1. SUSY Dark Matter Collider – direct – indirect search bridge. Sabine Kraml Laboratoire de Physique Subatomique et de Cosmologie Grenoble, France ● 43. Rencontres de Moriond La Thuile, 1-8 March 2008

2. Moriond EW 20082 S. Kraml: SUSY dark matter WIMP paradigm DM should be stable, electrically neutral, weakly and gravitationally interacting  WIMPs ― weakly interacting massive particles WIMPs are predicted by most theories beyond the Standard Model (BSM) Stable as result of discrete symmetries Thermal relic of the Big Bang Testable at colliders! Neutralino, gravitino, axino, lightest KK state, T-odd little Higgs, etc.,... BSM-DM c.f. talk by M. Tytgat

3. Moriond EW 20083 S. Kraml: SUSY dark matter let‘s go SUSY...

4. Moriond EW 20084 S. Kraml: SUSY dark matter What is SUSY?  Supersymmetry (SUSY) is a symmetry between fermions and bosons.  The SUSY generator Q changes a fermion into a boson & vice versa  Extension of space-time to include anticommuting coordinates x  → (x ,   ) with         This combines the relativistic “external” symmetries (such as Lorentz invariance) with the “internal” symmetries such as weak isospin.  Actually the unique extension of the Poincare algebra * * (the algebra of space-time translations, rotations and boosts)

5. Moriond EW 20085 S. Kraml: SUSY dark matter space-time symmetry (special relativity) Antiparticles space-time supersymmetry Superpartners doubling of the spectrum

6. Moriond EW 20086 S. Kraml: SUSY dark matter The beauties of SUSY  Unique extension of relativistic symmetries  Solution to gauge hierarchy problem  Radiative EW symmetry breaking, light Higgs  Gauge coupling unification  Ingredient of string theories  Very rich collider phenomenology  Cold dark matter candidate ....

7. Moriond EW 20087 S. Kraml: SUSY dark matter SUSY as a local gauge theory includes a spin-2 state, the graviton (!) and its superpartner the gravitino. Minimal Supersymmetric Standard Model (MSSM) gluino 2 charginos  ± 4 neutralinos   If SUSY comes with a new conserved parity, R P, then the lightest SUSY particle (LSP) is stable  DARK MATTER CANDIDATE Gravitino, sneutrino or lightest neutralino

8. Moriond EW 20088 S. Kraml: SUSY dark matter I am concentrating on the neutralino case. For gravitino DM, see talk by F. Steffen tomorrow morning

9. Moriond EW 20089 S. Kraml: SUSY dark matter SUSY searches at the LHC CMS

10. Moriond EW 200810 S. Kraml: SUSY dark matter 0101 Z q q 0202 jet jets, l + l − missing energy Large cross sections  ~100 events/day for M ~ 1 TeV Spectacular signatures  SUSY could be found early on Cascade decays into LSP lead to typical signature: multi-jets / multi-leptons plus large missing energy SUSY @ LHC Every SUSY event → 2 LSPs. Abundant production! LHC as DM factory

11. Moriond EW 200811 S. Kraml: SUSY dark matter Mass measurements: cascade decays E T miss → no peaks → mass reconstruction through kinematic endpoints [ATLAS, G. Polesello] Typical precisions: a few %

12. Moriond EW 200812 S. Kraml: SUSY dark matter Neutralino annihilation:   LSP as thermal relic: relic density computed as thermally avaraged cross section of all annihilation channels →  h 2 ~  v  −1

13. Moriond EW 200813 S. Kraml: SUSY dark matter Consequences 1. 0.094 <  h 2 < 0.136 puts strong constraints on the parameter space of any model variant CMSSM: GUT-scale boundary conditions: m 0, m 1/2, A 0, plus tanb, sgn(  )

14. Moriond EW 200814 S. Kraml: SUSY dark matter Consequences 1. 0.094 <  h 2 < 0.136 puts strong constraints on the parameter space of any model variant good  h 2 Simple SO(10) SUSY GUTs: dual requirement of Yukawa unification and DM relic density is extremley predictive → Very distinct LHC signatures: ~500 - 600 GeV gluinos 50-75 GeV  1 talk by S. Sekmen in YSF2

15. Moriond EW 200815 S. Kraml: SUSY dark matter Consequences 1. 0.094 <  h 2 < 0.136 puts strong constraints on the parameter space of any model variant 2. If we can measure the properties of the SUSY particles precisely enough, then we can compute  v of the LSP → „collider prediction“ of  h 2 → compare with cosmological observations Note: this means measuring (or at least putting limits on) masses and couplings of most of the SUSY spectrum to infer

16. Moriond EW 200816 S. Kraml: SUSY dark matter Consequences 1. 0.094 <  h 2 < 0.136 puts strong constraints on the parameter space of any model variant 2. If we can measure the properties of the SUSY particles precisely enough, then we can compute  v →  h 2 3. We can also compute the direct and indirect detection rates direct detection: m ,  N  v, local DM density indir. det.: v→0, density profile, propagation model

17. Moriond EW 200817 S. Kraml: SUSY dark matter However, uncertainties in   N calculation are large (~50%) Direct detection: limits and predictions Xenon10 new CDMS result! Predictions of various SUSY models

18. Moriond EW 200818 S. Kraml: SUSY dark matter Indirect searches: high energetic positrons or gamma rays from  annihilation

19. Moriond EW 200819 S. Kraml: SUSY dark matter Indirect detection: EGRET signal? [W. DeBoer, arXiv:0711.1912] 50–70 GeV neutralino? EGRET

20. Moriond EW 200820 S. Kraml: SUSY dark matter Higgs? SUSY? 1 GeV ~ 1.3 * 10 13 K „It is impossible to overestimate the importance of discovering dark matter at the LHC. Such a discovery will imply a revision of the SM, it will strenghten the connection between particle physics, cosmology and astrophysics, and it will enormously enlarge our understanding of the present and past universe.“ G.F. Giudice, Theories for the Fermi Scale (2007)