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Neutralino Dark matter detection in the MSSM and NMSSM David G. Cerdeo D.G.C., C. Muoz, JHEP 10 (2004) 015 S. Baek, D.G.C., Y.G. Kim, P . Ko, C. Muoz, arXiv:hep-ph/0505019 D.G.C., C. Hugonie, D. Lpez-Fogliani, C. Muoz, A.M. Teixeira,

  1. ✱ ❅ ✓ ✌ ✝☞ Usual Suspects The nature of Dark Matter is still to be deciphered. » Outline Introduction » Motivation for Dark Matter Baryonic Matter: (cold gas, MACHO’s, white dwarves...) is not suf£cient » Motivation for Dark Matter » Cosmological parameters (inconsistent with BBN) from CMB » Usual Suspects Non-Baryonic Candidates: are provided by particle physics » Direct detection of neutralinos Neutralino dark matter in the Neutrinos: (hot dark matter) constrained by structure formation. MSSM Supergravity models Axions: with a mass of eV. Neutralino dark matter in the NMSSM Weakly Interacting Massive Particles: They can be present in the right amount to explain the dark matter. Summary Lightest Supersymmetric Particle: stable in Supersymmetric theories with R-parity. The LSP can be the lightest Neutralino, , which is a WIMP . ❯✵❱ Other interesting possibilities are axino or gravitino dark matter. SIMPs, CHAMPs, SIDM, WIMPzillas, Scalar DM, KK, Light DM... 24.5.2005 Seoul-The dark side of the Universe - p. 7/55

  2. Direct detection of neutralinos If Neutralinos constitute the bulk of dark matter they would cluster with ordinary stars in » Outline galactic halos, raising the hope of their direct detection on Earth experiments. Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters Direct detection of neutralinos would be possible through their elastic scattering with nuclei from CMB inside a detector. » Usual Suspects » Direct detection of neutralinos Neutralino dark matter in the MSSM The recoiling energy can be detected by Supergravity models Ionization on solids Neutralino dark matter in the Scattered NMSSM WIMP Ionization in scintillators (measured by emission of Summary photons) Recoiling nucleus Increase in the temperature (measured by the released phonons) Target crystal 24.5.2005 Seoul-The dark side of the Universe - p. 8/55

  3. Direct detection of neutralinos If Neutralinos constitute the bulk of dark matter they would cluster with ordinary stars in » Outline galactic halos, raising the hope of their direct detection on Earth experiments. Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters Direct detection of neutralinos would be possible through their elastic scattering with nuclei from CMB inside a detector. » Usual Suspects » Direct detection of neutralinos Sensitivity for WIMP detection (Spin-independent cross section) Neutralino dark matter in the MSSM Many experiments around the world Supergravity models Neutralino dark matter in the NMSSM Cresst, Heidelberg-Moscow, IGEX, UKDMC(NAI), DAMA, CDMS, Summary ZEPLIN, EDELWEISS, ... 24.5.2005 Seoul-The dark side of the Universe - p. 8/55

  4. Direct detection of neutralinos If Neutralinos constitute the bulk of dark matter they would cluster with ordinary stars in » Outline galactic halos, raising the hope of their direct detection on Earth experiments. Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters Direct detection of neutralinos would be possible through their elastic scattering with nuclei from CMB inside a detector. » Usual Suspects » Direct detection of neutralinos Sensitivity for WIMP detection (Spin-independent cross section) Neutralino dark matter in the MSSM Many experiments around the world Supergravity models Neutralino dark matter in the NMSSM Cresst, Heidelberg-Moscow, IGEX, UKDMC(NAI), DAMA, CDMS, Summary ZEPLIN, EDELWEISS, ... With increasing sensitivities and projected improvements ZEPLIN II and III, GENIUS, CDMSII, GEDEON, ... 24.5.2005 Seoul-The dark side of the Universe - p. 8/55

  5. Direct detection of neutralinos If Neutralinos constitute the bulk of dark matter they would cluster with ordinary stars in » Outline galactic halos, raising the hope of their direct detection on Earth experiments. Introduction » Motivation for Dark Matter » Motivation for Dark Matter » Cosmological parameters Direct detection of neutralinos would be possible through their elastic scattering with nuclei from CMB inside a detector. » Usual Suspects » Direct detection of neutralinos Sensitivity for WIMP detection (Spin-independent cross section) Neutralino dark matter in the MSSM Many experiments around the world Supergravity models Neutralino dark matter in the NMSSM Cresst, Heidelberg-Moscow, IGEX, UKDMC(NAI), DAMA, CDMS, Summary ZEPLIN, EDELWEISS, ... With increasing sensitivities and projected improvements ZEPLIN II and III, GENIUS, CDMSII, GEDEON, ... Could neutralinos be detected in the (near) future? How large can their detection cross section be? 24.5.2005 Seoul-The dark side of the Universe - p. 8/55

  6. » Outline Introduction Neutralino dark matter in the MSSM » The Lightest Neutralino » Neutralino-nucleon cross Neutralino dark matter in the MSSM section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 9/55

  7. t ❱ ☛ ❅ ❥ ❦ ✱ ❅ ❅ ❥ ✆ ❅ ✱ ❅ ✱ ❯ ✒ ☞ ✐ ❤ ❡ ❢ ❣ ❤ ❡ ❢ ❡ ✐ ☞ ❣ ❢ ✱ ❧ ❤ ❅✇ q ✉ t q r s qr ♣ ③ ♦ ♦ ♣ ② ❥ ♠♥♦ ❦ ✒ ❅ ❥ ❦ t q ✉ t q r s qr ♣ ❣ ❤ ❣ ❢ ❡ ❢ ❡ ❞ ❝ ❤ ❣ ❡ ☞ ☞ ❅ ❢ ✆ ✱ ❳ ✒ ✱ ❤ ❝ ❡ ❢ ☛ ❝ ❣ ❝ ❢ ❣ ❤ ❤ ❡ ❣ ❞ The Lightest Neutralino » Outline Introduction ❯✲❲ ✱❨❳ ❯✲❩ The neutralinos in the MSSM are physical superpositions of the bino and wino ( ) ✱❃❪ ✱❴❫ Neutralino dark matter in the ❯❭❬ ❯❭❬ and Higgsinos ( ). MSSM » The Lightest Neutralino » Neutralino-nucleon cross section ❝☎❞ » Supergravity scenarios ❝✄❞ ❝✄❞ » Experimental Constraints ❵❜❛ ❝✄❞ » Charge and Colour Breaking Constraints ❝✄❞ ❝✄❞ Supergravity models Neutralino dark matter in the The properties of the lightest neutralino, , are very dependent on its composition. NMSSM Summary ✱✈❪ ✱①❫ ❯✲❲ ❯✲❩ ❯✲❬ ❯✲❬ ❯✵❱ 24.5.2005 Seoul-The dark side of the Universe - p. 10/55

  8. ✇ ❺ ⑩ ⑤ ⑩ ✴ ✱ ❅ ✌ ❶ ✿ ❹ ❿ ⑩ ✿ ☛ ✿ ☛ ✱ ❅ ☛ ❥ ❅ ❅ ⑤ ⑥ ④ ④ ④ ④ Neutralino-nucleon cross section One can evaluate the spin-independent part of the cross-section and analyse the » Outline feasibility of their direct detection. Introduction Neutralino dark matter in the MSSM Squark-exchange: » The Lightest Neutralino ⑦⑨⑧ ⑦⑨⑧ ⑤✵⑥ » Neutralino-nucleon cross section » Supergravity scenarios ☛❴❷ ☛❼❻ ❽✵❾ » Experimental Constraints » Charge and Colour Breaking ❵❜❛ ✫✵❸ ❵❜➀ Constraints ❵❜❛ Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 11/55

  9. ❅ ✿ ✱ ✿ ☛ ✿ ✫ ☛ ❿ ☛ ❸ ➒ ❺ ❹ ☛ ➀ ✿ ❅ ❥ ✌ ➎ ➎ ❛ ➉ ➈ ✱ ➏ ❅ ❶ ✌ ➇ ➇ ➇ ➇ ✇ ❅ ❶ ❅ ✴ ❅ ❺ ❥ ❅ ❅ ❹ ❥ ☛ ✱ ☛ ❥ ❅ ❅✇ ✿ ✻ ❹ ❅✇ ➁ ➆ ✿ ✴ ✇ ➆ ✻ ➃ ➂ ➂ ➆ ❥ ❅ ➁ ➁ ➁ ❵ Neutralino-nucleon cross section One can evaluate the spin-independent part of the cross-section and analyse the » Outline feasibility of their direct detection. Introduction Neutralino dark matter in the MSSM Squark-exchange: » The Lightest Neutralino ➄⑨➅ ➄⑨➅ ➂✵➃ » Neutralino-nucleon cross section » Supergravity scenarios ☛❴❷ ☛❼❻ ❽✵❾ » Experimental Constraints » Charge and Colour Breaking ❵❜❛ ✫✵❸ ❵❜➀ Constraints ❵❜❛ Supergravity models Neutralino dark matter in the NMSSM Higgs-exchange: Summary ➋➍➌ ➋➍➌ ☛❙❷ ➈➊➉ ✒➔➓ ➋➑➐ This diagram is typically dominant and can be enhanced with Higgsino-like neutralinos (increase ) ✒➔➓ Light Higgses (decrease ) 24.5.2005 Seoul-The dark side of the Universe - p. 11/55

  10. ❪ ✕ ✿ ✆ ☛ ✐ ✐ ❻ ➟ ✕ ➤ ✑ ✿ ➙ ➟ ➙ ➢ ➙➟ ✕ ❾ ➞ ❽ ➟ ❪ ❫ ❻ ☛ ❬ ❫ ❬ ✆ ➩ ❾ ➙ ➤ ❞ ❝ ➤ ✧ ✝ ✝ ➩ ☛ ❾ ➙ ➤ ❾ ➙ ➡ ❽ ✕ ✎ ✝☞ ✧ ↔ ➣ ✑ ➙ ❻ ❻ ✕ ❻ ❝ ❀ ➝ ✏ ➙ ➞ ➙➟ ✑ ➙ ❻ ❻ ❅↕ Supergravity scenarios Working in the framework of SUGRA, several assumptions are made: » Outline Introduction The soft parameters are generated once SUSY is broken through gravitational Neutralino dark matter in the MSSM interactions. » The Lightest Neutralino » Neutralino-nucleon cross They are given at a high energy scale (e.g., the GUT scale ❝✄→ GeV) section » Supergravity scenarios ✔✖➙➛ ❽✵❾➜ » Experimental Constraints » Charge and Colour Breaking ✿✄➠ Constraints ➥➦➠ ❤✵➧ Supergravity models Neutralino dark matter in the With these inputs, the RGEs are used to evaluate the low-energy supersymmetric NMSSM spectrum. Summary Radiative Electroweak Symmetry Breaking is imposed, and as a consequence the Higgsino mass parameter is determined by the minimization of the Higgs effective potential. This implies ☛❃➨ ☛❃➨ ☛❜➩ 24.5.2005 Seoul-The dark side of the Universe - p. 12/55

