1 / 46

GUT-less SUSY Phenomenology

GUT-less SUSY Phenomenology. Pearl Sandick University of Minnesota. Ellis, Olive & PS, Phys. Lett. B 642 (2006) 389 Ellis, Olive & PS, JHEP 06 (2007) 079. Dark Matter Candidate!. R-Parity conservation. Why we like SUSY. Solves the Naturalness Problem Gauge coupling unification (GUTs)

gino
Download Presentation

GUT-less SUSY Phenomenology

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

  2. Dark Matter Candidate! R-Parity conservation Why we like SUSY • Solves the Naturalness Problem • Gauge coupling unification (GUTs) • Predicts a light Higgs boson Pearl Sandick, UMN

  3. Some other scale? What We Do • SUSY must be broken, so introduce soft SUSY-breaking parameters and assume high (GUT) scale values for them • Evolve parameters down to weak scale using RGEs of low energy effective theory (MSSM) • CMSSM: GUT-scale universality of soft breaking parameters • 5 inputs: m0, m1/2, A0, tan(), sign() Pearl Sandick, UMN

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

  5. 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

  6. 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

  7. 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

  8. 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

  9. 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

  10. 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

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

  12. How do we expect the constraints to evolve? • mA decreases logarithmically with Min • BR(b  s ) and BR(Bs  +--) at large tan() have important contributions from heavy Higgs exchange. These constraints will become more important as Min is lowered. •  decreases as Min is lowered. • Expect that the unphysical region where 2 < 0 encroaches farther into the plane. • When the LSP is bino-like, its mass increases as Min is lowered, so the forbidden stau LSP region encroaches into the plane. When the LSP becomes Higgsino-like, it’s mass decreases as Min is lowered, so the stau LSP boundary falls back down. Pearl Sandick, UMN

  13. 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

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

  15. 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

  16. Lowering Min - tan() = 10 Pearl Sandick, UMN

  17. Lowering Min - tan() = 10 Pearl Sandick, UMN

  18. Lowering Min - tan() = 10 Pearl Sandick, UMN

  19. Lowering Min - tan() = 10 Pearl Sandick, UMN

  20. Lowering Min - tan() = 10 Pearl Sandick, UMN

  21. Lowering Min - tan() = 10 Pearl Sandick, UMN

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

  23. bs B+-- Large tan() Pearl Sandick, UMN

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

  25. Lowering Min - tan() = 50 Pearl Sandick, UMN

  26. Lowering Min - tan() = 50 Pearl Sandick, UMN

  27. Lowering Min - tan() = 50 Pearl Sandick, UMN

  28. Lowering Min - tan() = 50 Pearl Sandick, UMN

  29. Lowering Min - tan() = 50 Pearl Sandick, UMN

  30. Lowering Min - tan() = 50 Pearl Sandick, UMN

  31. Lowering Min - tan() = 50 Pearl Sandick, UMN

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

  33. 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

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

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

  36. 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 or 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

  37. Neutralino-Nucleon Cross Sections Pearl Sandick, UMN

  38. Neutralino-Nucleon Cross Sections Pearl Sandick, UMN

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

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

  41. Lowering Min Pearl Sandick, UMN

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

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

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

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

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

More Related