Where is SUSY? Institut für Experimentelle Kernphysik

Transcription

1 Where is SUSY? Institut ür Experimentelle Kernphysik KIT Universität des Landes Baden-Württemberg und nationales Forschungszentrum in der Helmholtz-Gemeinschat

2 I supersymmetric particles exist, B- mesons ought to decay ar more oten than i they do not exist. CDF ound hint, but LHCb and CMS ailed to ind this eect. Where is SUSY? Where do we stand? From:

3 Open questions in Standard Model Magic solution: SUPERSYMMETRY What is origin o mass? Radiative electroweak symmetry breaking What is origin o dark matter? Why 3 dierent gauge groups? Why 3 dierent coupling constants? Why so large mass dierences in third generation? Why do neutrinos have mass at all? Lightest SUSY particle (LSP) Uniied group broken at lower energies Gauge couplings uniied at high energy Yukawa couplings uniied at high energy Larger groups require right-handed neutrinos. Mass suppressed by see-saw. What to do with quadratic divergencies? They are canceled in SUSY Why large hierarchy between Planck scale and electroweak scale? Why quark charges 1/3(/3) o lepton charges? Connected by radiative corrections in Supersymmetry Connected in uniied theories 3

4 Precise measurements o couplings at LEP-> Uniication in SUSY 4

5 On the citation list.. 5

6 Constrained Minimal Supersymmetric Model (MSSM) Mass uniication at GUT scale: m 0 or scalars m 1/ ür S=1/ gauginos m 1,m or Higgs Lightest Supersymmetric Particle =LSP =Neutralino ( Photino S=1/ Photon) m <0 by radiative corr. mtop m <0 at electroweak scale or 140<mtop<00 GeV. BINGO, mtop predicted by SUSY BEFORE observation mtop = 171 ± 1.3 GeV So SUSY connects, MGUT, mtop and m Z correctly and predicts Higgs mechanism with lightest Higgs around 10 GeV (and it its LEP electroweak data) 6 6

7 Phenomenology studied together with Dmitri Top constraint solutions: low tanβ high tanβ Triple uniication at large tanβ Quasi-ixed endpoints-> In SUSY mtop, mb,mtau indep. o initial GUT conditions Dubna SUSY 001 db,grimm,kazakov,gladyshev, PLB, hep-ph/ v3 Log Q 7

8 10 years ago WdB, M.Huber, C. Sander and D.I Kazakov, A Global Fit To g- and bsgamma In The CMSSM, PLB 515 (001) 83. b->sγ 001 b->sγ 011 SM: EXP: SM: 3.15(3).10-4 EXP: 3.55(4) : b sγ <SM, as expected or µ>0 rom g- and A 0 =0 011: : b sγ >SM -> tension 8

9 Dubna SUSY Con

10 Dubna SUSY Con

11 Visiting KARLSRUHE 11

12 1

13 CMS limits on SUSY parameter space arxiv: gg 700 GeV gq 700 GeV qq squark and gluino masses above around 700 GeV at 95% CL Electroweak production dominates (pp->) 13

14 Strongest constraint rom cosmology: WIMP annihilation cross section Thermal equilibrium abundance Actual abundance Comoving number density Gary Steigmann T=M/ x=m/t T>>M: +->M+M; M+M->+ T<M: M+M->+ T=M/: M decoupled, stable density (when annihilation rate expansionrate, i.e. Γ=<σv>n(x r ) H(x r )!) WMAP -> Ωh =0.113± > <σv>=.10-6 cm 3 /s DM increases in Galaxies: 1 WIMP/coee cup 10 5 <ρ>. DMA ( ρ ) restarts again.. Annihilation into lighter particles, like quarks and leptons -> π 0 s -> Gammas! Only assumption in this analysis: WIMP = THERMAL RELIC! 14

15 15 Relic Density Constraint determines tanβ! m 1/ m m A A A W W + i + Z Z i W W + i + W W + i + Z Z i Z Z i Z _ Z _ 4 tan m A β σν Problem: or excluded irst diagram too small. Last 3 diagrams also small can get correct relic density by m A s-channel annihilation q m m A can be tuned with tanβ or any m 1/ tanβ 50 (see next slide) arxiv:

16 Relic Density Constraint Dependence on tanβ V tree ( ) ( ) ( ) + H H = m H + m H m H H + h. c. + H H + H H 1, 1 1 m A = m1 + m (Tree Level) m 1 running mtop m running mb tan β small m A or tanβ= m t /m b 50 Fit o Ωh determines m A and tanβ 3 1 g + g 8 1 g 1 tanβ 50 Co-annihilation m A m 1/ arxiv:

17 m A cross sections tanβ Beskidt, db, Kazakov, , PLB

18 What about Higgs m A limit? tanβ 50 arxiv: (CMS PAS HIG ) Atlas similar For tanβ 50 m A > 440 GeV 18

19 B s μμ depends on tan 6 β and A 0 arxiv:hep-ph/003069v arxiv: Stop mass dierence Becomes small, i t 1 t can be achieved by adjusting A t, till mixing term (A t μ/tanβ) becomes small. Important only or light SUSY masses (see blue region) 19

20 I both, A 0 and tanβ, varied, little exclusion rom Bs->µ µ 95% CL excluded 95% CL excluded B s < arxiv: Hypothetical limit: B s < (x SM) Limits rom Bs->µµ smaller than limits rom direct searches/cosmology 0

21 95% CL exclusion rom cosmology/ew Allowed parameter space (95% CL contour) in the m 0 -m 1/ plane including all constraints g- + b sγ m h all constraints 1

22 95% C.L. exclusion contours in 011 allowed Cosmo/EW ( =5.99, m g 1 TeV LHC Higgs combined with cosmology arxiv: LHC direct Searches (CMS-SUS ) (Atlas similar)

23 Direct Detection o WIMPs 0 0 Experimental limit has uncertainties rom assumptions on halo clumpiness, rotation Theoretical prediction has uncertainties on nuclear orm actors (actor 5-10) 3

24 Including Direct Dark Matter Search rom Xenon-100 arxiv: Problem: N scattering cross sections depends on orm actors Lattice has strange quark content in nucleus similar to light quarks (arxiv: v3) To be conservative use the smaller orm actor-> excluded region small! preliminary allowed minimum p u p d p s = 0.0; = 0.06; = 0.0; arxiv: v maximum p = 0.03; u p d p s = 0.033; = 0.6; n u p d p s = 0.014; = 0.036; = 0.0; n u p d p s = 0.018; = 0.04; = 0.6; Red=95% C.L. excluded by combined EW / Higgs limits 4

25 Supersymmetry in Particle Physics and Cosmology hep-ph/94066 Possible evolution o the universe with GUT scale breaking into SU3xSUxU1 ater s -> Inlation reeze-out o SUSY ater ew ps reeze-out o electroweak interactions ater ew µs. 5 5

26 0 ± 0 q q g 6