  11. ✿ ✿ ➫ ❅ ➭ ✝ ☞ ✢ ➭ ✝➲ ☞ ✿ ➭ ✠ ✪ Experimental Constraints For consistency with experimental results, several constraints have to be imposed on the » Outline SUSY spectrum and low energy observables. Introduction Neutralino dark matter in the GeV, Supersymmetric spectrum (LEP , Tevatron) : MSSM ❵❜❛ » The Lightest Neutralino GeV ❵❜➯ » Neutralino-nucleon cross GeV, section ❵❜➳ . . . » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 13/55

  12. ✞ ✻ ➼ ❤ ✌ ➠ ■ ✝ ✿ ✫ ✝ ✝ ➭ Experimental Constraints For consistency with experimental results, several constraints have to be imposed on the » Outline SUSY spectrum and low energy observables. Introduction Neutralino dark matter in the Supersymmetric spectrum (LEP , Tevatron) : MSSM » The Lightest Neutralino » Neutralino-nucleon cross section GeV Higgs Mass (LEP2) : » Supergravity scenarios ☛➻➺ (dependent on ➵✦➸ in the MSSM) » Experimental Constraints » Charge and Colour Breaking Constraints Supergravity models Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 13/55

  13. ✱ ✝ ✿ ✻ ➭ ✝ ✝ ✫ ✞ ✌ ❅ ✱ ■ ❅ ❊ ➠ ✌ ❤ ✌ ✱ ❅ ➚➪ ❅ ❊ ❅ ➽ ❉ ✇ ➾ ❀ ➾ ✌ ✹ ➴ ✹ ✱ ❅ ➼ Experimental Constraints For consistency with experimental results, several constraints have to be imposed on the » Outline SUSY spectrum and low energy observables. Introduction Neutralino dark matter in the Supersymmetric spectrum (LEP , Tevatron) : MSSM » The Lightest Neutralino » Neutralino-nucleon cross section GeV Higgs Mass (LEP2) : » Supergravity scenarios ☛➻➺ (dependent on ➵✦➸ in the MSSM) » Experimental Constraints » Charge and Colour Breaking Constraints Muon anomalous magnetic moment (Davier et al.; Hagiwara et al.; Trocóniz, Ynduráin ’04) : ➚➶➘➹ ❉➔➽ (from data) (Bennett et al. ’04) Supergravity models Neutralino dark matter in the ~ ~ 0 ν µ χ NMSSM Summary µ µ µ µ ~ − ~ χ µ γ γ 24.5.2005 Seoul-The dark side of the Universe - p. 13/55

  14. ➮ ❊ ✱ ■ ❅ ✌ ➠ ✌ ❤ ➼ ❡➱ ✱ ✫ ❅ ❅ ✝ ✱ ✌ ❅ ✱ ➾ ❀ ➚➪ ❅ ➾ ✇ ❉ ➽ ✘ ✞ ❊ ✝ ✽ ➷➬ ✘ ✇ ✌ ☞ ✝ ✧ ✾ ✇ ✌ ☞ ✝ ✫ ✞ ✌ ✹ ➴ ✹ ✿ ✻ ➭ ✝ ✝ ❅ Experimental Constraints For consistency with experimental results, several constraints have to be imposed on the » Outline SUSY spectrum and low energy observables. Introduction Neutralino dark matter in the Supersymmetric spectrum (LEP , Tevatron) : MSSM » The Lightest Neutralino » Neutralino-nucleon cross section GeV Higgs Mass (LEP2) : » Supergravity scenarios ☛➻➺ (dependent on ➵✦➸ in the MSSM) » Experimental Constraints » Charge and Colour Breaking Constraints Muon anomalous magnetic moment (Davier et al.; Hagiwara et al.; Trocóniz, Ynduráin ’04) : ➚➶➘➹ ❉➔➽ (from data) (Bennett et al. ’04) Supergravity models Neutralino dark matter in the NMSSM : (CLEO, BELLE) Summary ~ − ~ 0 χ χ ~ , g ~ ~ b u s b s d γ γ 24.5.2005 Seoul-The dark side of the Universe - p. 13/55

  15. ➾ ✱ ➚➪ ❀ ➾ ✱ ❅ ✌ ❅ ✇ ❊ ❅ ➷➬ ✽ ➮ ➼ ✘ ✇ ✌ ✱ ☞ ✌ ✹ ➴ ✹ ✌ ❅ ❉ ✌ ✱ ❅ ❊ ❅ ➽ ❤ ➠ ✝ ✘ ✇ ❲ ✐ ➴ ✐ ✌ ✧ ❡➱ ✞ ✳ ✝ ☞ ✌ ❉ ✌ ✧ ☞ ✫ ✾ ■ ✘ ✫ ✝ ✞ ✝ ✝ ➭ ✻ ✿ ✞ ✝ ✝ Experimental Constraints For consistency with experimental results, several constraints have to be imposed on the » Outline SUSY spectrum and low energy observables. Introduction Neutralino dark matter in the Supersymmetric spectrum (LEP , Tevatron) : MSSM » The Lightest Neutralino » Neutralino-nucleon cross section GeV Higgs Mass (LEP2) : » Supergravity scenarios ☛➻➺ (dependent on ➵✦➸ in the MSSM) » Experimental Constraints » Charge and Colour Breaking Constraints Muon anomalous magnetic moment (Davier et al.; Hagiwara et al.; Trocóniz, Ynduráin ’04) : ➚➶➘➹ ❉➔➽ (from data) (Bennett et al. ’04) Supergravity models Neutralino dark matter in the NMSSM : (CLEO, BELLE) Summary ✱❴✃ B( ) (CDF , D0) 24.5.2005 Seoul-The dark side of the Universe - p. 13/55

  16. ☞ ✝ ✌ ☞ ✝ ✧ ✞ ✌ ✹ ➴ ✹ ✱ ✘ ❅ ✌ ✱ ❅ ❊ ❅ ➽ ❉ ✇ ➾ ✇ ➷➬ ➚➪ ❉ ✧ ✘ ✝ ✌ ✐ ➴ ✐ ☞ ❲ ✌ ✇ ✽ ✌ ☞ ✝ ✝ ✞ ✫ ✘ ✾ ❡➱ ➮ ✘ ❀ ✳ ✘ ✻ ✿ ✞ ✢ ☞ ✞ ☞ ✳ ✫ � ➾ ✱ ❅ ✡ ☛ ✘ ☞ ✞ ✝ ✧ ✳ ➭ ✝ ✝ ➼ ✱ ❅ ✌ ✱ ❅ ❊ ❅ � ✱ ❅ ❤ ✫ ✌ ➠ ✡ ☛ ■ ✘ ☞ ✝ ✞ ✞ Experimental Constraints For consistency with experimental results, several constraints have to be imposed on the » Outline SUSY spectrum and low energy observables. Introduction Neutralino dark matter in the Supersymmetric spectrum (LEP , Tevatron) : MSSM » The Lightest Neutralino » Neutralino-nucleon cross section GeV Higgs Mass (LEP2) : » Supergravity scenarios ☛➻➺ (dependent on ➵✦➸ in the MSSM) » Experimental Constraints » Charge and Colour Breaking Constraints Muon anomalous magnetic moment (Davier et al.; Hagiwara et al.; Trocóniz, Ynduráin ’04) : ➚➶➘➹ ❉➔➽ (from data) (Bennett et al. ’04) Supergravity models Neutralino dark matter in the NMSSM : (CLEO, BELLE) Summary ✱❴✃ B( ) (CDF , D0) Astrophysical Constraints For the neutralino to be a solution to the problem of dark matter, its relic density has to be in agreement with observations Relic density: ( ) ❵❜❛ ❵❜❛ 24.5.2005 Seoul-The dark side of the Universe - p. 13/55

  17. Charge and Colour Breaking Constraints The presence of scalar £elds with Colour and Electric Charge in SUSY theories may » Outline induce the appearance of dangerous charge and colour breaking minima (CCB) deeper Introduction than the realistic minimum. Neutralino dark matter in the MSSM V » The Lightest Neutralino » Neutralino-nucleon cross section » Supergravity scenarios » Experimental Constraints » Charge and Colour Breaking φ Constraints Supergravity models S.M. MINIMUM Neutralino dark matter in the <H > u,d NMSSM Summary CCB MINIMUM <u,e...> Also the (tree level) potential can become Unbounded from Below (UFB) along particular directions in the £eld space. Avoiding these cases leads to constraints on the parameter space, among which the UFB constraints are the most important ones. 24.5.2005 Seoul-The dark side of the Universe - p. 14/55

  18. » Outline Introduction Neutralino dark matter in the MSSM Supergravity models Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 15/55

  19. ➥ ✿ ❝ mSUGRA In mSUGRA, where soft terms are taken to be universal, , , , the parameter space » Outline is very constrained: Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 16/55

  20. ✿ ➥ ❝ mSUGRA In mSUGRA, where soft terms are taken to be universal, , , , the parameter space » Outline is very constrained: Introduction Neutralino dark matter in the MSSM Experimentally accepted Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 16/55

  21. ✢ � ❝ ✿ ➥ ☞ ✞ ✝ ✘ ✱ ❅ ✡ ☛ ✘ ☞ ✞ mSUGRA In mSUGRA, where soft terms are taken to be universal, , , , the parameter space » Outline is very constrained: Introduction Neutralino dark matter in the MSSM Experimentally accepted Supergravity models » mSUGRA » mSUGRA ❵❜❛ » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 16/55

  22. ❰ ✫ ✘ � ✱ ❅ ✡ ☛ ✘ ☞ ✞ ✢ ☞ ✞ ☞ ✳ ✘ ☞ � ✱ ❅ ✡ ☛ ✘ ☞ ✞ ✝ ✧ ✳ ☞ ✝ ❮ ✝ ✞ ➥ ✿ ❝ mSUGRA In mSUGRA, where soft terms are taken to be universal, , , , the parameter space » Outline is very constrained: Introduction Neutralino dark matter in the MSSM Experimentally accepted Supergravity models » mSUGRA » mSUGRA ❵❜❛ » Increasing the detection cross section » Non-universal scalar masses * » Non-universal scalar masses ❵❜❛ » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary ❐✖❒ 24.5.2005 Seoul-The dark side of the Universe - p. 16/55

  23. ❰ ✫ ✘ � ✱ ❅ ✡ ☛ ✘ ☞ ✞ ✢ ☞ ✞ ☞ ✳ ✘ ☞ � ✱ ❅ ✡ ☛ ✘ ☞ ✞ ✝ ✧ ✳ ☞ ✝ ❮ ✞ ✝ ➥ ✿ ❝ mSUGRA In mSUGRA, where soft terms are taken to be universal, , , , the parameter space » Outline is very constrained: Introduction Neutralino dark matter in the MSSM Experimentally accepted Supergravity models » mSUGRA » mSUGRA ❵❜❛ » Increasing the detection cross section » Non-universal scalar masses * » Non-universal scalar masses ❵❜❛ » Correlation between... » Non-universal scalar and gaugino masses Disfavoured by UFB constraints » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary ❐✖❒ 24.5.2005 Seoul-The dark side of the Universe - p. 16/55

