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S uper WIMP Dark matter

S uper WIMP Dark matter. in SUSY with a Gravitino LSP. Shufang Su • U. of Arizona. J. Feng, F. Takayama, S. Su hep-ph/0404198, 0404231. ~.  th G    v -1  ( gravitional coupling) -2 (comparig to WIMP of weak coupling strength)   v too small

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S uper WIMP Dark matter

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  1. SuperWIMP Dark matter in SUSY with a Gravitino LSP Shufang Su • U. of Arizona J. Feng, F. Takayama, S. Su hep-ph/0404198, 0404231

  2. ~ • thG v-1  (gravitional coupling)-2 • (comparig to WIMP of weak coupling strength) • vtoo small • thG too big, overclose the Universe ~ Why gravitino not considered as CDM usually? - However, gravitino can get relic density by other means SuperWIMP

  3. WIMP  SWIMP + SM particle - FRT hep-ph/0302215, 0306024 WIMP 104 s  t  108 s SWIMP SM Gravitino LSP  LKK graviton 106

  4. Outline - • SWIMP dark matter and gravitino LSP • Constraints • Late time energy injection and BBN • NLSP gravitino +SM particle slepton, sneutrino, neutralino - approach I: fix SWIMP=0.23 - approach II: SWIMP=(mSWIMP/mNLSP) thNLSP • Collider phenomenology • Conclusion

  5. ~ SWIMP: G (LSP) WIMP: NLSP mG» mNLSP ~ NLSP  G + SM particles SWIMP and SUSY WIMP - • SUSY case ~ Ellis et. al., hep-ph/0312262; Wang and Yang, hep-ph/0405186. 104 s  t  108 s

  6. /10-10 = 6.1 0.4  Dark matter density G· 0.23 ~ || · 9 £ 10-5 Fixsenet. al.,astro-ph/9605054 Hagiwara et. al., PDG Fields, Sarkar, PDG (2002) Constraints - ~ NLSP  G + SM particles  CMB photon energy distribution  Big bang nucleosynthesis Late time EM/had injection could change the BBN prediction of light elements abundances

  7. had EM had (GeV) EM (GeV) EM » mNLSP-mG Cyburt, Ellis, Fields and Olive, PRD 67, 103521 (2003) Kawasaki, Kohri and Moroi, astro-ph/0402490 BBN constraints on EM/had injection - • Decay lifetime NLSP • EM/had energy release EM,had=EM,had BrEM,had YNLSP

  8. approach I:fix G = 0.23 ~  m · 80 » 300 GeV 200 GeV · m · 400 » 1500 GeV mG¸ 200 GeV NLSP, EM,had=EM,had BEM,had YNLSP ~ apply CMB and BBN constraints on (NLSP, EM/had)  viable parameter space YNLSP: approach I - slepton and sneutrino

  9. G = (mG/mNLSP) thNLSP ~ ~ Approach II: right-handed slepton -

  10. G = (mG/mNLSP) thNLSP ~ ~ Approach II: sneutrino -

  11. Collider Phenomenology - • SWIMP Dark Matter • no signals in direct / indirect dark matter searches • SUSY NLSP:rich collider phenomenology NLSP in SWIMP: long lifetime  stable inside the detector • Charged slepton highly ionizing track, almost background free Distinguish from stau NLSP and gravitino LSP in GMSB • GMSB: gravitino m » keVwarm not cold DM • collider searches: other sparticle (mass) • (GMSB) ¿(SWIMP): distinguish experimentally Feng, Murayama and Smith, in preparation.

  12. Sneutrino and neutralino NLSP vs. ,  0.23  favor gravitino LSP ~ ~ - • sneutrino and neutralino NLSP missing energy signal: energetic jets/leptons + missing energy Is the lightest SM superpartner sneutrino or neutralino? • angular distribution of events (LC) Does it decay into gravitino or not? • sneutrino case: most likely gravitino is LSP • neutralino case: most likely neutralino LSP • direct/indirect dark matter search positive detection  disfavor gravitino LSP • precision determination of SUSY parameter: th, ~ ~

  13. Conclusions - • SuperWIMP is possible candidate for dark matter • SUSY models SWIMP:gravitino LSP WIMP:slepton/sneutrino/neutralino • Constraints from BBN: EM injection and hadronic injection need updated studies of BBN constraints on hadronic/EM injection • Favored mass region • Approach I: fix G=0.23 • Approach II: G = (mG/mNLSP) thNLSP • Rich collider phenomenology(no direct/indirect DM signal) • charged slepton:highly ionizing track distinguish from GMSB • sneutrino/neutralino:missing energy stable or not? ~ ~ ~

  14. ~ ~ ~ ~ ~ G G G G G • Decay life time  Mpl • SM energy distribution  mG  SUSY breaking scale NLSP SM NLSP SM ~ SM NLSP SM NLSP SM NLSP

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