1 / 26

Dark Matter Phenomenology of the GUT-less CMSSM

Dark Matter Phenomenology of the GUT-less CMSSM. 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

ryder
Download Presentation

Dark Matter Phenomenology of the GUT-less CMSSM

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. Dark Matter Phenomenologyof the GUT-less CMSSM 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. Parameter Soup • Don’t observe boson-fermion degeneracy, so SUSY must be broken (How?) • Most general case (MSSM) has > 100 new parameters! • Make some assumptions about SUSY breaking at a high scale, and evolve mass parameters down to low scale for observables • Explicitly add [soft] SUSY-breaking terms to the theory • Masses for all gauginos and scalars • Couplings for scalar-scalar and scalar-scalar-scalar interactions • CMSSM (similar to mSUGRA) • Assume universality of soft SUSY-breaking parameters at MGUT • Free Parameters: m0, m1/2, A0, tan(), sign() Pearl Sandick, UMN

  4. SUSY Dark Matter 1. Assume neutralinos were once in thermal equilibrium • 2. Solve the Boltzmann rate equation to find abundance now Pearl Sandick, UMN

  5. Be Careful! • Situations when care must be taken to properly calculate (approximate) the relic density: 1. s - channel poles • 2 m  mA 2. Coannihilations • m  mother sparticle 3. Thresholds • 2 m  final state mass Griest and Seckel (1991) Pearl Sandick, UMN

  6. Constraints Apply constraints from collidersandcosmology: mh > 114 GeV m± > 104 GeV BR(b  s ) HFAG BR(Bs  +--) CDF (g -- 2)/2 g-2 collab. LEP 0.09  h2  0.12 Pearl Sandick, UMN

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

  8. Rapid annihilation funnel 2m  mA bs B+-- CMSSM Pearl Sandick, UMN

  9. tan() CMSSM >0 and A0=0 0.094 < h2 < 0.129 tan() = 5,10,15,20,25,30, 35,40,45,50,55 Pearl Sandick, UMN

  10. CMSSM Summary • (If DM consists mainly of neutralinos), the constraint on the relic density of neutralinos restricts m1/2 and m0 to thin strips of parameter space. • tan() provides leverage. • Most of parameter space is not compatible with measured DM density. Pearl Sandick, UMN

  11. GUT-less CMSSM • What if SUSY breaking appears below the GUT scale? • Should the soft breaking parameters be universal below the SUSY GUT scale? • Mixed modulus-anomaly mediated SUSY breaking with KKLT type moduli stabilization (mirage mediation models), warped extra dimensions, … • SUSY broken in a hidden sector (communication to observable sector?) Add one new parameter! Scale of universality of the soft breaking parameters: Min Pearl Sandick, UMN

  12. M1/2 = 800 GeV 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

  13. 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

  14. 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

  15. Mass Evolution with Min • m1/2 = 800 GeV • m0= 1000 GeV • A0 = 0 • tan() = 10 • > 0 Pearl Sandick, UMN

  16. Neutralinos and Charginos Must properly include coannihilations involving all three lightest neutralinos! • m1/2 = 800 GeV • m0= 1000 GeV • A0 = 0 • tan() = 10 • > 0 Pearl Sandick, UMN

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

  18. h2 too small! Lowering Min – large tan() Pearl Sandick, UMN

  19. Direct Detection If neutralinos are DM, they are present locally, so will occasionally bump into a nucleus. • Plot all cross sections not forbidden by constraints • If calc < CDMWMAP, scale by calc/CDMWMAP Effective 4-fermion lagrangian for neutralino-nucleon scattering (velocity-independent pieces): spin independent (scalar) spin dependent • Fraction of nucleus participates • Important for capture & annihilation rates in the sun • Whole nucleus participates • Best prospects for direct detection Pearl Sandick, UMN

  20. Neutralino-Nucleon Scattering tan = 10, Min = MGUT Pearl Sandick, UMN

  21. Neutralino-Nucleon Scattering tan = 10, Min = 1012GeV Pearl Sandick, UMN

  22. Summary/Conclusions • Relaxed the standard CMSSM assumption of universality of soft breaking parameters at the GUT scale • Examined the impact of lower Min on the constraints from colliders and cosmology • Specific attention to consequences for neutralino dark matter • In GUT-less CMSSM, constraint on dark matter abundance changes dramatically with Min • Below critical Min, neutralinos can not account for the measured relic density! Pearl Sandick, UMN

  23. EXTRA SLIDES Pearl Sandick, UMN

  24. Non-zero Trilinear Couplings • 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

  25. Neutralino-Nucleon Scattering tan = 50, Min = MGUT Pearl Sandick, UMN

  26. Neutralino-Nucleon Scattering tan = 50, Min = 1014GeV Pearl Sandick, UMN

More Related