  24. ❰ ☞ ❅ ✱ � ✘ ✫ ✳ ✞ ☛ ☞ ✢ ✞ ☞ ✘ ☛ ❅ ✡ ✘ � ✘ ❮ ✝ ☞ ➥ ➥ ☞ ✧ ➩ ☞ ❾ ➙ ➤ ✳ ✧ ✝ ✞ ✱ ✡ ✘ ✝ ✞ ☞ ❝ ➥ ✿ mSUGRA In mSUGRA, where soft terms are taken to be universal, , , , the parameter space » Outline is very constrained: Introduction Neutralino dark matter in the MSSM Experimentally accepted Supergravity models » mSUGRA » mSUGRA ❵❜❛ » Increasing the detection cross section » Non-universal scalar masses * » Non-universal scalar masses ❵❜❛ » Correlation between... » Non-universal scalar and gaugino masses Disfavoured by UFB constraints » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos is disfavoured for any » Summary (MSSM) Larger values can also be Neutralino dark matter in the forbidden for certain NMSSM Summary ❐✖❒ 24.5.2005 Seoul-The dark side of the Universe - p. 16/55

  25. ❶ ✌ ❅ ✱ ✴ ➩ ❾ ➙ ➤ mSUGRA Larger values of lead to an increase of » Outline ❵❜❛ Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 17/55

  26. Ï ❮ ✝ ☞ ❶ ✌ ❅ ✱ ✴ ➩ ❾ ➙ ➤ mSUGRA Larger values of lead to an increase of » Outline ❵❜❛ Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary ❐✖❒ 24.5.2005 Seoul-The dark side of the Universe - p. 17/55

  27. ❀ ❝ Increasing the detection cross section Departures from the mSUGRA scenario can lead to an increase in the neutralino-nucleon » Outline cross section. Introduction Neutralino dark matter in the Intermediate scales MSSM (Gabrielli, Khalil, Muñoz, Torrente-Lujan ’00) Supergravity models » mSUGRA » mSUGRA Non-universal soft parameters » Increasing the detection cross section » Non-universal scalar masses Non-universal scalar masses ✿✄➠ » Non-universal scalar masses (Bottino, Donato, Fornengo, Scopel ’99; Arnowitt, Nath ’99; Accomando, Arnowitt, Dutta, Santoso ’00) » Correlation between... » Non-universal scalar and Non-universalities in the Higgs sector induce the largest effects. gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and Non-universal gaugino masses gaugino masses » Very light neutralinos (Corsetti, Nath ’00; D.G.C., Khalil, Muñoz ’01) » Summary (MSSM) General case, with non-universal scalar and gauginos Neutralino dark matter in the NMSSM (D.G.C, C. Muñoz ’04; Baek, D.G.C., Kim, Ko, Muñoz ’05) Summary Neutralinos within the reach of detectors in the near future can appear with a wide range of masses. 24.5.2005 Seoul-The dark side of the Universe - p. 18/55

  28. ☛ ✿ Ð ❦ ✝ ✽ ✱ ☛ ✆ ✾ ❪ ❫ ✿ ❝ ☛ Ð ❅ ❳ ❅ ✝ ✿ ❪ ✾ ✿ Ð ❦ ✽ ✿ ✱ ☛ ✿ ✆ ❫ ➨ ☛ ☛ Ð ✿ ❩ ❅ ✌ ❶ ❩ ❩ ✡ Ò ✴ Ò � ❵ ❛ ✱ ❅ ✱ ❞ ❞ ☛ ✐ ❶ ✌ ❅ ✱ ☛ ✴ ✿ ❫ ❅ ☛ ❝ ✆ Non-universal scalar masses Non-universal scalar masses can help increasing . » Outline ❵❜❛ Introduction The most important effect is due to non-universalities in the Higgs masses at the GUT Neutralino dark matter in the scale, which can be parametrized by and : MSSM Supergravity models ☛✈➨ » mSUGRA » mSUGRA » Increasing the detection cross section RGES for the Higgs parameters » Non-universal scalar masses » Non-universal scalar masses » Correlation between... δ > 0 2 » Non-universal scalar and ☛❃Ñ ☛❃➨ ☛❃➨ 2 m 2 0 gaugino masses m H d » Non-universal scalar and gaugino masses ☛❃➨ » Non-universal scalar and δ < 0 1 gaugino masses » Very light neutralinos 2 m » Summary (MSSM) H u Neutralino dark matter in the NMSSM M EW M GUT Summary The Higgsino components of the lightest neutralino increase and the Higgs masses decreaase, thus there is an increase in . ❵❜❛ Also, new annihilation channels appear (with e.g., , , in the £nal products) and decreases. 24.5.2005 Seoul-The dark side of the Universe - p. 19/55

  29. Ô ➙ ❾ ➙ ➤ ➲ ✢ ✆ ➩ ❾ ➤ ✆ ✱ ☛ ✿ ✧ ✆ ❫ ✿ ❳ ➩ ✢ ❪ ✌ ➢ ↕ ✌ ☞ ✝ ✢ ✘ ❶ ❅ ➲ ✱ ❛ ❵ ✴ ➩ ❾ ➙ ➤ ✆ ☞ ✿ ❫ ✿ ☛ ✱ ❳ ✿ ✆ ❪ ✧ ✿ ☛ ✱ ✿ ✆ Non-universal scalar masses ☛Ó➨ ☛Ó➨ ☛Ó➨ ☛Ó➨ » Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary Although in principle points ful£lling all the experimental constraints and with a consistent value for the relic density can be found within the reach of dark matter detectors, even for moderate . . . 24.5.2005 Seoul-The dark side of the Universe - p. 20/55

  30. Ô ❾ ➩ ❾ ➙ ➤ ➲ ✢ ✆ ➩ ➙ ✢ ➤ ✱ ☛ ✿ ✧ ✆ ❫ ✿ ✆ ➲ ✆ ✌ ➢ ❉ ✌ ☞ ✝ ✢ ✘ ❶ ❅ ❲ ✱ ❛ ❵ ✴ ✌ ✐ ➴ ✐ ☞ ❳ ❪ ✿ ❪ ✆ ✿ ☛ ✱ ❳ ❫ ✆ ✧ ✿ ☛ ✱ ✿ ✿ Non-universal scalar masses ☛Ó➨ ☛Ó➨ ☛Ó➨ ☛Ó➨ » Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM (Baek, D.G.C., Kim, Ko, Muñoz ’05) Summary ✱❴✃ . . . the recent experimental constraint on B( ) rules out most of those regions. 24.5.2005 Seoul-The dark side of the Universe - p. 20/55

  31. ✿ ✆ ❪ ✆ ✿ ☛ ✱ ❳ ✿ ✧ ❫ ✧ ✿ ✿ ☛ ✱ ✿ ✱ ❪ ✆ ☞ ❳ ✿ ☛ ✆ ❫ ➲ ➩ ❾ ➙ ➤ ✌ ✐ ➴ ✐ ❲ ☞ ✆ ➤ ➩ ❾ ➙ ➤ ☞ ➲ ✆ ➩ ❾ ➙ Non-universal scalar masses ☛Ó➨ ☛Ó➨ ☛Ó➨ ☛Ó➨ » Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM (Baek, D.G.C., Kim, Ko, Muñoz ’05) Summary ✱❴✃ . . . the recent experimental constraint on B( ) rules out most of those regions. Especially in the large regime, where neutralinos could escape detection in some of the projected experiments. 24.5.2005 Seoul-The dark side of the Universe - p. 20/55

  32. ✇ ✾ ✿ ↕ ➩ ❾ ➙ ➤ ✌ ❶ ✐ ➴ ✐ ➤ ❲ ✽ ➷ Ñ ✐ ❡ ❅ ✴ ✱ ✌ ✐ ➴ ✐ ❲ ➥ ✌ ☛ ✣ ❵ ☛ ✿ ✣ ➙ ➮ ❛ ✧ ☛ ✱ ❳ ✿ ❫ ✆ ✿ ✆ ☛ ✱ ✴ ✱ ❅ ✌ ❶ ✿ ❪ ❵ ✐ Ñ ✿ ➩ ❾ ✌ ✿ ✐ ❲ ➴ Correlation between and B( ) Õ×Ö ✱❙✃ From the leading contribution to the B( ) process, the chargino mediated » Outline transition one obtains the qualitative expression Introduction Neutralino dark matter in the MSSM ✱①✃ Supergravity models » mSUGRA ✱❙✃ Both observables, B( ) and , increase for large and small . » mSUGRA » Increasing the detection cross section ☛Ó➨ ☛Ó➨ » Non-universal scalar masses » Non-universal scalar masses » Correlation between... Points with larger are typically excluded. ❵❜❛ » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 21/55

  33. ✣ ❾ ➥ ✐ ✇ Ñ ✿ ↕ ➩ ➙ ✿ ➤ ✾ ✌ ✐ ➴ ✐ ✿ ✣ ☛ ✽ ❾ ❶ ✌ ❅ ✱ ❛ ❵ ✴ ✌ ❵ ✐ ➴ ✐ ➩ ❲ ✿ ☛ Ñ ❲ ➷ ➤ ❅ ✆ ✧ ✿ ☛ ✱ ✴ ✱ ✌ ✿ ❶ ➥ ➭ ☞ ➥ ➭ ☞ ❫ ❳ ❪ ✱ ❡ ➮ ✌ ✐ ➴ ✐ ❲ ✿ ✆ ☛ ➙ Correlation between and B( ) Õ×Ö ✱❙✃ From the leading contribution to the B( ) process, the chargino mediated » Outline transition one obtains the qualitative expression Introduction Neutralino dark matter in the MSSM ✱①✃ Supergravity models » mSUGRA ✱❙✃ Both observables, B( ) and , increase for large and small . » mSUGRA » Increasing the detection cross section ☛Ó➨ ☛Ó➨ » Non-universal scalar masses » Non-universal scalar masses » Correlation between... Points with larger are typically excluded. ❵❜❛ » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses The correlation can be diluted if the term in » Non-universal scalar and parenthesis is reduced by gaugino masses » Very light neutralinos - Decreasing the stop mixing (e.g., with ) » Summary (MSSM) - Decreasing the Higgsino mixing (e.g., with Neutralino dark matter in the non-universal Higgses) NMSSM - Increasing the stop mass (e.g., with ) Summary 24.5.2005 Seoul-The dark side of the Universe - p. 21/55

  34. ✐ ✇ ☛ ✣ ❵ ☛ ✿ ✣ ➥ ✐ Ñ ❲ ✿ ↕ ➩ ❾ ➙ ➤ ✾ ✌ ❳ ✱ ➴ ✌ ✿ ❪ ➩ ❾ ➙ ➤ ✆ ❶ ❅ ☛ ✱ ❛ ❵ ✴ ✿ ✌ ✐ ➴ ✐ ✐ ✿ ➥ ✴ ✱ ❅ ✌ ❶ ➥ ➭ ☞ ➭ ☛ ☞ ✴ ❵ ❛ ✱ ❅ ✌ ❶ ✱ ✿ ✿ ✧ ❲ ✽ ➷ ❫ ❡ ➮ ✌ ✐ ➴ ✐ ❲ ✆ Ñ Correlation between and B( ) Õ×Ö ✱❙✃ From the leading contribution to the B( ) process, the chargino mediated » Outline transition one obtains the qualitative expression Introduction Neutralino dark matter in the MSSM ✱①✃ Supergravity models » mSUGRA ✱❙✃ Both observables, B( ) and , increase for large and small . » mSUGRA » Increasing the detection cross section ☛Ó➨ ☛Ó➨ » Non-universal scalar masses » Non-universal scalar masses » Correlation between... Points with larger are typically excluded. ❵❜❛ » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses The correlation can be diluted if the term in » Non-universal scalar and parenthesis is reduced by gaugino masses » Very light neutralinos - Decreasing the stop mixing (e.g., with ) » Summary (MSSM) - Decreasing the Higgsino mixing (e.g., with Neutralino dark matter in the non-universal Higgses) NMSSM - Increasing the stop mass (e.g., with ) Summary As a consequence, points with large are still attainable. 24.5.2005 Seoul-The dark side of the Universe - p. 21/55

