1. MSSM in view of PAMELA and Fermi-LAT Ts. Enkhbat 2 nd workshop on LHC physics, CYCU, Chungli Based on: arXiv: 1002.3631 B. BajcB. Bajc, Ts. E, D. K. Ghosh, G. Senjanovic, Y. ZhangD. K. GhoshG. SenjanovicY. Zhang

2. Outline Introduction Decaying gravitino as the MSSM dark matter – Simple case Pamela and Fermi-LAT vs MSSM Phenomenological and cosmological implications Conclusions

3. Introduction The MSSM* is the main extension of the SM Virtues of the MSSM Stabilize the Gauge hierarchy Unification of the gauge couplings Dark matter candidate In addition can provide the light Neutrino masses and mixings through RPV Electroweak baryogenesis if stop is light or [Carena et al, 2008] Affleck-Dine baryogenesis through flat directions [Affleck & Dine, 1985] Inflation along the same flat directions [Allahverdi, 2006] *Here we define the MSSM as supersymmetrization of the SM + gravitino The last item is the topic of the present talk: The dark matter candidate in light of recent Sattillete experiments: PAMELA & Fermi-LAT

4. Sattellite experiments Pamela: 1.5 to 100GeV antiproton &positron flux PAMELA collaboration, arXiv: 0810.4995

5. Fermi-LAT Measures electron spectrum from 7GeV to 1TeV Fermi LAT collaboration, arXiv: 0905.0025, 1008.3999

6. Possible interpretations Astrophysical sources - Supernova remnants for Fermi LAT D. Grasso et al, 2009 [Fermi-LAT collaboration] - Nearby pulsars e.g. D. Hooper et al, 2009; P. Blasi, 2009; S. Profumo, 2008 Dark Matter - Annihilating DM - Decaying DM A viable mechanism must induce excess leptons not hadrons. We address this question in general MSSM

7. MSSM & decaying gravitino DM In its most general form, MSSM contains Constraints : nucleon decay A. Y. Smirnov & F. Vissani, 1996 : oscillation S. Dimopoulos & L.J. Hall, 1996; I. Hinchliffe & T. Kaeding, 1993; F. Zwirner, 1983; K.S. Babu& R. Mohapatra, 2001

8. Neutrino masses (or )dominates : dominates : a seesaw mechanism with the gaugino playing the role of the right handed neutrinos.

9. The size of the neutrino masses Large values for RPV couplings : Neutralinos cannot be DM! The only viable candidate for DM is the Gravitino!

10. Gravitino decays Relevant gravitino interactions in SUGRA Effective 2&3-body decay operators

11. Mass rangesGravitino decay modes

12. Photon & Neutrino mode Takayama & Yamaguchi, 2000 Monochromatic photons and neutrinos No such signal observed by Fermi-LAT If neutrino mass is dominated by sneutrino VEV or This case cannot explain PAMELA or Fermi-LAT!

13. 2 & 3-body decay rates

14. 2&3-body diagrams Neutrino channels

15. Charged lepton channels Higgs channels Three-body decay channels

16. Criteria to fit neutrino mass and PAMELA and/or Fermi-LAT ( ν mass) (PAMELA/Fermi-LAT) (leptophilic DM) (perturbativity bound)

17. The lower and upper bound on the slepton mass The upper limit on the gravitino mass An optimal fit for Fermi-LATfor this leaves narrow range for gravitino mass

18. Allowed region compatible with PAMELA The dashed line is the perturbativity bound. Blue (red) region is excluded by the gravitino (neutrino) mass.

19. Allowed region for Fermi-LAT The dashed line is the perturbativity bound

20. The fit for PAMELA only

21. The allowed region in theplane (for PAMELA)

22. The simultaneous fit for PAMELA positron excess and Fermi-LAT due to 3-body gravitino decay Fit for PAMELA

23. The fit for Fermi-LAT

24. Phenomenological consequences There is no LHC signatures if both PAMELA and Fermi-LAT are to be explained by gravitino decay: Phenomenologically interesting case is if gravitino is behind PAMELA only Gaugino NLSP: for Sizable amount decays inside detector. If charged wino is NLSP, leave highly ionized tracks.

25. Light slepton (with vanishing RPV coupling) as NLSP In this case the NLSP decays outside the detector Light slepton with If charged Displaced vertex /ionizing track, dilepton+ If sneutrino 2 charged lepton final states

26. Conclusions The MSSM even if taken as the theory of the neutrino masses it explain PAMELA excess. The sleptons are heavy with masses in the range 500 to 10^6 TeV The gravitino mass can be as light as 300 GeV Phenomenologically there is no constraint on the squark masses The Fermi-LAT data can be explaind only if the gravitino is around 3TeV. Perturbativity pushes the gravitino to lighter values. The decaying gravitino as the explanation of Fermi-LAT will kill any chance of MSSM being in the LHC range