1 / 29

Phenomenology of GUT-less SUSY Breaking

Phenomenology of GUT-less SUSY Breaking. Pearl Sandick University of Minnesota. Ellis, Olive & PS, Phys. Lett. B 642 (2006) 389 Ellis, Olive & PS, JHEP 06 (2007) 079. Standard CMSSM. Soft SUSY-breaking parameters GUT-scale universality Use RGEs to run down to weak scale.

sylvie
Download Presentation

Phenomenology of GUT-less SUSY Breaking

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Phenomenology of GUT-lessSUSY Breaking Pearl Sandick University of Minnesota Ellis, Olive & PS, Phys. Lett. B 642 (2006) 389 Ellis, Olive & PS, JHEP 06 (2007) 079

  2. Standard CMSSM • Soft SUSY-breaking parameters • GUT-scale universality • Use RGEs to run down to weak scale Pearl Sandick, UMN

  3. mh > 114 GeV m± > 104 GeV BR(b  s ) HFAG BR(Bs  +--) CDF (g -- 2)/2 g-2 collab. LEP GUT-less CMSSM • Universality at GUT-scale Min < MGUT • Constraints from colliders and cosmology: 0.09  h2  0.12 Pearl Sandick, UMN

  4. SUSY Dark Matter • Solve Boltzmann rate equation: • Special Situations: • s - channel poles • 2 m  mA • thresholds • 2 m  final state mass • Coannihilations • m  mother sparticle Pearl Sandick, UMN

  5. M1/2 = 800 GeV No EWSB Evolution of the Soft Mass Parameters • First look at gaugino and scalar mass evolution. Gauginos (1-Loop): • Running of gauge couplings identical to CMSSM case, so low scale gaugino masses are all closer to m1/2 as Min is lowered. Pearl Sandick, UMN

  6. No EWSB m0 = 1000 GeV Evolution of the Soft Mass Parameters • First look at gaugino and scalar mass evolution. Scalars (1-Loop): • As Min low scale Q, expect low scale scalar masses to be closer to m0. Pearl Sandick, UMN

  7. Evolution of the Soft Mass Parameters • Higgs mass parameter,  (tree level): • As Min low scale Q, expect low scale scalar masses to be closer to m0. • 2 becomes generically smaller as Min is lowered. Pearl Sandick, UMN

  8. Mass Evolution with Min m1/2 = 800 GeV m0= 1000 GeV A0 = 0 tan() = 10 • > 0 No EWSB Pearl Sandick, UMN

  9. Neutralinos and Charginos m1/2 = 1800 GeV m0= 1000 GeV A0 = 0 tan() = 10 • > 0 Must properly include coannihilations involving all three lightest neutralinos! Pearl Sandick, UMN

  10. Focus Point LEP Higgs mass Relaxed LEP Higgs LEP chargino mass 2 < 0 (no EWSB) g--2 suggested region stau LSP Coannihilation Strip Standard CMSSM Pearl Sandick, UMN

  11. h2 too small! Lowering Min - tan() = 10 Pearl Sandick, UMN

  12. Rapid annihilation funnel 2m  mA bs B+-- Large tan() Pearl Sandick, UMN

  13. h2 too small! Lowering Min - tan() = 50 Pearl Sandick, UMN

  14. A0 0 • A0 > 0  larger weak-scale trilinear couplings, Ai • Large loop corrections to  depend on Ai, so  is generically larger over the plane than when A0 = 0. • Also see stop-LSP excluded region Pearl Sandick, UMN

  15. Spin-Dependent Scalar Direct Detection:Neutralino-Nucleon Cross Sections • Interaction Lagrangian (neglecting velocity dep. terms): • Plot all cross sections not forbidden by constraints • If calc < CDMWMAP, scale by calc/CDMWMAP Pearl Sandick, UMN

  16. Direct Detection:Neutralino-Nucleon Cross Sections CDMS (2006) Pearl Sandick, UMN

  17. Direct Detection:Neutralino-Nucleon Cross Sections Pearl Sandick, UMN

  18. Conclusions • Intermediate scale unification results in: • Rapid annihilation funnel even at low tan() • Merging of funnel and focus point • Below some critical Min (dependent on tan() and other factors), all of nearly all of the (m1/2, m0) plane is disfavored because the relic density of neutralinos is too low to fully account for the relic density of cold dark matter. Pearl Sandick, UMN

  19. Extra Slides

  20. Neutralino-Nucleon Cross Sections Pearl Sandick, UMN

  21. Neutralino-Nucleon Cross Sections Pearl Sandick, UMN

  22. Sparticle Masses m1/2 = 800 GeV m0= 1000 GeV A0 = 0 tan() = 10 • > 0 Guaginos Squarks Pearl Sandick, UMN

  23. Lowering Min h2 too large Pearl Sandick, UMN

  24. Lowering Min Pearl Sandick, UMN

  25. Lowering Min h2 too small! Pearl Sandick, UMN

  26. Lowering Min - Large tan() Pearl Sandick, UMN

  27. Lowering Min - Large tan() Pearl Sandick, UMN

  28. Lowering Min - Large tan() Pearl Sandick, UMN

  29. Lowering Min - Large tan() h2 too small! Pearl Sandick, UMN

More Related