  35. ❝ ❝ ☛ ✴ ❵ ❛ ✱ ❅ ✌ ❶ ❅ ❝ ✆ ❝ ❺ ☛ ✆ ❝ ✽ ✝ Ð ✾ ✒ ❝ ✐ ❫ ✿ ☞ ✘ ✒ ❺ Ð ✒ ❦ ✆ ✾ ✒ ❺ Ð ❦ ✝ ✽ ❝ Non-universal scalar and gaugino masses Non-universal gaugino masses can also induce an increase of . » Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section ☛Ó➨ Decreasing ( ) leads to an increase in the value of through the » Non-universal scalar masses » Non-universal scalar masses corresponding RGEs. Thus, the parameter is reduced and the cross section increases. » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 22/55

  36. ✽ Ð ✆ ✒ ❝ ✾ ☛ ❺ ❦ ✆ ✝ ✽ ❝ ✆ ☛ ❝ ❝ ✝ ✆ ✿ ✐ ☞ ✘ ✒ ❺ Ð ✒ ❦ ❝ ❪ ✾ ✒ ❺ Ð ❝ ❅ ❫ ☛ ✿ ☛ ➨ ❫ ✆ ✿ ✱ ❅ ✽ ✝ ❦ Ð ☛ ✾ ✾ Ð ❝ ❦ ❶ ✌ ❅ ✱ ❛ ❵ ✴ ✿ ☛ ✱ ✽ ✝ ✿ Non-universal scalar and gaugino masses Non-universal gaugino masses can also induce an increase of . » Outline Introduction Neutralino dark matter in the MSSM Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross section ☛Ó➨ Decreasing ( ) leads to an increase in the value of through the » Non-universal scalar masses » Non-universal scalar masses corresponding RGEs. Thus, the parameter is reduced and the cross section increases. » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and In the general case, a combination of these and scalar non-universalities gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos ☛✈➨ » Summary (MSSM) Neutralino dark matter in the NMSSM Summary provides more ¤exibility in the neutralino sector. Neutralinos with a wide range of masses can be obtained within the reach of dark matter detectors. 24.5.2005 Seoul-The dark side of the Universe - p. 22/55

  37. ❝ ✜ ✜ ❅ ✐ ✒ ✴ ✱ ❅ ✌ ❶ � ❵ ❛ ✱ ❅ ✐ ❲ ✐ ➴ ✐ ✌ ✴ ✱ ❅ ✌ ❶ ✒ Non-universal scalar and gaugino masses In the general case, non-universalities in scalars and gauginos provide more ¤exibility in » Outline the neutralino sector. Neutralinos with a wide range of masses can be obtained within the Introduction reach of dark matter detectors. Neutralino dark matter in the MSSM Decrease Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross The parameter decreases through the in¤uence of on the RGEs of the Higgs section parameters » Non-universal scalar masses » Non-universal scalar masses » Correlation between... Heavier neutralinos are found with a larger Higgsino composition. » Non-universal scalar and gaugino masses » Non-universal scalar and The Higgs-exchanging interaction becomes more important and there is a slight gaugino masses increase of . There is also a reduction of . » Non-universal scalar and ❵❜❛ gaugino masses » Very light neutralinos ✱❙✃ Also, due to the decrease in , and the reduction in the stop mixing, B( ) » Summary (MSSM) slightly decreases. As a consequence, larger are obtained. ❵❜❛ Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 23/55

  38. ✱ ✒ ✆ ✢ ➲ ➤ ➙ ❾ ➩ ✆ ➲ ☞ ❝ ❅ ✆ ✇ ❝ ❾ ☛ ➓ ✒ ✿ ❪ ✆ ☞ ❳ ✿ ❫ ✆ ✧ ✿ ☛ ➩ ➙ ➤ ❅ ✜ ✒ ✜ Non-universal scalar and gaugino masses In the general case, non-universalities in scalars and gauginos provide more ¤exibility in » Outline the neutralino sector. Neutralinos with a wide range of masses can be obtained within the Introduction reach of dark matter detectors. Neutralino dark matter in the MSSM Decrease Supergravity models ☛Ó➨ ☛Ó➨ » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 23/55

  39. ✱ ✒ ✆ ✢ ➲ ➤ ➙ ❾ ➩ ✆ ➲ ☞ ❝ ❅ ✆ ✇ ❝ ❾ ☛ ➓ ✒ ✿ ❪ ✆ ☞ ❳ ✿ ❫ ✆ ✧ ✿ ☛ ➩ ➙ ➤ ❅ ✜ ✒ ✜ Non-universal scalar and gaugino masses In the general case, non-universalities in scalars and gauginos provide more ¤exibility in » Outline the neutralino sector. Neutralinos with a wide range of masses can be obtained within the Introduction reach of dark matter detectors. Neutralino dark matter in the MSSM Decrease Supergravity models ☛Ó➨ ☛Ó➨ » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 23/55

  40. ➴ ✐ ✜ ❅ ✐ ✐ ❲ ✐ ✌ ✜ ✴ ❵ ❛ ✱ ❅ ✌ ❶ ✒ Non-universal scalar and gaugino masses In the general case, non-universalities in scalars and gauginos provide more ¤exibility in » Outline the neutralino sector. Neutralinos with a wide range of masses can be obtained within the Introduction reach of dark matter detectors. Neutralino dark matter in the MSSM Increase Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross The parameter increases section » Non-universal scalar masses Lighter neutralinos are obtained, which have a larger Bino composition. » Non-universal scalar masses » Correlation between... » Non-universal scalar and In this case, due to the increase in the parameter, and in the the stop mixing, gaugino masses » Non-universal scalar and ✱❙✃ B( ) increases, and smaller are obtained. gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 24/55

  41. ✱ ☛ ✆ ✢ ➲ ➤ ➙ ❾ ➩ ✆ ➲ ☞ ❝ ❅ ✆ ❅ ❝ ❾ ☛ ➓ ✒ ✿ ❪ ✆ ☞ ❳ ✿ ❫ ✆ ✧ ✿ ☛ ➩ ➙ ➤ ❅ ✜ ✒ ✜ Non-universal scalar and gaugino masses In the general case, non-universalities in scalars and gauginos provide more ¤exibility in » Outline the neutralino sector. Neutralinos with a wide range of masses can be obtained within the Introduction reach of dark matter detectors. Neutralino dark matter in the MSSM Increase Supergravity models ☛Ó➨ ☛Ó➨ » mSUGRA » mSUGRA » Increasing the detection cross section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 24/55

  42. ✐ ❝ ❝ ☛ ➓ ✒ ❳ � ✱ ❅ ➤ ➙ ❾ ➩ ✿ Ñ ✘ ✧ ☞ ☞ ❲ ✐ ➴ ✐ ✌ ❅ Very light neutralinos With very light (Bino-like) neutralinos can be obtained, which are » Outline compatible with experimental constraints. Introduction (Griest, Roszkowski ’92; Gabutti, Olechowski, Cooper, Pokorski, Stodolski ’96; Hooper, Plehn ’02) Neutralino dark matter in the MSSM Supergravity models Despite them having typically a too high relic density, a signi£cant reduction in can » mSUGRA ❵❜❛ » mSUGRA be obtained for large if the mass of the CP-odd Higgs is small ( GeV). » Increasing the detection cross section (Bottino, Fornengo, Scopel ’02; Bottino, Donato, Fornengo, Scopel ’03 ’04) » Non-universal scalar masses (Bélanger, Boudjema, Cottrant, Pukhov, Rosier-Lees ’03) » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and Although this can be achieved precisely with non-universalities in the Higgs masses, gaugino masses ✱❴✃ this entails a very large increase in B( ) and makes this possibility very » Non-universal scalar and gaugino masses constrained. » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 25/55

  43. ✱ ➲ ❾ ➤ ➙ ❾ ➩ ➙ ✿ ➤ ✱ ❅ ➭ ✢ ☞ ✧ ✐ ✴ ✆ ✱ ❅ ✌ ❶ ➭ ✝☞ ✌ ↕ ➢ Ô ➩ ➤ ➩ ❳ ❾ ❝ ☛ ✿ ✧ ✆ ❫ ✿ ❳ ☞ ✆ ❪ ✿ ✒ ➓ ☛ ✇ ✒ ❅ ➓ ☛ ❝ ❅ ❝ ➙ ✆ ➲ ☞ ❝ ❅ ✆ Very light neutralinos With very light (Bino-like) neutralinos can be obtained, which are » Outline compatible with experimental constraints. Introduction Neutralino dark matter in the MSSM Still, for moderate values of , neutralinos as light as GeV can be ❵❜❛ Supergravity models obtained with very large values for the detection cross section, . » mSUGRA ❵❜❛ » mSUGRA » Increasing the detection cross section ☛❃➨ ☛❃➨ » Non-universal scalar masses » Non-universal scalar masses » Correlation between... » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Non-universal scalar and gaugino masses » Very light neutralinos » Summary (MSSM) Neutralino dark matter in the NMSSM Summary 24.5.2005 Seoul-The dark side of the Universe - p. 25/55

  44. ✴ ✐ ➴ ✐ ✌ ✱ ❅ ✌ ❶ ✴ ✱ ❅ ✌ ❶ ✴ ✱ ❅ ✌ ☞ ☞ ✫ ✘ ❅ ✱ ❲ ❛ ❵ ✿ ✘ ☞ ✢ ❶ Summary (MSSM) Supersymmetric theories provide a natural dark matter candidate in terms of the » Outline Lightest SUSY particle. Introduction Neutralino dark matter in the The impressive experimental efforts in dark matter detection, in particular of WIMPS MSSM motivate the theoretical analysis of the theoretical predictions for neutralino detection Supergravity models » mSUGRA » mSUGRA » Increasing the detection cross MSSM section » Non-universal scalar masses » Non-universal scalar masses » Correlation between... Experimental and astrophysical constraints play a leading role in restricting the parameter » Non-universal scalar and ✱❙✃ space. In particular, the recent constraint on B( ) typically rules out regions gaugino masses » Non-universal scalar and with larger . ❵❜❛ gaugino masses » Non-universal scalar and gaugino masses Departures from the mSUGRA case, allowing intermediate initial scales and/or » Very light neutralinos non-universal soft parameters can induce an increase of . » Summary (MSSM) ❵❜❛ Neutralino dark matter in the NMSSM Non-universalities in the scalar and gaugino sectors allow for ¤exibility in the neutralino sector. Summary Points of the parameter space can be obtained, where the experimental constraints are satis£ed and is within the sensitivity of detectors in the near future for a wide range ❵❜❛ of neutralino masses ( GeV). 24.5.2005 Seoul-The dark side of the Universe - p. 26/55

