1. Singlet Dark Matter, Type II Seesaw and Cosmic Ray Signals Nobuchika Okada Miami 2009 @ Fort Fauderdale, Dec. 15-20, 2009 University of Alabama, Tuscaloosa In collaboration with Ilia Gogoladze (University of Delaware) Qaisar Shafi (University of Delaware) Toshifumi Yamada (KEK, Japan) Ref: Gogoladze, N.O. and Shafi, “Type II Seesaw and the PAMELA/ATIC Signals, ” PLB 679 (2009) 237 Gogoladze, N.O.,Shafi, and Yamada, in preparation

2. 1. Introduction Existence of Dark Matter has been established! Wilkinson Microwave Anisotropy Probe (WMAP) satellite has established the energy budget of the present Universe with a great accuracy Dark Matter particle: non-baryonic electric charge neutral (quasi) stable

3. The property of the DM is still a prime open question in particle physics and cosmology Weakly Interacting Massive Particles (WIMPs) are among the best motivated classes of candidates for the dark matter  No candidate in the SM  New Physics beyond the SM What is the scale of WIMP? TeV scale New Physics is suitable for WIMP DM physics! Solving the Boltzmann Equation,

4. Investigating the nature of Dark Matter Collider Physics (LHC, ILC,…) Producing DM particles at colliders and measure DM properties mass, couplings with SM particles, spin, etc. Direct detection of DM A variety of experiments has been carried out to directly detect dark matter particle through its elastic scattering off a nucleon nucleon detector DM underground

5. cosmic rays originating from DM pair annihilations in the halo associated with our galaxy, sun, … Indirect detection of DM Sun Halo Sun DM Earth Cosmic-ray Many experiments: HEAT, PAMELA, ATIC, PPB-BETS, Fermi-LAT HESS, MAGIC, EGRET, Fermi-GLAST Super-K, IceCube

6. Recent hot topic: cosmic-ray e+/e- excesses (1) The PAMELA experiment has reported a significant positron excess over the expected background without a corresponding increase in the flux of anti-protons! Adriani et al., Nature 458, (2009) 607 Positron excess Expected Solar activity Expected

7. (2) Fermi satellite experiment also shows an excess of the sum of cosmic-ray e+ and e- flux

8. PAMELA and Fermi data may constitute the first indirect evidence of dark matter pair annihilations in the halo! Puzzle: excess of cosmic-ray e+/e- fluxes no excess of cosmic-ray anti-proton flux DM leptons DM quarks favored? disfavored? In normal dark matter models, there is no significant difference This implies a leptophilic nature of DM

9. Plan of this talk 1. Introduction 2. Propose a simple model of leptophilic DM 3. Numerical analysis Fitting to PAMELA and Fermi data and implication to neutrino physics 4. Summary

10. 2. Simple model of leptophilic dark matter What’s missing in the SM? 1. Dark Matter particle  we’ve already discussed 2. Neutrino masses and mixings Oscillation data Very small mass scale Large mixing angle

11. Simplest extension of the SM to incorporate Dark Matter particle & Neutrino Masses Introduce 2 scalars Gogolzdze, N.O. & Shafi, PLB 679 (2009) 237

12. Neutrino mass via Type II seesaw

13. DM relic abundance When, we get the right DM abundance

14. Leptophilic nature of DM If is small, dominates When DM pair annihilations happen in the halo, they produce mostly lepton flux The flavor structure of the primary lepton fluxes are determined by the Yukawa coupling and hence, there is a correlation with neutrino oscillation data

15. Interesting Implications Flavor structure of lepton flux carry the information of neutrino mass matrix: Cosmic-ray neutrino flux  would be detected in future experiments (ex: IceCube)

16. 3. Numerical Analysis We will show the proposed model can fit PAMELA and Fermi data with a suitable choice of parameters For data fitting, it is necessary to introduce a boost factor (BF~1000) to enhance the annihilation cross section of DMs in the halo DM relic abundance: Typical scale to fit PAMELA data: BF could either have astrophysical origin: large inhomogeneities in DM distribution a particle physics origin: Breit-Wigner enhancement New scalar S Arrange Gogolzadze, N.O., Shafi, and Yamada in preparation

17. In our analysis, free parameters in the model are: DM mass Annihilation cross section (with BF) Triplet scalar mass Yukawa coupling For simplicity, we consider two cases for triplet scalar mass (1)  triplets from DM annihilation almost at rest (2)  highly boosted triplets Energy distribution of primary leptons from triplet decay (1) (2)

18. In type II seesaw, For simplicity, we assume hierarchical neutrino mass spectrum From the formula of partial decay width and the neutrino oscillation data, we find the flavor structure of primary leptons as (i) Normal hierarchical case  e : mu : tau = 0.02 : 1 : 1 e : mu : tau = 2 : 1 : 1 (ii) Inverted hierarchical case 

19. We calculate cosmic-ray e+/e- flux from DM pair annihilation for various values of DM mass with the annihilation cross section with the boost factor being a free parameter and fit the PAMELA and Fermi data Positron and electron propagation in the galaxy is determined by the static diffusion equation Diffusion coef. Energy loss rate Source term Background flux:

20. Best fits to PAMELA and Fermi data (A) NH &

21. (B) NH &

22. (C) IH &

23. Upper bound on neutrino flux from galactic center by Super-K DM pair annihilations produce neutrino flux directly or via the decay of mu and tau SuperK measured the up-ward muon flux induced by cosmic-ray muon neutrinos  gives us the upper bound on neutrino flux from galactic center Earth SK Neutrinos from GC

24. Neutrino flux vs. SK upper bound Flux highly depend on DM density profile around the GC We consider two typical DM density profiles: NFW profile & isothermal profile with 4 kps core (A) NH & (B) NH & Too much flux

25. (C) IH & Inverted hierarchical case is consistent with SK bound

26. IceCube+DeepCore experiment can significantly improve the SK bound in the near future Mandal et al., arXiv:0911.5188 [hep-ph]

27. 5. Summary We have proposed a very simple extension of the SM to incorporate the DM particle and neutrino masses in the SM, where only one gauge singlet scalar and one SU(2) triplet scalar with a unit hypercharge are introduced. Neutrino masses are obtained by type II seesaw The type II seesaw structure naturally induces a leptophilic nature for the DM The flavor structure of the primary lepton fluxes are related to neutrino oscillation data because of type II seesaw

28. We have calculated cosmic-ray e+/e- fluxes for two typical masses, and, and for NH and IH neutrino mass spectrum We have shown that a suitable choice of mass and annihilation cross section (with the boost factor) can fit both PAMELA and Fermi data We have also calculated neutrino flux form GC and found that NH cases predict too much flux which is severely constrained by Super-K up-ward muon flux On the other hand, IH case with DM mass 1 TeV and can give a very nice fits to both the PAMELA and Fermi data without tension with the SK bound, and IH neutrino mass spectrum is favored