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Probing neutralino dark matter in the MSSM and the NMSSM with directional detection

D. Albornoz Vásquez, G. Bélanger, J. Billard, and F. Mayet
Phys. Rev. D 85, 055023 – Published 28 March 2012
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  • INTRODUCTION
  • DIRECTIONAL DETECTION FRAMEWORK
  • SPIN-DEPENDENT ELASTIC SCATTERING…
  • TESTING SUPERSYMMETRIC CONFIGURATIONS
  • RESULTS
  • IMPACT OF LHC RESULTS ON THE PARAMETER…
  • A DISCOVERY SCENARIO
  • CONCLUSION
  • ACKNOWLEDGEMENTS
    • References

    Abstract

    We investigate the capability of directional detectors to probe neutralino dark matter in the minimal supersymmetric standard model and the next-to-minimal supersymmetric standard model with parameters defined at the weak scale. We show that directional detectors such as the future MIMAC detector will probe spin-dependent dark matter scattering on nucleons that are beyond the reach of current spin-independent detectors. The complementarity between indirect searches, in particular, using gamma rays from dwarf spheroidal galaxies, spin-dependent and spin-independent direct search techniques is emphasized. We comment on the impact of the negative results on squark searches at the LHC. Finally, we investigate how the fundamental parameters of the models can be constrained in the event of a dark matter signal.

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    • Received 30 January 2012

    DOI:https://doi.org/10.1103/PhysRevD.85.055023

    © 2012 American Physical Society

    Authors & Affiliations

    D. Albornoz Vásquez1,2, G. Bélanger1, J. Billard3, and F. Mayet3

    • 1LAPTH, U. de Savoie, CNRS, BP 110, 74941 Annecy-Le-Vieux, France
    • 2Institut d’Astrophysique de Paris, UMR 7095 CNRS, Université Pierre et Marie Curie, 98 bis Boulevard Arago, Paris 75014, France
    • 3Laboratoire de Physique Subatomique et de Cosmologie, Université Joseph Fourier Grenoble 1, CNRS/IN2P3, Institut Polytechnique de Grenoble, Grenoble, France

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    Issue

    Vol. 85, Iss. 5 — 1 March 2012

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    Images

    • Figure 1
      Figure 1
      Spin-dependent cross section on proton (cm2) as a function of the WIMP mass (GeV) in the case of the pure-proton approximation [75] showing the sensitivity of a forthcoming 30  kg·year directional experiment (solid red line). It is defined as the minimal cross section required to obtain a DM discovery with a significance greater than the 3σ level at 90% C.L. [6]. For the same exposure, the dotted black line presents the projected exclusion limit [8] in the background-free case. The red star is the input value of the benchmark model and the black contour is the 68% contour level obtained with the MCMC analysis [9]. The exclusion limit from COUPP-2010 [11] (black dotted line) is also presented.Reuse & Permissions
    • Figure 2
      Figure 2
      Feynman diagrams contributing to spin-dependent elastic scattering of neutralinos on nucleons.Reuse & Permissions
    • Figure 3
      Figure 3
      Left (resp. right) panel present the constraints in the constructive (resp. destructive) case, for a 20  GeV. The light grey area is the region already excluded by the most constraining experiments (COUPP-2010 [11] and XENON10 [12]). For a 30  kg·year CF4 directional detector, the dark grey area is the 3σ discovery region, while the solid light curve labeled “exclusion” is the background-free projected limit. Dashed light curve presents the same result for the alternative F19 spin content values [81].Reuse & Permissions
    • Figure 4
      Figure 4
      Spin-independent cross section versus the neutralino mass. Top: MSSM. Bottom: NMSSM. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region. The CDMS-II [23] and XENON100 [20] limits are also displayed.Reuse & Permissions
    • Figure 5
      Figure 5
      Flux of γ rays expected from neutralino annihilations from the Draco dwarf spheroidal galaxy versus the neutralino mass. Top: MSSM. Bottom: NMSSM. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region. The Fermi-LAT limits [102] are also displayed.Reuse & Permissions
    • Figure 6
      Figure 6
      Proton-neutralino spin-dependent elastic scattering cross section versus the neutralino mass with the exclusion and discovery projections for a nominal directional detector. Top: MSSM. Bottom: NMSSM. In blue safe points and in yellow points excluded by either XENON100 or Fermi-LAT.Reuse & Permissions
    • Figure 7
      Figure 7
      Spin-dependent elastic scattering cross sections correlations: proton-neutralino versus neutron-neutralino interactions. Contrarily to Fig. 3, the result is presented for all neutralino masses. Top: MSSM. Bottom: NMSSM. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region.Reuse & Permissions
    • Figure 8
      Figure 8
      Frequency distribution of ap/an. Top: MSSM. Bottom: NMSSM. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region.Reuse & Permissions
    • Figure 9
      Figure 9
      Flux of γ rays expected from neutralino annihilations from the Draco dwarf spheroidal galaxy versus spin-independent cross section. Top: MSSM. Bottom: NMSSM. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region. The Fermi-LAT limits [102] are also displayed. Points excluded by XENON100 are not shown.Reuse & Permissions
    • Figure 10
      Figure 10
      Correlation plot between the μ mass term and the bino mass M1. Top: MSSM. Bottom: NMSSM. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region.Reuse & Permissions
    • Figure 11
      Figure 11
      Free parameter frequency distribution normalized to Qmax in the MSSM run. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region.Reuse & Permissions
    • Figure 12
      Figure 12
      Free parameter frequency distribution normalized to Qmax in the NMSSM run. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region.Reuse & Permissions
    • Figure 13
      Figure 13
      Top Panel: Spin-dependent elastic scattering cross sections correlations: proton-neutralino versus neutron-neutralino interactions in the MSSM. In pink the points in the discovery region of directional detectors and in cyan in the exclusion region. Here, in contrast with Figs. 7, we have removed those points falling above the ATLAS limit on the Mq˜ vs Mg˜ plane. Bottom panel: frequency distribution of ap/an for the same points with the same color code.Reuse & Permissions
    • Figure 14
      Figure 14
      Proton-neutralino spin-dependent elastic scattering cross section versus the neutralino mass in the discovery scenario runs. Top: MSSM. Bottom: NMSSM. We display the 1σ and 3σ contours, while we used the former as the constraint for the random walk. Also displayed are the exclusion and discovery projections for a nominal directional detector. We display only safe points regarding XENON100, Fermi-LAT and CMS (MSSM only) limits on SI elastic scattering interactions, γ rays from the Draco dSph, and Higgs interactions.Reuse & Permissions
    • Figure 15
      Figure 15
      Free parameter frequency distribution normalized to Qmax in the MSSM discovery scenario run.Reuse & Permissions
    • Figure 16
      Figure 16
      Flux of γ rays expected from neutralino annihilations from the Draco dwarf spheroidal galaxy versus spin-independent cross section. Top: MSSM. Bottom: NMSSM. The Fermi-LAT limits [102] are also displayed. Only the points overcoming all constraints (from XENON100, Fermi-LAT and CMS) in the discovery scenario are displayed.Reuse & Permissions
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