Discriminating dark matter candidates using direct detection

Bélanger, G.; Nezri, E.; Pukhov, A.

doi:10.1103/physrevd.79.015008

Cited by 31 publications

(33 citation statements)

References 124 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(7). This would correspond, e.g., to a DM candidate whose SD interaction is dominated by Z exchange [66]. Other choices of a p =a n lead to qualitatively similar results (but then a linear combination with the other components, S 00 and S 01 , also appears).…”

Section: Resultssupporting

confidence: 64%

Nuclear uncertainties in the spin-dependent structure functions for direct dark matter detection

et al. 2013

View full text Add to dashboard Cite

We study the effect that uncertainties in the nuclear spin-dependent structure functions have in the determination of the dark matter (DM) parameters in a direct detection experiment.We show that different nuclear models that describe the spin-dependent structure function of specific target nuclei can lead to variations in the reconstructed values of the DM mass and scattering cross section. We propose a parametrization of the spin structure functions that allows us to treat these uncertainties as variations of three parameters, with a central value and deviation that depend on the specific nucleus. The method is illustrated for germanium and xenon detectors with an exposure of 300 kg yr, assuming a hypothetical detection of DM and studying a series of benchmark points for the DM properties. We find that the effect of these uncertainties can be similar in amplitude to that of astrophysical uncertainties, especially in those cases where the spin-dependent contribution to the elastic scattering cross section is sizableD. G. C. is supported by the Ramo´n y Cajal program of the Spanish MICINN. M. F. is supported by a Leverhulme Trust grant. J.-H. H. is supported by a MultiDark Fellowship. M. P. is supported by a MultiDark Scholarship. This work was supported by the Consolider-Ingenio 2010 Programme under MultiDark Grant No. CSD2009-00064. We also thank the support of the Spanish MICINN under Grants No. FPA2009-08958 and FPA2012-34694, the Spanish MINECO ‘‘Centro de excelencia Severo Ochoa Program’’ under Grant No. SEV-2012-0249, the Community of Madrid under Grant No. HEPHACOS S2009/ESP-1473, and the European Union under the Marie Curie-ITN Program No. PITN-GA-2009-23792

show abstract

Section: Resultssupporting

confidence: 64%

Nuclear uncertainties in the spin-dependent structure functions for direct dark matter detection

et al. 2013

View full text Add to dashboard Cite

show abstract

“…While σ SD is typically considerably larger than σ SI , SI experimental constraints are commensurately stronger than SD, so these two limits are comparable in strength [21,22]. Note that σ SI depends on nuclear form factors, in particular the strange quark content of the nucleon.…”

Section: Observational Constraintsmentioning

confidence: 98%

Prospects and blind spots for neutralino dark matter

Cheung

Hall²,

Pinner³

et al. 2013

J. High Energ. Phys.

198

271

View full text Add to dashboard Cite

Using a simplified model framework, we assess observational limits and discovery prospects for neutralino dark matter, taken here to be a general admixture of bino, wino, and Higgsino. Experimental constraints can be weakened or even nullified in regions of parameter space near 1) purity limits, where the dark matter is mostly bino, wino, or Higgsino, or 2) blind spots, where the relevant couplings of dark matter to the Z or Higgs bosons vanish identically. We analytically identify all blind spots relevant to spin-independent and spin-dependent scattering and show that they arise for diverse choices of relative signs among M 1 , M 2 , and µ. At present, XENON100 and IceCube still permit large swaths of viable parameter space, including the well-tempered neutralino. On the other hand, upcoming experiments should have sufficient reach to discover dark matter in much of the remaining parameter space. Our results are broadly applicable, and account for a variety of thermal and non-thermal cosmological histories, including scenarios in which neutralinos are just a component of the observed dark matter today. Because this analysis is indifferent to the fine-tuning of electroweak symmetry breaking, our findings also hold for many models of neutralino dark matter in the MSSM, NMSSM, and Split Supersymmetry. We have identified parameter regions at low tan β which sit in a double blind spot for both spin-independent and spin-dependent scattering. Interestingly, these low tan β regions are independently favored in the NMSSM and models of Split Supersymmetry which accommodate a Higgs mass near 125 GeV.1

show abstract

“…Moreover, in order to eliminate the large astrophysical and theoretical uncertainties which affect the dark matter rates, the ratio of WIMP-proton and WIMP-neutron amplitudes can be used [152] and compared for different target materials. For example, the comparative study of the ratios of SD Left) The detection with a given target such as CF 3 I can only loosely constrain models for the dark matter (blue squares for neutralinos, green circles for the LKP) in the σ SI p /σ SD p versus count-rate plane.…”

Section: Discrimination Of Dark Matter Candidatesmentioning

confidence: 99%

Direct detection of WIMPs

Cerdeño¹,

Green²

2010

Particle Dark Matter

View full text Add to dashboard Cite

Citation for published item:gerde£ noD hFqF nd qreenD eFwF @PHIHA 9hiret detetion of swsF9D in rtile drk mtterX oservtionsD models nd serhesF gmridgeX gmridge niversity ressD ppF QRUEQTWF Further information on publisher's website: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. Abstract A generic weakly interacting massive particle (WIMP) is one of the most attractive candidates to account for the cold dark matter in our Universe, since it would be thermally produced with the correct abundance to account for the observed dark matter density. WIMPs can be searched for directly through their elastic scattering with a target material, and a variety of experiments are currently operating or planned with this aim. In these notes we overview the theoretical calculation of the direct detection rate of WIMPs as well as the different detection signals. We discuss the various ingredients (from particle physics and astrophysics) that enter the calculation and review the theoretical predictions for the direct detection of WIMPs in particle physics models.

show abstract

Discriminating dark matter candidates using direct detection

Cited by 31 publications

References 124 publications

Nuclear uncertainties in the spin-dependent structure functions for direct dark matter detection

Nuclear uncertainties in the spin-dependent structure functions for direct dark matter detection

Prospects and blind spots for neutralino dark matter

Direct detection of WIMPs

Contact Info

Product

Resources

About