  45. » Outline Introduction Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 27/55

  46. ß ✾ ➚➪ ❝ ❳ Þ ✽ ✐ Û ➶ ❋ ➸ ✽ ✐ ☛ ❬ ❬ ➚ ✾ ✆ ❬ ➒ ✆ ã ã à ☛ ❅ ❩ ❬ ß ➒ ✆ ✾ ✐ ✽ ✐ ❅ ✾ ✐ ✽ ❩ ✐ ✐ Motivation The Next-to-Minimal Supersymmetric Standard Model constitutes a very well motivated » Outline extension of the MSSM. Introduction Neutralino dark matter in the Offers an elegant solution to the -problem of the MSSM MSSM Supergravity models The -term in the MSSM, present in the superpotential faces a naturaleness problem: Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross Whereas a natural value for is , minimisation of the scalar potential ØÙ✦Ú section implies » Enhancing the cross section » Constraints on the parameter space ❝ÝÜ » Case(i) » Masses and compositions » Cross section » Overview In the NMSSM » Variations in the gaugino masses ✐âá Summary 24.5.2005 Seoul-The dark side of the Universe - p. 28/55

  47. ✱ ❅ ✻ ✿ ✐ ✝ ✫ ☞ ✗ Motivation The Next-to-Minimal Supersymmetric Standard Model constitutes a very well motivated » Outline extension of the MSSM. Introduction Neutralino dark matter in the Offers an elegant solution to the -problem of the MSSM MSSM Supergravity models Less severe “Higgs-little £ne tuning” problem of the MSSM Neutralino dark matter in the NMSSM In the MSSM » Motivation » Overview of the NMSSM » Higgs Sector ✔✖✕ » The neutralino in the NMSSM » Neutralino-nucleon cross section and so far it has not been detected. » Enhancing the cross section » Constraints on the parameter space This problem is less severe in the NMSSM, since the upper bound for the Higgs » Case(i) mass is larger than in the MSSM. » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 28/55

  48. ✐ Motivation The Next-to-Minimal Supersymmetric Standard Model constitutes a very well motivated » Outline extension of the MSSM. Introduction Neutralino dark matter in the Offers an elegant solution to the -problem of the MSSM MSSM Supergravity models Less severe “Higgs-little £ne tuning” problem of the MSSM Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM Rich phenomenology » Higgs Sector » The neutralino in the NMSSM Very light Higgses and neutralinos are experimentally viable. » Neutralino-nucleon cross section » Enhancing the cross section Although the Higgs phenomenology has been thoroughly studied, there are only a » Constraints on the parameter few works on the implications for neutralino dark matter. space » Case(i) Flores, Olive, Thomas ’91 » Masses and compositions Bednyakov, Klapdor-Kleingrothaus ’98 » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 28/55

  49. ✐ Motivation The Next-to-Minimal Supersymmetric Standard Model constitutes a very well motivated » Outline extension of the MSSM. Introduction Neutralino dark matter in the Offers an elegant solution to the -problem of the MSSM MSSM Supergravity models Less severe “Higgs-little £ne tuning” problem of the MSSM Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM Rich phenomenology » Higgs Sector » The neutralino in the NMSSM Very light Higgses and neutralinos are experimentally viable. » Neutralino-nucleon cross section » Enhancing the cross section Although the Higgs phenomenology has been thoroughly studied, there are only a » Constraints on the parameter few works on the implications for neutralino dark matter. space » Case(i) Flores, Olive, Thomas ’91 » Masses and compositions Bednyakov, Klapdor-Kleingrothaus ’98 » Cross section » Overview » Variations in the gaugino Thorough analysis of the NMSSM parameter space, calculating the masses particle spectrum and the experimental constraints from LEP . Summary Implications for Neutralino-nucleon cross section. 24.5.2005 Seoul-The dark side of the Universe - p. 28/55

  50. ✾ ❅ ✹ ❬ ❅ ➒ ß ❬ ❬ ❦ ☛ ❦ ✝ ✢ ó ß ✒ í ð õ í ➤ ➟ ➞ ➜ ❩ ✆ ❫ î ❬ ☛ ❦ í ❪ ❬ ❅ ô ■ ✕ ✢ ❬ ❅ ❬ ☛ ❦ ✝ ó ➒ ß ✒ ❦ è ✞ ✏ ✞ ß ✽ ■ö ø ã ÷ ✆ ✿ ✷ ❬ ✷ ❦ ❬ ✷ ❦ ✿ ß ø ß ➛ ➙ å ä ✎ ✎ ❽ è ➙ ➟ ➤ ✕ç ✧ ß ❦ ✽é ➞ ➝ ➝ æ ✆ æ ➝ ➝ åæ ß ä ❻ æ ê ✾ ➤ ❾ ❽ ì ➙ ì ✕ë ➙ ✝ ➜ ❽ ì ì ➜ ê é ❳ ❾ ✕ Overview of the NMSSM In the NMSSM the £eld structure of the MSSM is modi£ed by the addition of a new » Outline super£eld , which is a singlet under the SM gauge group: Introduction Neutralino dark matter in the MSSM ❽✵❾ Supergravity models Neutralino dark matter in the NMSSM » Motivation This leads to the following new terms in the superpotential » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM î✖ï ñ✵ò » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space and in the Lagrangian » Case(i) » Masses and compositions » Cross section ➵✦õ ☛✈➨ ☛✈ù ➥✯ú ➥✭û » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 29/55

  51. ✾ ✆ ß ✒ ô õ ■ ■ö ã ÷ ✿ ✢ ✷ ❬ ø ✷ ❬ ✷ ❦ ✿ ó ✝ ø í ☛ í ❪ ❬ ❅ î ð ❦ ✹ ❦ ❬ ❅ ➒ ß ❬ ❅ ❬ ☛ ß ß ❫ ü ✆ ü ❅ à ❬ ✱ ☛ ✆ ☛ ✱ à ß ✆ ❡ ✽ ✆ ✐ ➒ ❅ ❬ ❦ ✝ ✽ ➒ ß ❬ ❅ ❬ ☛ ❦ ✢ ✾ ó ß ✒ ❦ è ✞ ✏ ✞ ❬ ❦ í ❽ ê é ❳ ❾ ✕ ✕ë ê æ ✽é ❻ ✎ ✎ è ➜ ➙ ➟ ✆ ➤ ✕ç ✧ ß ä ❦ ✆ æ ➝ ➝ ➝ æ ì ❩ ä ➜ ß ➞ ➙ ➟ ➤ ➛ ✕ å ➞ ➙ åæ ❾ ➜ ❽ ➤ ❽ ì ì ➙ ✝ ✾ ì ➝ Overview of the NMSSM In the NMSSM the £eld structure of the MSSM is modi£ed by the addition of a new » Outline super£eld , which is a singlet under the SM gauge group: Introduction Neutralino dark matter in the MSSM ❽✵❾ Supergravity models Neutralino dark matter in the NMSSM » Motivation This leads to the following new terms in the superpotential » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM î✖ï ñ✵ò » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space and in the Lagrangian » Case(i) » Masses and compositions » Cross section ➵✦õ ☛✈➨ ☛✈ù ➥✯ú ➥✭û » Overview » Variations in the gaugino masses Summary When Electroweak Symmetry Breaking occurs the Higgs £eld takes non-vanishing VEVs: 24.5.2005 Seoul-The dark side of the Universe - p. 29/55

  52. þ ✾ þ ☛ ❬ ❳ þ ❅ ❬ ✽ ✆ ✱ ❬ ❇ ß ß ❳ ✱ ➥ ✽ ✆ ✱ ý û ➥ ➥ ❳ þ ✾ ❅ ✱ ß ✒ ❅ ß ❦ þ ☛ ✱ ❬ ☛ ß ✾ ❦ þ ❅ ✱ ❬ ❅ ❅ ß ✆ ❅ ✱ ✡ ❡ ú û ✆ ❄ ❳ ó ❳ ❡ ❳ ➤ ➙ ❾ ➩ ❳ ✿ ✽ ❳ ☛ ✿ ❳ ➥ ú ❅ ✿ ❳ ➥ ➒ Higgs Sector » Outline The minimisation conditions for the scalar potential can be used to reexpress the soft Introduction breaking Higgs masses in terms of the rest of the parameters: Neutralino dark matter in the MSSM ☛✈➨ ☛✈➨ ☛✈ù Supergravity models And restrictions on the signs of , and appear Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector After rotating away the CP-odd would-be Goldstone boson we are left with £ve neutral Higgs » The neutralino in the NMSSM states, and two charged states. » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter CP-even and CP-odd states do not mix, since we made the assumption of no CP-violation space on the Higgs sectors. Thus the mass matrices are written in the corresponding basis: » Case(i) » Masses and compositions » Cross section » Overview CP-odd Higgs: » Variations in the gaugino masses CP-even Higgs: Summary The lightest Higgs has a singlet component: 24.5.2005 Seoul-The dark side of the Universe - p. 30/55

  53. t ❧ ✟ ✒ ✌ Õ ☛ ✡ ✠ ✡ ☛ ✟ ✡ ✠ ✟ ♠♥♦ ☛ ✟ ✠ ✡ ♣ ✠ ☛ ✡ ❅ ❥ ❦ ✱ ❯ ❅ ❅ ❥ ✆ ✱ ✄ ❩ ✱ Õ ✌ ☛ ✟ ✠ ✡ ✝ ☛ ✠ ☛ ♦ ❥ ❅ ✒ ❦ ❥ ❅✇ ② ♣ ♦ t ③ ♣ qr s r q t ✉ q ❦ q ✡ ☛ ✝ ✄ qr Õ ☛ ✟ ✠ ✟ s ✡ ✉ ✠ ✟ r Õ q ✂ ✱ t ❅ The neutralino in the NMSSM » Outline Introduction ✄✆☎ ✄✞✝ ✄✞✝ Neutralino dark matter in the MSSM ✄✆☞ ✄✞✝ Supergravity models ✄✞✝ ✄✞✝ ÿ ✁� Neutralino dark matter in the NMSSM ✄✞✝ » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter The lightest neutralino space » Case(i) » Masses and compositions ✱✈❪ ✱①❫ ❯❭❲ ❯❭❬ ❯❭❬ ❯✵❱ » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 31/55

