015)133mentioning

confidence: 99%

Signatures of large composite Dark Matter states

Hardy

Lasenby

March-Russell

et al. 2015

J. High Energ. Phys.

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Abstract:We investigate the interactions of large composite dark matter (DM) states with the Standard Model (SM) sector. Elastic scattering with SM nuclei can be coherently enhanced by factors as large as A 2 , where A is the number of constituents in the composite state (there exist models in which DM states of very large A 10 8 may be realised). This enhancement, for a given direct detection event rate, weakens the expected signals at colliders by up to 1/A. Moreover, the spatially extended nature of the DM states leads to an additional, characteristic, form factor modifying the momentum dependence of scattering processes, altering the recoil energy spectra in direct detection experiments. In particular, energy recoil spectra with peaks and troughs are possible, and such features could be confirmed with only O(50) events, independently of the assumed halo velocity distribution. Large composite states also generically give rise to low-energy collective excitations potentially relevant to direct detection and indirect detection phenomenology. We compute the form factor for a generic class of such excitations -quantised surface modes -finding that they can lead to coherently-enhanced, but generally sub-dominant, inelastic scattering in direct detection experiments. Finally, we study the modifications to capture rates in astrophysical objects that follow from the elastic form factor, as well as the effects of inelastic interactions between DM states once captured. We argue that inelastic interactions may lead to the DM collapsing to a dense configuration at the centre of the object.

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“…Models of the type considered here retain the appeal of the thermal relic hypothesis while remaining experimentally verifiable. We have furthermore demonstrated that in this class of indirect annihilation searches, all astrophysical uncertainties can be "integrated out" [40] and experimental sensitivities can be directly compared.…”

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confidence: 99%

“…The kinematics of scattering in the non-relativistic case are controlled by the minimum DM particle velocity, v min (E R ), required to produce a nuclear recoil of energy E R . In the absence of unknown form factors, all experimental data can be mapped into v minspace at each DM mass and compared without specifying the nature of the astrophysical distribution or density of DM [39,40]. These "halo-independent" methods have received significant attention [41][42][43][44][45][46][47][48][49][50][51][52][53][54][55][56].…”

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confidence: 99%

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Direct Detection Phenomenology in Models Where the Products of Dark Matter Annihilation Interact with Nuclei

2015

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We investigate the direct detection phenomenology of a class of dark matter (DM) models in which DM does not directly interact with nuclei, but rather the products of its annihilation do. When these annihilation products are very light compared to the DM mass, the scattering in direct detection experiments is controlled by relativistic kinematics. This results in a distinctive recoil spectrum, a non-standard and or even absent annual modulation, and the ability to probe DM masses as low as a ∼10 MeV. We use current LUX data to show that experimental sensitivity to thermal relic annihilation cross sections has already been reached in a class of models. Moreover, the compatibility of dark matter direct detection experiments can be compared directly in Emin space without making assumptions about DM astrophysics, mass, or scattering form factors. Lastly, when DM has direct couplings to nuclei, the limit from annihilation to relativistic particles in the Sun can be stronger than that of conventional non-relativistic direct detection by more than three orders of magnitude for masses in a 2-7 GeV window.Introduction -While very little is known about Dark Matter (DM), its cosmological abundance is experimentally quite well-determined: Ω CDM h 2 = 0.1199 ± 0.0027 [1]. An appealing framework for understanding the relic abundance of Dark Matter (DM) is thermal freeze-out [2]. Number-changing interactions in the early universe, XX ↔ (SM)SM keep DM in thermal equilibrium with the SM bath, until the rate of these annihilation processes drops below the rate of Hubble expansion. After this point the abundance of DM is essentially fixed at, Ω CDM h 2 0.12 6 × 10 −26 cm 3 s −1 / σ ann v rel , singling out a characteristic annihilation cross section σ ann v rel for thermally produced DM to yield the observed abundance. This scenario is attractive in that it provides a simple and elegant framework for the relic abundance that can be tested in a variety of ways, including direct detection (DD) [3]. However, current constraints from DD rule out many of the simplest models of thermal relic DM, which may indicate a modification of the above picture.In this paper we investigate a modification of thermal DM which alleviates the tension between DD constraints and the thermal relic hypothesis, while making unique predictions for DD. In particular, we take the abundance of DM, X, to be determined by the annihilation process XX ↔ Y Y , where Y is a much lighter dark sector species. The interactions of the dark sector state Y with ordinary nuclei allows for a unique test of the scenario at DD experiments. The resulting DD phenomenology of this class of models is distinctive, owing to the fact that (1) the scattering partner of the nucleus is relativistic, rendering the kinematics of scattering completely different and (2) it is the flux of the scattering partner Y that determines the rate of events at a detector rather than X. Both of these features have novel consequences not considered in the literature of "model-independent" direct detecti...

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Integrating out astrophysical uncertainties

Cited by 162 publications

References 58 publications

Scalar simplified models for dark matter

Scalar simplified models for dark matter

Signatures of large composite Dark Matter states

Direct Detection Phenomenology in Models Where the Products of Dark Matter Annihilation Interact with Nuclei

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