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Dark Matter in the Left Right Twin Higgs Model

Ethan Dolle University of Arizona Work done with Shufang Su and Jessica Goodman. Dark Matter in the Left Right Twin Higgs Model. Outline. Left Right Twin Higgs Model Relic Density Analysis Direct and Indirect Detection Conclusion. Left Right Twin Higgs Model.

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Dark Matter in the Left Right Twin Higgs Model

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  1. Ethan Dolle University of Arizona Work done with Shufang Su and Jessica Goodman Dark Matter in theLeft Right Twin Higgs Model

  2. Outline • Left Right Twin Higgs Model • Relic Density Analysis • Direct and Indirect Detection • Conclusion

  3. Left Right Twin Higgs Model • Chacko, Goh, and Harnik: arXiv:hep-ph/0506256v1 • solution to Little Hierarchy Problem • To avoid EW precision constraints, add a second Higgs Ĥ that couple to gauge boson only

  4. Left Right Twin Higgs Model EWSB SM Higgs doublet SU(2)L Higg doublet Couples only to gauge bosons DM candidate

  5. Left Right Twin Higgs Model • Ĥ couples only to gauge bosons could be achieved by impose a discrete symmetry Good Bad • the lighter one of S, and A are stable, weakly interacting ⇒Natural WIMP candidates

  6. Left Right Twin Higgs Model • Need to impose mass splitting between A and S: Constraints from direct detection • h1 and h2 mass splitting

  7. Left Right Twin Higgs Model • Similar to Inert Higgs Doublet Model • Proposed by Barbieri, et al. • arXiv:hep-ph/0603188v2 • Dark matter analyzed by Honorez, et al. • arXiv:hep-ph/0612275 • Indirect detection analyzed by Gustafsson, et al. • arXiv:astro-ph/0703512

  8. Inert Higgs Doublet Model Left Right Twin Higgs Model Mhsm ~ 500 GeV Mhsm ~ 170 GeV New particles New particles extra scalars extra scalars Heavy gauge bosons Heavy top, heavy neutrinos Model Comparison

  9. Relic Density Analysis • WMAP: 0.093<Ωh2<0.128 at 2σ level • Need to solve Boltzmann equation • Must consider co-annihilations when mass splittings are small • Used program micrOMEGAS_2.0 • Solves Boltzmann equation exactly

  10. Relic Density Analysis • Modest choice of parameters yields • High mass: MS ~ 500 GeV • Low mass: MS<MW ( in progress)

  11. Omg h2 vs MS • Two regions: • Bulk • Pole • Due to heavy gauge bosons • Can change regions by changing: • f • mass splittings

  12. Contour plot of Omg h2 • MS in bulk region consistent • Can change regions by changing mass splittings

  13. Direct Detection • General idea: observe recoil of detector nuclei from dark matter collisions • Contributions from spin independent (SI) and spin dependent (SD) cross sections • Spin independent contribution dominates

  14. Contributing Processes • First 2 are difficult to see due to small CW couplings • ~(gv)2 instead of usual ~(λv)2 • Third process too big (~10-31 cm2) • Current CDMS limit: ~10-43 cm2 • Impose A-S mass splitting to avoid constraint

  15. Direct Detection Experiments • SI beats SD by 8 orders of magnitude • THM predicts values below future CDMS limits • Difficult!

  16. Indirect Detection • General idea: dark matter annihilates into photons, positrons, and neutrinos • Looked at photons • Monochromatic photons • Hadronization and fragmentation • Final state charged particle radiation

  17. Indirect Detection • Γ~(ρ)2 • Increased events for areas of high density • Galactic Halo • Sun • Earth • High dependence on halo dark matter density distribution

  18. Monochromatic Photons • Photon flux as a function of density: • Parameterize density with J: • Photon flux as a function of JΔΩ:

  19. Monochromatic Photons • J gives the clumping of DM near galactic center • Highly model dependent • 103 for NFW profile • 105 for Moore et al profile • ΔΩ indicates field of view of telescope • 10-3 sr for ground based ACTs (typical) • JΔΩ~1-100 • Flux scales linearly

  20. Monochromatic Photons • Contributing processes • Through loop processes only • Difficult to observe due to small couplings • Same problem as with direct detection!

  21. Hadronization and Fragmentation • Number as a function of Eγ • Spectra depends only on W/Z initial energies • Contributing processes

  22. Hadronization and Fragmentation • THM predictions for 2 regions • Detector limits: • GLAST • ACTs • Difficult, unless J is large • DM strongly clumped at galactic center GLAST BULK ACT POLE J ΔΩ = 1

  23. Final state radiation Contributing Processes

  24. Final State Radiation • Predictions for THM • 2 processes • Unique knee signature • 2 orders of magnitude below detector limits • Difficult! BULK POLE J ΔΩ = 1

  25. Conclusion • Left Right Twin Higgs Model provides a natural dark matter candidate • Can explain 100% of dark matter observed by WMAP • Direct detection difficult • Indirect detection: hadronization possible, other 2 are difficult • Thank you!

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