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SUSY in the sky: supersymmetric dark matter

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SUSY in the sky: supersymmetric dark matter. David G. Cerdeño Institute for Particle Physics Phenomenology. Based on works with S.Baek, K.Y.Choi, C.Hugonie, K.Jedamzik, Y.G.Kim, P.Ko, D.López-Fogliani, C.Muñoz, R.R. de Austri, L.Roszkowski, A.M.Teixeira. Contents. Present status - PowerPoint PPT Presentation

Text of SUSY in the sky: supersymmetric dark matter

  • SUSY in the sky: supersymmetric dark matterDavid G. CerdeoInstitute for Particle Physics Phenomenology Based on works with S.Baek, K.Y.Choi, C.Hugonie, K.Jedamzik, Y.G.Kim, P.Ko, D.Lpez-Fogliani, C.Muoz, R.R. de Austri, L.Roszkowski, A.M.Teixeira

  • 2-12-05 DurhamContents Present status

    Dark matter is a necessary ingredient in present models for the Universe but we have not identified it yet

    Can it be the Lightest Supersymmetric Particle (LSP)?

    Direct detection experiments will continue providing data in the near future.

    It may be detected in running or projected dark matter experiments?The lightest Neutralino?

    Or maybe not?

    The gravitino (or the axino)?

  • 2-12-05 DurhamSUSY dark matter The lightest Neutralino

  • 2-12-05 DurhamDirect detection of Neutralinos Could the lightest neutralino be found in direct detection experiments?Direct detection through the elastic scattering of a WIMP with nuclei inside a detector.Many experiments around the world are currently looking for this signal with increasing sensitivitiesHow large can the neutralino detection cross section be?Could we explain a hypothetical WIMP detection with neutralino dark matter?

  • 2-12-05 DurhamNeutralinos How large can the direct detection cross section for neutralinos be?1) In which theory? (field content, interactions, parameters)

    MSSM NMSSM

    Parameters given at the GUT scale MGUT (e.g., coming from SUGRA theories) or at the EW scale (effMSSM)2) Effect of experimental constraints?

    masses of superpartners

    Low energy observables ( (g-2)m , bsg, BS m+m-, )

    3) Reproduce the correct relic density?

  • 2-12-05 DurhamNeutralinos In the MSSM the mechanisms which allow for an increase in the detection cross section are well knownIn the MSSM, the neutralino is a physical superposition of the B, W, H1, H2The detection properties of the neutralino depend on its composition~~~~

  • 2-12-05 DurhamNeutralinos Large detection cross sectionsSquark-exchangeHiggs-exchangeLeading contribution. It can increase when The Higgsino components of the neutralino increase The Higgs masses decrease

  • 2-12-05 DurhamNeutralinosHiggs-exchangeLeading contribution. It can increase when The Higgsino components of the neutralino increase The Higgs masses decrease In terms of the mass parameters in the RGEmHd2mHu2Non-universal soft terms (e.g., in the Higgs sector)MGUTmHu2 mHd2

  • 2-12-05 DurhamNeutralinosHiggs-exchangeLeading contribution. It can increase when The Higgsino components of the neutralino increase The Higgs masses decrease In terms of the mass parameters in the RGEmHd2mHu2Non-universal soft terms (e.g., in the Higgs sector)MGUTMIOr intermediate scalesmHu2 mHd2

  • 2-12-05 DurhamNeutralinosIn a general Supergravity theory (Non-universal soft supersymmetry-breaking terms in the scalar and gaugino sector) the neutralino can be within the reach of dark matter detectors for a wide range of masses. Very light Neutralinos

    Bino-likeHeavy Neutralinos

    Bino-HiggsinoM1

  • 2-12-05 DurhamNeutralinos Neutralinos in the NMSSMIn the Next-to-MSSM, the neutralino has a new singlino (S) component.The detection properties depend on the neutralino composition~

  • 2-12-05 DurhamNeutralinos Large detection cross sections in the NMSSMSquark-exchangeHiggs-exchangeLeading contribution. It can increase when The Higgsino components of the neutralino increase The Higgs masses decrease

  • 2-12-05 DurhamNeutralinos Large detection cross sections in the NMSSMHiggs-exchangeLeading contribution. It can increase when The Higgsino components of the neutralino increaseHiggses lighter than 70 GeV and mostly singlet-likeThe relic density for these neutralinos is still to be calculated. The Higgs masses decrease

  • 2-12-05 DurhamSUSY dark matter The lightest Neutralino

    The Gravitino

  • 2-12-05 DurhamGravitinos The gravitino can be the LSP in SupergravityThe gravitino mass depends on the SUSY-breaking mechanism

  • 2-12-05 DurhamGravitinos Gravitino production mechanisms Thermal production

    Through scattering processes and an annihilation with (s)particles during thermal expansion of the Early Universe.

    Non-thermal production

    Through late decays of the NLSP (normally staus or neutralinos) Constraints from NucleosynthesisLate decays of the NLSP can generate highly energetic electromagnetic and hadronic fluxes which may alter significantly the abundances of light elements (thus spoiling the success of Big Bang Nucleosynthesis).

  • 2-12-05 DurhamGravitinos In mSUGRAAll the regions where the neutralino is the NLSP are excluded by BBN constraints. Only part of those areas with stau NLSP are left. In order to obtain the correct relic density of dark matter thermal production alone is not sufficient. Important contributions from non-thermal production are also necessary.In the remaining regions the Fermi vacuum is metastable. The global minimum breaks charge and/or colour.

  • 2-12-05 DurhamSummary The identification of dark matter is still an open problem pointing towards physics beyond the SM. Supersymmetric dark matter is one of the most attractive possibilities with an interesting future: The lightest neutralino (both in the MSSM and NMSSM) could explain a hypothetical detection of WIMP dark matter in the next generation experiments Gravitino dark matter would lead to an interesting phenomenology

    Charged observable LSP (stau)

    No detection in dark matter experiments

    The Fermi vacuum may be metastable