  54. ☎ ✟ ✏ ☎ ✎ ✍ ☞ ✎ ✍ Õ Õ ♣ ✎ ✍ Õ ✍ ✟ ☛ ✟ ✠ ✡ ✝ ✄ ☛ ✟ ✠ ✟ ♦ ☞ ✎ ✍ ✑ ② ✍ ✒ ❅ ❥ ❦ t q ✉ t q r s qr ♣ ♠♥♦ ❧ ✱ ❯ ❥ ☛ ❅ ❥ ❦ ✱ ❅✇ ❅ ❅ ❥ ✆ ❅ ✱ ❱ ✟ Õ ❦ ❯ r Õ q ✂ ✱ t ✉ q t ❦ ❥ ❅ ✓ ß ☛ ✒ ♣ q ♦ ✓ ♣ qr s r q t ✉ q t ✟ ✠ ✡ ♣ ✡ ✠ ✡ ♦ ☛ ✡ ✠ ✟ ③ Õ ☛ ✟ ✠ ✡ ☛ ☛ ✡ ✠ ✡ ✝ ✄ qr Õ Õ ☛ ✟ ✠ ✟ s ✒ The neutralino in the NMSSM » Outline Introduction ✄✆☎ ✄✞✝ ✄✞✝ Neutralino dark matter in the MSSM ✄✆☞ ✄✞✝ Supergravity models ✄✞✝ ✄✞✝ ÿ ✁� Neutralino dark matter in the NMSSM ✄✞✝ » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter The lightest neutralino has now a singlino component space » Case(i) » Masses and compositions ✱✈❪ ✱①❫ ❯❭❲ ❯❭❩ ❯❭❬ ❯❭❬ » Cross section » Overview » Variations in the gaugino masses Summary This, together with changes in the Higgs sector, alters the neutralino direct detection properties, in particular, the Neutralino-nucleon cross section has to be re-evaluated. 24.5.2005 Seoul-The dark side of the Universe - p. 31/55

  55. ✛ ✜ ✕ ✖ ✔ ✛ ✛ ✔ ❯ ✕ ✜ ✱ ❅ ✔ ✔ Neutralino-nucleon cross section We only concentrate on the spin-independent part of the cross-section » Outline Introduction Neutralino dark matter in the Squark-exchange: MSSM ✘✚✙ ✘✚✙ ✕✗✖ Supergravity models formally identical to MSSM; new mixings in coupling ❯✵❱ Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 32/55

  56. ➼ ❅ ❦ ✧ ➒ ß ❀ ✒ ❥ ø ✒ ❅✇ ❥ ø ❅✇ ❦ ❥ ❅ ✓ ø ß ❦ ø ☛ ❅ ➤ ➙ ❾ ❿ ❆ ❥ ø ❅ ß ❥ ❀ ❅ ❥ ø ❅ ✒ ß ❀ ☛ ❀ ❥ ❅ ❫ ❅ ➺ ☛ ➼ ✵ ✆ ❹ ✿ ✧ ø ❝ ❆ ❻ ➩ ß ❀ ☛ ➺ ❅ ✴ ✓ ø ✧ ❅ ✒ ❦ ß ❀ ❅ ❥ ø ❅✇ ✧ ❅ ó ß ❀ ✒ ❥ ❅ ✓ ø ❥ ☛ ø ❥ ✜ ❖ ✯ ✪ ✩ ✰ ✯ ★ ★ ★ ★ ✱ ❯ ✒ ✜ ✧ ✤ ✣ ✧ ✣ ✧ ✢ ✢ ✢ ✢ ✻ ❅ ✷ ✴ ❹ ✧ ✆ ➨ ✷ ✆ ✴ ✸ ➨ ✷ ❀ ✴ ✶ ✕ ➬ ❀ ❀ ☛ ✱ ✒ ❀ ✳ ✻ ❅ ❅ ✬ Neutralino-nucleon cross section We only concentrate on the spin-independent part of the cross-section » Outline Introduction Neutralino dark matter in the Squark-exchange: MSSM ✥✚✦ ✥✚✦ ✣✗✤ Supergravity models formally identical to MSSM; new mixings in coupling ❯✵❱ Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section Higgs-exchange: » Enhancing the cross section » Constraints on the parameter space ✬✮✭ ✬✮✭ ✷ ✮✵ ✩✫✪ » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino ✬✲✱ masses Summary ❽✵❾ 24.5.2005 Seoul-The dark side of the Universe - p. 32/55

  57. ✺ ✾ ✹ ✹ ✹ ✿ ✻ ✾ ✴ ❵ ❛ ✱ ❅ ✌ ❶ ✱ ❅ ❥ ❅ ✒ ❥ ❅✇ ✿ ✻ ✱ ✿ ➨ ✱ ✹ Enhancing the cross section » Outline Introduction In the MSSM larger predictions for can be obtained ✼✮✽ ✼✮✽ ✺✫✻ Neutralino dark matter in the when the Higgs-exchange diagrams are enhanced by MSSM Supergravity models ✼✲❀ Increasing the Higgsino content of ❯✵❱ ( and ) Neutralino dark matter in the NMSSM » Motivation Decreasing the mass of the exchanged Higgses ( and » Overview of the NMSSM ) » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 33/55

  58. ❅ ✴ ❥ ❁ ❁ ❆ ❇ ❅✇ ❂ ❃ ❆ ❵ ✿ ❛ ✱ ❅ ✌ ❶ ❥ ✒ ✱ ❅ ❁ ❁ ✻ ❶ ❅ ✱ ✴ ✗ ☞ ✧ ✜ ➭ ✱ ✻ ✿ ✰ ✜ ✡ ✱ ➨ ✿ ✱ ✌ Enhancing the cross section » Outline Introduction In the MSSM larger predictions for can be obtained ❄✮❅ ❄✮❅ ❂✫❃ Neutralino dark matter in the when the Higgs-exchange diagrams are enhanced by MSSM Supergravity models ❄✲❈ Increasing the Higgsino content of ❯✵❱ ( and ) Neutralino dark matter in the NMSSM » Motivation Decreasing the mass of the exchanged Higgses ( and » Overview of the NMSSM ) » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter The second possibility is particularly important in the NMSSM space » Case(i) » Masses and compositions » Cross section Very light Higgses can be obtained, considerably enhancing the -channel. » Overview » Variations in the gaugino masses Such light Higges ( ✔✖✕ ), which have a relatively large singlet composition, can induce an increase in of several orders of magnitude. Summary ❵❜❛ The lightest Higgs cannot be pure singlet, since the coupling vanishes. 24.5.2005 Seoul-The dark side of the Universe - p. 33/55

  59. ❯ ➤ ✱ ❱ ✧ P ❅ ✱ ✕ ✌ ò ➴ ò ❞ ❳ ❻ ▲ ❳ ➱ ↔ ➣ → ❝ ➱ ❳ ❅ ❬ ✸ ✌ ➮ ◆ ➮ ✱ ✡ ✶ ➴ Ò ✱ ✡ ò ➴ ➴ ò ❖ Ò ✱ ✡ ✌ ò ➴ ò ✌ ë ■❏❑ ❖ ❡ ✡ ✱ ✶ ✡ ✱ ◗ ✱ ✫ ➮ ❺ ❳ ❋●❍ ✫ ❖ ❺ ❡ ❳ ❙ ➮ ❺ ❡ ✸ ✌ ➒ ó ➴ ❉❊ ò ✵ ù ➣ ù ❝ ☛ ❝ ❅ ❝ ò ➩ ❾ ➙ ➤ ✾ ➒ ✐ ✆ ✽ ❡ ❳ Constraints on the parameter space We work with the following input parameters, given at the EW scale: » Outline Introduction Neutralino dark matter in the ➥✯ú ➥✭û MSSM Supergravity models The Higgs potential is minimised numerically with the code . Neutralino dark matter in the Ellwanger, Gunion, Hugonie ’04 NMSSM » Motivation » Overview of the NMSSM The NMSSM spectrum is then obtained and the following constraints applied » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross Absence of Landau poles below section » Enhancing the cross section Experimental constraints from LEP » Constraints on the parameter space ➵✦➸ ▼ » Case(i) Neutralino: , direct production ( ); Chargino and ❯✵❱ » Masses and compositions » Cross section Neutral Higgs: Constraints on production rates » Overview » Variations in the gaugino masses (IHDM) Summary (DHDM) ❽✵❾ ✱ ❘◗ (APM) The constraint on the neutralino relic density is not imposed. 24.5.2005 Seoul-The dark side of the Universe - p. 34/55

  60. ❾ ➤ ➤ ó ➭ ☞ ✐ ✘ ☞ ➙ ❾ ✾ ➩ ➥ û ✐ ✽ ➒ ➙ ✐ ➩ ➥ ✝☞ ✝ ✆ ✐ ☞ ☞ ✧ ✆ û ✆ ❳ ☞ ú ✢ ☞ ➥ ✧ ✆ Results ( , (i) , ) ➥✯ú ➥✭û For £xed values of ➥✯ú , , , , we analyse the constraints on the plane: » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 35/55

  61. ➩ ➤ ➤ ó ➭ ☞ ✐ ✘ ☞ ➙ ❾ ❾ ✾ ➥ û ✐ ✽ ➒ ➙ ✐ ➩ ➥ ✝☞ ✝ ✆ ✐ ☞ ☞ ✧ ✆ û ✆ ❳ ☞ ú ✢ ☞ ➥ ✧ ✆ Results ( , (i) , ) ➥✯ú ➥✭û For £xed values of ➥✯ú , , , , we analyse the constraints on the plane: » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM Landau Pole » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 35/55

  62. ➩ ➤ ➤ ó ➭ ☞ ✐ ✘ ☞ ➙ ❾ ❾ ✾ ➥ û ✐ ✽ ➒ ➙ ✐ ➩ ➥ ✝☞ ✝ ✆ ✐ ☞ ☞ ✧ ✆ û ✆ ❳ ☞ ú ✢ ☞ ➥ ✧ ✆ Results ( , (i) , ) ➥✯ú ➥✭û For £xed values of ➥✯ú , , , , we analyse the constraints on the plane: » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM Landau Pole » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) Higgs tachyons » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 35/55

  63. ❳ ➤ ➤ ó ➭ ☞ ✐ ✘ ☞ ➙ ❾ ❾ ➩ ✾ ➥ û ✐ ✽ ➒ ➙ ✐ ➩ ✐ ✆ ✝ ☞ ✧ ✆ û ➥ ✆ ☞ ☞ ✧ ✆ ú ➥ ✝☞ ✢ ☞ Results ( , (i) , ) ➥✯ú ➥✭û For £xed values of ➥✯ú , , , , we analyse the constraints on the plane: » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM Landau Pole » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) Higgs tachyons » Masses and compositions » Cross section » Overview » Variations in the gaugino False minima masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 35/55

  64. ❳ ➤ ➤ ó ➭ ☞ ✐ ✘ ☞ ➙ ❾ ❾ ➩ ✾ ➥ û ✐ ✽ ➒ ➙ ✐ ➩ ✐ ✆ ✝ ☞ ✧ ✆ û ➥ ✆ ☞ ☞ ✧ ✆ ú ➥ ✝☞ ✢ ☞ Results ( , (i) , ) ➥✯ú ➥✭û For £xed values of ➥✯ú , , , , we analyse the constraints on the plane: » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM Landau Pole » Neutralino-nucleon cross section » Enhancing the cross section LEP constraints » Constraints on the parameter space » Case(i) Higgs tachyons » Masses and compositions » Cross section » Overview » Variations in the gaugino False minima masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 35/55

