1. Overview of indirect dark matter detection Jae Ho HEO Theoretical High Energy group jaeheo1@gmail.com Yonsei University 2012 Jindo Workshop, Sep. 20-23

2. Outlines Jae Ho HEO2 1.Introduction 2.Relic abundance 3.Indirect detections (positrons, antiprotons, photons) 4.Direct detections (annual modulation, iDM) 5.Triplet dark matter (no hypercharge Y=0, but weak charge SU(2) ) 6.Future work Heo, PRD 80, 033001 (2009)

3. Jae Ho HEO3 1930s Zwicky L. Bergstrom Rept. Prog. Phys 63, 793 (2000) Galactic Rotation Curves Newtonian prediction  expect velocity to fall across the galactic disk as mass density falls. Observed rotational curves not consistent with visible distribution of matter. Supports the view that galaxies are immersed in a halo of so-called dark matter. Appears to make up ~83% of mass in the Universe

4. World Composition ( mass-energy density ) Nobody knows these

5. Jae Ho HEO5

6. 6 Targets

7. Jae Ho HEO7 Antimatters: rarely produced in astrophysical background. Gamma rays: can transport freely long distance without energy loss or transmutations of the direction. Dark matter particles can annihilate and create other particles relic abundance, indirect DM detection  Dark Matter Annihilation

8. RELIC ABUNDANCE Jae Ho HEO8 Relic density : Time evolution Boltzmann equation Constant inverse freeze out temperature : x F ~20-25 for 10 GeV<M <1000 GeV 25-… for M>1000 GeV 25-… for M>1000 GeV Thermal average for this annihilation P. Gondolo NP B360, 124 (1991) WMAP data : 0.1097 <  CDM h 2 <0.1165 (at 3  ) WMAP Col. AJS 180, 330 (2009) From Boltzman distribution considered relativity v~0.3 c

9. Source for Cosmic Ray Signals Jae Ho HEO9 Emissivity/energy at location x from GC Injected particle spectra DM density at location x (DM halo profile) : NFW, Moore, core Isothermal, Einasto Boost factor Fluxes Number of particles

10. Jae Ho HEO10 Boost factors Subhalo structure : less than 10 or 20 at GH, it can be very large ~100(000) around GC Sommerfeld nonperturbative effect : non-relativistic velocity and a long-range attractive force For a singe Abelian massless vector with potential Breit-Wigner resonance : In case that mediators have mass just below twice the DM mass annihilation rates can be enhanced  Sommerfeld enhancement factor: Cirelli et al., NPB 800, 204 (2008)

11. Jae Ho HEO11 Propagation of CRs Particles, emitted by whatever process, must reach the detector (Earth) travelling through a medium with structure (the galaxy): interstellar gas, magnetic field We have a standard diffusion model (Galprop) which assumes the galaxy is a flat cylinder with free scape at the boundaries Space diffusionEnergy lossConvective wind Scattering in IS (H, He atoms) Casse, Lemoine, Pelleetier, PRD 65, 023002 (2002)

12. Jae Ho HEO12 Two-Zone model Positrons: Antiprotons: Three propagation models : MIN, MED, MAX Correspond to minimal(MIN), medium (MED), maximum(MAX) antiproton fluxes.  Deliahaye et al., PRD 77, 063527 (2008) L=3-20 kpc h=0.1 kpc R=20 kpc 8.5 kpc SUN H, He

13. Jae Ho HEO13 A model with magnetic dipole Heo, Kim, arXiv:1207.1341

14. Jae Ho HEO14 Positrons Predicted signals have almost no difference in halo profiles or diffusion models. Predicted fractions exhibit rather sharp distribution at E~M, since our candidate can directly annihilate into electron-positron pair. Predicted signals with the boost factor, 30-80 nicely fit measurements of the PAMELA, Fermi LAT, etc We predict that an enhancement of 16 factor comes from Sommerfeld effect, and the rest 2-5 enhancements from the subhalo structure (dark clumps). Solar modulation at low energies (<10 GeV) Gleeson et al., Astropart. Phys. 154, 1011 (1968)

15. Jae Ho HEO15 Gamma-Rays from GH Almost no difference in the halo profiles Slightly touch EGRET anomaly The predicted signals are within the current unobservable experimental constraint.

16. Jae Ho HEO16 Antiprotons No difference in halo profiles Sensitive to the propagation models Viable in MIN propagation model Likely rule out for other propagation Models, MED and MAX The MED propagation parameters are in uncertainty of one order of magnitude. The MED propagation model might be viable, if we consider uncertainty of Propagation parameters.

17. Jae Ho HEO17 Gamma-Rays from around GC Most complex regions in galaxy due to many possible sources : difficult to model the diffuse emission, and discriminate the DM annihilation signals from background. Smoking-gun signatures : monochromatic gamma-ray lines

18. Jae Ho HEO 18 Signals from around GC Predictions are under experimental exclusion limits The predicted signals are in the potential probe at the AMS-02 with the better experimental method (energy resolution 1.5-2%, Fermi LAT 11-13%). C. Weniger, hep-ph/1205.2797 E. Tempel, A. Hektor, M. Raidal, hep-ph/1205.1045 A. Kounine, astro-ph/1009.5349; http://ams.cern.ch. Fermi. Col., astro-ph/1205.12739

19. Jae Ho HEO19 Direct dark matter detection

20. Jae Ho HEO20 Normal dark matter (elastic scattering)

21. Jae Ho HEO21 Inelastic dark matter

22. Jae Ho HEO22 M=50 GeV M=100 GeV M=300 GeV

23. Jae Ho HEO23 Triplet Dark Matter Extend the SM with an exotic lepton triplet E per family Anomaly constraints provide gauge charge of E Heo, PRD 80, 033001 (2009) Fermion gauge charges

24. Jae Ho HEO24 There are no photon and Z boson couplings : This avoids direct detection constraint. Neutral and charged Es have mass splitting by radiative correction (~165 MeV) :induce inelastic scattering for direct detection, but splitting is large -> also avoid direct detection constraint. I need consider indirect detection of this model

25. Thanks for the attention Jae Ho HEO25 Future Work Fermion triplet dark matter Scalar triplet dark matter Neutrino Telescopes : We need the magnetic profile of the SUN