  65. ➥ ➙ ➙ ✐ ➭ ☞ ✐ ✘ ☞ ➤ ❾ ➩ ➩ ➤ û ✐ ✽ ➒ ❳ ó ❾ ✾ ✆ ✢ ➒ ó ✝☞ ✝ ✆ ✐ ☞ ☞ ✧ ✆ û ➥ ➥ ☞ ☞ ú ✆ ✧ Results ( , (i) , ) ➥✯ú ➥✭û For £xed values of ➥✯ú , , , , we analyse the constraints on the plane: » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the Higgsino NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross Neutralino sector: section » Enhancing the cross section The Singlino composition increases » Constraints on the parameter for small and , and the mass Singlino space decreases. » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 36/55

  66. ➤ ❾ ✐ ➙ ☞ ✐ ✘ ☞ ➤ ➙ ➩ ✆ ➥ û ✐ ❾ ✽ ➒ ❳ ó ✾ ➩ ➭ ✢ û ➒ ó ➒ ó ✝☞ ✝ ✆ ✐ ☞ ☞ ➥ ✆ ✧ ➥ ☞ ☞ ✧ ✆ ú Results ( , (i) , ) ➥✯ú ➥✭û For £xed values of ➥✯ú , , , , we analyse the constraints on the plane: » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the Doublet NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross Neutralino sector: section » Enhancing the cross section The Singlino composition increases » Constraints on the parameter for small and , and the mass space Singlet decreases. » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino Higgs sector: masses Light Higgses which are mainly Summary Singlets are found for small and . 24.5.2005 Seoul-The dark side of the Universe - p. 36/55

  67. ✘ ✆ ✐ ☞ ➭ ✐ ➤ ➙ ❾ ➩ ✆ ✢ ú ➥ ✧ ☞ ✝☞ ✝ ✆ ✐ ☞ ☞ ☞ ✧ ✆ û ➥ ☞ Results ( , (i) , ) ➥✯ú ➥✭û The corresponding neutralino-nucleon cross section as a function of the neutralino mass » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross Black dots ful£l all the constraints. section » Enhancing the cross section » Constraints on the parameter Grey dots are excluded by LEP . space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary 24.5.2005 Seoul-The dark side of the Universe - p. 37/55

  68. ✪ ✧ ✝☞ ✝ ✆ ✐ ✒ ☞ ☞ ✆ ☛ û ➥ ✘ ☞ ☞ ✧ ✆ ú ❅ ß ✢ ✌ ✱ ✻ ✿ ✧ ☞ ☞ ↕ ✝☞ ✘ ➭ ❶ ✌ ❅ ✱ ✞ ✴ ✳ ➥ ✆ ➭ ☛ ❅ ✓ ✘ ☞ ✞ ✢ ❥ ❅ ❥ ✒ ❦ ❥ ☛ ❅✇ ➭ ☞ ✞ ☛ ➲ ➩ ✳ ❾ ➙ ➤ ☞ ✘ ✐ ☞ ➭ ✐ ☞ ✞ ❅ Results ( , (i) , ) ➥✯ú ➥✭û The corresponding neutralino-nucleon cross section as a function of the neutralino mass » Outline Introduction Neutralino dark matter in the MSSM GeV Supergravity models GeV Neutralino dark matter in the NMSSM GeV » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross Black dots ful£l all the constraints. section » Enhancing the cross section » Constraints on the parameter Grey dots are excluded by LEP . space » Case(i) » Masses and compositions » Cross section Large values for the cross section » Overview » Variations in the gaugino pb are obtained for masses ❵❜❛ very light singlet-like Higgses. Summary Lightest Higgs: GeV with Lightest Neutralino: and 24.5.2005 Seoul-The dark side of the Universe - p. 37/55

  69. ☞ ➥ ✫ ✱ ☞ ☞ ❙ ú ☞ ☞ ☞ ❙ ✝☞ ✝ ✆ ✐ ✴ ☞ ❳ ✆ ❳ ✫ ❳ ✢ ❳ ✧ ➩ ✫ ❾ ➙ ➤ ✝ ☞ ☞ ☞ ☞ ➲ ➲ ✝➲ ➤ ➙ ❾ ➩ ✘ ❥ ❅ ☛ ❅ ✓ ✘ ☞ ✞ ❙ ➭ ✱ ✆ ✻ ☛ ❝ ☛ ❅ ✆ ❅ ❝ ❅ ✌ ❶ ✿ ➲ Overview , (i-iii) The GUT relation is £xed GeV, with GeV » Outline Introduction Neutralino dark matter in the GeV , ➥✭û GeV , MSSM Supergravity models Neutralino dark matter in the NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section » Enhancing the cross section » Constraints on the parameter space » Case(i) » Masses and compositions » Cross section » Overview » Variations in the gaugino masses Summary Large values for correspond to: ❵❜❛ Very light singlet-like Higgses ( GeV), , and neutralinos which are Higgsino-singlino with . 24.5.2005 Seoul-The dark side of the Universe - p. 38/55

  70. ✾ ✆ ☞ ☞ ✧ ✆ û ➥ ☞ ☞ ✧ ✢ ✱ ✆ ➩ ❾ ➙ ➤ ☞ ☞ ➲ ❝ ✐ ❅ ➲ ❅ ✪ ✞ ☞ ➭ ❅✇ ☛ ❥ ❦ ✒ ☛ ✽ ❥ à ✢ ✞ ☞ ✘ ✓ ❅ ☛ ❥ ☞ ❅ ☞ ❅ ❝ ❝ ☛ ✘ ✐ ❝ ❅ ✆ ❅ ☛ ❝ ☛ ✐ ✆ ✝ ✝ ✘ Variations in the gaugino masses , (i) So far we have analysed the case . Let us now address variations in the » Outline gaugino mass parameters Introduction Neutralino dark matter in the Preserving the GUT relation MSSM Supergravity models Neutralino dark matter in the GeV NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section GeV » Enhancing the cross section » Constraints on the parameter space » Case(i) ➥✯ú GeV » Masses and compositions GeV » Cross section » Overview » Variations in the gaugino masses Summary For low ❯✵❱ , is singlino-Higgsino like 24.5.2005 Seoul-The dark side of the Universe - p. 39/55

  71. ➤ ☞ ☞ ➲ ❅ ❝ ☞ ➲ ✓ ☞ ❅ ✧ ✘ ☞ ✝ ✝ ✆ ✐ ☛ ☞ ☛ ☛ ✽ ❅ ☞ ☞ ✧ ✆ û ➥ ☞ ➙ ☞ ✧ ✆ ❥ ✢ ✆ ➩ ❾ ❝ ❅ ✐ ✪ ❦ ❥ ☛ ❅✇ ➭ ☞ ✞ ✾ ❅ ✐ ✱ ❅ ✴ ✱ ❅ ✌ ❶ ✒ ☛ ✆ ❥ ❅ ❝ ☞ ✞ ☛ ❝ ✘ ❅ ❝ ✘ ✐ ✢ à ✱ Variations in the gaugino masses , (i) So far we have analysed the case . Let us now address variations in the » Outline gaugino mass parameters Introduction Neutralino dark matter in the Preserving the GUT relation MSSM Supergravity models Neutralino dark matter in the GeV, GeV NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section GeV » Enhancing the cross section » Constraints on the parameter space » Case(i) ➥✯ú GeV » Masses and compositions GeV » Cross section » Overview » Variations in the gaugino masses Summary For low ❯✵❱ , is singlino-Higgsino like When increases, the gaugino components of become more important and ❯✵❱ ❵❜❛ decreases. 24.5.2005 Seoul-The dark side of the Universe - p. 39/55

  72. ✢ ❝ ➩ ❾ ➙ ➤ ❅ ☞ ☞ ➲ ❅ ☞ ☛ ➲ ✒ ☞ ☞ ➲ ❦ ☞ ☞ ✧ ✆ ❥ ☞ ✢ ❥ ✽ ✓ ❅ ✱ ✘ ☞ ✐ ✞ ☞ ✆ ☞ ✧ ✆ û ➥ à ☞ ☞ ✧ ❥ ✝ ❅ ❶ ✪ ✾ ✐ ✱ ❅ ✴ ✱ ❅ ✌ ✐ ☞ ✱ ❅ ✴ ❵ ❛ ✱ ❅ ✌ ❶ ✞ ➭ ✝ ☛ ✆ ✐ ☛ ❝ ☛ ❅ ✆ ❅ ❝ ❅✇ ☛ ❝ ✘ ❅ ❝ ✘ ✐ ☛ Variations in the gaugino masses , (i) So far we have analysed the case . Let us now address variations in the » Outline gaugino mass parameters Introduction Neutralino dark matter in the Preserving the GUT relation MSSM Supergravity models Neutralino dark matter in the GeV, GeV, GeV NMSSM » Motivation » Overview of the NMSSM » Higgs Sector » The neutralino in the NMSSM » Neutralino-nucleon cross section GeV » Enhancing the cross section » Constraints on the parameter space » Case(i) ➥✯ú GeV » Masses and compositions GeV » Cross section » Overview » Variations in the gaugino masses Summary For low ❯✵❱ , is singlino-Higgsino like When increases, the gaugino components of become more important and ❯✵❱ ❵❜❛ decreases. For large is bino-like and is beyond experimental sensitivity. ❯✵❱ 24.5.2005 Seoul-The dark side of the Universe - p. 39/55

  73. » Outline Introduction Neutralino dark matter in the MSSM Supergravity models Summary Neutralino dark matter in the NMSSM Summary » Summary (NMSSM) 24.5.2005 Seoul-The dark side of the Universe - p. 40/55

  74. ✱ ✘ ❶ ❛ ❵ ✴ ✿ ✻ ❶ ✌ ❅ ✱ ✱ ✴ ❅ ✪ ✌ ☞ ➲ ☞ ✘ ✿ ✱ ❅ ✘ ✝ ☞ ☞ ❅ Summary (NMSSM) Supersymmetric theories provide a natural dark matter candidate in terms of the » Outline Lightest SUSY particle. Introduction Neutralino dark matter in the The impressive experimental efforts in dark matter detection, in particular of WIMPS MSSM motivate the theoretical analysis of the theoretical predictions for neutralino detection Supergravity models Neutralino dark matter in the NMSSM Next-to-MSSM Summary » Summary (NMSSM) Large values of are attainable, within the reach of future dark matter experiments ❵❜❛ The increase in is due to an enhancement of Higgs-exchanging diagrams, due to the presence of very light Higgses ( GeV) with a signi£cant singlet composition. The lightest neutralino is a mixed singlino-Higgsino state with GeV ❵❜❛ In progress: Include calculation of the relic density and constraints on low energy observables. 24.5.2005 Seoul-The dark side of the Universe - p. 41/55

  75. » Outline Introduction Neutralino dark matter in the MSSM Supergravity models Extra Slides MSSM Neutralino dark matter in the NMSSM Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe - p. 42/55

  76. ❷ ❚ ☛ ü ✆ → ✜ ➺ ❷ ➼ ❷ ❚ ❷ ✜ ❷ ➺ ❷ ➼ ❝ ✾ ✆ ❣ ✰ ò ü ❅ ❲ ➼ ❷ ➺ ☛ → ✜ ✆ ❷ ▼ Rotation curves in spiral galaxies » Outline Introduction Neutralino dark matter in the rot MSSM rot Supergravity models Neutralino dark matter in the = distance to the center of the galaxy NMSSM = mass contained within that radius Summary Extra Slides MSSM » Rotation curves in spiral Beyond the luminous disk galaxies » Rotation curves in spiral galaxies r ✽ ❱❯ rot » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA v 24.5.2005 Seoul-The dark side of the Universe - p. 43/55

  77. ❫ ✾ → ➺ ❷ ➼ ❷ ❚ ❷ ❚ ✜ ➺ ❷ ➼ ❝ ✆ ü ❣ ✰ ò ü ❅ ❲ ❷ ❳ ❨ ❭ ❭ ð ❪ ❡ ✆ ✜ ☛ ☛ ❷ ➼ ❷ ➺ ✜ → ✆ ❷ ▼ Rotation curves in spiral galaxies » Outline Introduction Neutralino dark matter in the rot MSSM rot Supergravity models Neutralino dark matter in the = distance to the center of the galaxy NMSSM = mass contained within that radius Summary Extra Slides MSSM » Rotation curves in spiral Beyond the luminous disk galaxies » Rotation curves in spiral galaxies ✽ ❱❯ rot » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA Roy ’00, data from Corbelli, Salucci ’99 However, observations show for ❩✗❬ rot 24.5.2005 Seoul-The dark side of the Universe - p. 44/55

  78. ✰ ò ❝ ✾ ❯ ü ❣ Rotation curves in spiral galaxies » Outline Introduction The galaxy is surrounded by a spherical halo of Dark Matter with Neutralino dark matter in the MSSM Supergravity models Neutralino dark matter in the NMSSM ✽ ❱❯ Summary rot ( i.e., self gravitational ball of ideal gas ) Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe - p. 45/55

  79. Clusters of galaxies » Outline Introduction Neutralino dark matter in the MSSM Supergravity models Measurement of peculiar velocities (Zwicky ’33) Neutralino dark matter in the NMSSM Summary X-ray measurements of the temperature of the gas Extra Slides MSSM » Rotation curves in spiral (Briel, Henry, Bohringer ’92; White ’93) galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral Gravitational lensing galaxies » Clusters of galaxies (Tyson ’94) » mSUGRA Coma Cluster 24.5.2005 Seoul-The dark side of the Universe - p. 46/55

  80. ❯ ❖ mSUGRA The constraint on the relic density leaves narrow accepted regions. » Outline Introduction Neutralino dark matter in the MSSM Bulk region Supergravity models Neutralino dark matter in the NMSSM Coannihilation “tail” with Next-to-LSP (in this case the ) Summary Extra Slides MSSM » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe - p. 47/55

  81. ❯ ❖ mSUGRA The constraint on the relic density leaves narrow accepted regions. » Outline Introduction Neutralino dark matter in the MSSM Bulk region Supergravity models Neutralino dark matter in the NMSSM Coannihilation “tail” with Next-to-LSP (in this case the ) Summary Extra Slides MSSM Rapid annihilation through CP-odd Higgs » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Rotation curves in spiral galaxies » Clusters of galaxies » mSUGRA 24.5.2005 Seoul-The dark side of the Universe - p. 47/55

  82. » Outline Introduction Neutralino dark matter in the MSSM Supergravity models Extra Slides NMSSM Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe - p. 48/55

  83. þ ó ☛ ❝ ☛ ❞ ✧ ❻ ✧ ➩ ➒ ❡ ✽ ❦ ❡ ☛ ✾ ➓ ❅ ✒ ✆ ✧ ➒ ☛ ü ❅ ❡ ➒ ü ü ➒ ✽ ❡ ➩ ✽ ó ❡ ✾ ➓ ✒ ✒ ✆ ✫ ó ☛ ☛ ✆ ❦ ó ❡ ❦ ➒ ❡ ü ❅ ü ☛ ➓ ❅ ☛ ☛ ❦ ➜ þ ✮ à ✡ ✱ ❅ ✆ ß ❅ ❅ ❬ ✱ ❅ ❦ ❬ ß ❅ ☛ ❬ ✱ ☛ þ ❦ ß ❅ ✒ ß ✱ ✱ ✮ ✧ ❡ ó ❡ ✾ ➓ ☛ ✒ ✆ ✧ ➒ ☛ ü ☛ ➒ ❀ ü ❅ ✽ ❦ ✧ ó ❡ ✾ ✡ ✱ ❀ ✆ ß ➤ ❦ ✏ ◗ ✃ ❻ ❡ ✧ ➩ ✢ ó ó ❡ ✱ ❡ ✷ ✆ ✽ ý ✷ ❴ ý ✱ ❤ ❴ ☛ ú ➸ ✽ ➥ ➒ ú ✧ ó ❡ ✾ ➒ ü ✾ Ñ ✧ ó ❡ ✾ ➒ ❦ ✧ ó ❦ ☛ ➓ ü ✆ ó ☛ ❡ ✾ ✆ ➓ ☛ ☛ ❝ ❅ ☛ ❞ ❻ ❈ ☛ ☛ ➩ ❦ ➒ ❦ ú ✽ ✃ ➵ ❅ ✆ ❝ ☛ ❞ ✏ ➜ ❻ ☛ ➩ ❦ ➒ ❡ ■ ➤ ➙ ❾ ➩ ✽ Higgs Sector CP-odd Higgs: » Outline Introduction ➥✯ú Neutralino dark matter in the ➥✯ú ➥✭û ❽✵❾ MSSM Supergravity models Neutralino dark matter in the NMSSM CP-even Higgs: Summary Extra Slides NMSSM ☛✈ù ➥✚ú » Higgs Sector » Variations of the parameters ☛✈ù » Variations in the gaugino ➥✯ú ❽✵❾ masses » Variations in the gaugino masses ☛✈ù ➥✭û ➥✯ú » Case (ii) » Case (iii) » Case (iv) ☛✈ù ➥✯ú ❽✵❾ ☛✈ù ➥✯ú ☛✈ù ➥✯ú 24.5.2005 Seoul-The dark side of the Universe - p. 49/55

  84. ❾ ➙ ✴ ✻ ✱ ❅ ✌ ❶ ✘ ✝ ☞ ✌ ❉ ✿ ➤ ✝☞ Ò ➩ ✆ ✢ ✝ ➥ ú ✆ ✧ ☞ ☞ ✆ ✐ ✆ ✱ ✱ ☞ ☛ ☞ ✪ ➭ ❅ ✱ ✿ ➲ ✠ ✞ ☞ ➭ ✒ ❅ ß ✡ ➲ ✪ ➭ ❅ ò ➴ ò ✌ ➲ Variations of the parameters , (i) Decrease ➥✭û : » Outline Despite the decrease in the tachyonic region, the region excluded experimentally by Introduction (IHDM and DHDM) is much larger and imply pb. Neutralino dark matter in the ❵❜❛ MSSM , GeV , ➥✭û GeV , GeV Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) GeV with Mixed singlino-Higgsino neutralinos with GeV ❵❜❛ 24.5.2005 Seoul-The dark side of the Universe - p. 50/55

  85. ✱ ➩ ➙ ❾ ➩ ➲ ➤ ➙ ❾ ❳ ❾ ✧ ✴ ✆ ➩ ❅ ✌ ❶ ➤ ➤ ➙ ☞ ✧ ✝☞ ✝ ✆ ✐ ☞ ❾ ✆ ➙ ☞ ☞ ➩ ✧ ✆ ú ➥ ➤ Variations of the parameters , (i) Variations in : » Outline Low values of are more experimentally constrained, but allow for lighter Higgses with Introduction a large singlet component and thus large ❵❜❛ Neutralino dark matter in the MSSM , GeV , ➥✭û GeV , GeV Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) For large tachyonic regions are larger, the Higgs is mainly a doublet and the Neutralino is Higgsino-like. Similar results to those in the MSSM are obtained. 24.5.2005 Seoul-The dark side of the Universe - p. 50/55

  86. ✱ ➲ ✌ ❅ ➙ ❛ ❵ ✴ ❾ ➩ ✆ ✢ ➥ ➤ ✆ ú ☞ û ✝☞ ✝ ✆ ✐ ☞ ➲ ✆ ➥ ❳ ☞ ➲ ✫ ❶ Variations of the parameters , (i) Variations in ➥✯ú : » Outline There is a range of “optimal” values for ➥✯ú outside of which tachyons appear more easily in Introduction the Higgs sector and experimental constraints are more important. large Neutralino dark matter in the MSSM , GeV , GeV , GeV Supergravity models Neutralino dark matter in the NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters » Variations in the gaugino masses » Variations in the gaugino masses » Case (ii) » Case (iii) » Case (iv) 24.5.2005 Seoul-The dark side of the Universe - p. 50/55

  87. ✾ ☞ ✐ ☞ ☞ ✧ ✆ û ➥ ☞ ✧ ❅ ✆ ✢ ✆ ➩ ❾ ➙ ➤ ☞ ➲ ✱ ✽ ❝ ❅ ✪ ✞ ☞ ➭ ❅✇ ☛ ❥ ❦ ✒ ☛ ❥ ❥ à ✢ ✞ ☞ ✘ ✓ ❅ ☛ ❅ ☞ ☞ ✐ ❝ ☛ ➲ ❝ ✘ ❝ ❅ ✆ ❅ ☛ ❅ ❝ ☛ ✐ ✆ ✝ ✝ ☞ ✘ Variations in the gaugino masses , (i) So far we have analysed the case . Let us now address variations in the » Outline gaugino mass parameters Introduction Neutralino dark matter in the Preserving the GUT relation MSSM Supergravity models Neutralino dark matter in the GeV NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters GeV » Variations in the gaugino masses » Variations in the gaugino masses ➥✯ú GeV » Case (ii) GeV » Case (iii) » Case (iv) For low ❯✵❱ , is singlino-Higgsino like 24.5.2005 Seoul-The dark side of the Universe - p. 51/55

  88. ❾ ❅ ✞ ➙ ➤ ✢ ☞ ☞ ➲ ❝ ✆ ☞ ➲ à ☞ ☞ ✧ ❥ ☞ ➩ ✢ ✝ ☞ ✱ ❥ ☛ ✐ ❅ ✓ ☞ ✧ ☞ ✆ û ➥ ✘ ☞ ☞ ✧ ✆ ✝ ✆ ✽ ✾ ❥ ☛ ❅✇ ➭ ☞ ✞ ✪ ✐ ✒ ✱ ❅ ✴ ✱ ❅ ✌ ❶ ❦ ❅ ✐ ❝ ❅ ✆ ❅ ❝ ☛ ❅ ☛ ❝ ✘ ❅ ❝ ✘ ✐ ☛ ☛ Variations in the gaugino masses , (i) So far we have analysed the case . Let us now address variations in the » Outline gaugino mass parameters Introduction Neutralino dark matter in the Preserving the GUT relation MSSM Supergravity models Neutralino dark matter in the GeV, GeV NMSSM Summary Extra Slides NMSSM » Higgs Sector » Variations of the parameters GeV » Variations in the gaugino masses » Variations in the gaugino masses ➥✯ú GeV » Case (ii) GeV » Case (iii) » Case (iv) For low ❯✵❱ , is singlino-Higgsino like When increases, the gaugino components of become more important and ❯✵❱ ❵❜❛ decreases. 24.5.2005 Seoul-The dark side of the Universe - p. 51/55

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