1. SUSY Dark Matter in light of CDMS/XENON Results
Jin Min Yang
Institute of Theoretical Physics, Beijing
arXiv: , in PRD(R)
arXiv: , in JHEP
With Cao, Hikasa, Wang, Yu
, Tsinghua Univ

2. Outline Introduction: SUSY—Dark Matter—Higgs
2 Experimental Constraints on SUSY
2.1 Collider Constraints
2.2 Dark Matter Constraints
3 Currently Allowed SUSY Parameter Space
4 Implication for LHC Higgs Search
5 Conclusion

3. 1. Introduction SUSY Higgs Boson Dark Matter
In the following I will give a very brief discussion

4. standard non-standard theory – D. Gross
1.1 About SUSY
standard non-standard theory – D. Gross
Edward Witten
International Conference on String Theory, Beijing, (Aug 17, 2002)

5. David Gross August 17, 2002 Supersymmetry 1028ev 1012ev LHC ENERGY
SRTRENGTH
STRONG OF
FORCE
Supersymmetry
WEAK
UNIFICATION
ELECTRO
Planck Scale
GRAVITY
1028ev
1012ev
Present day observation
LHC
ENERGY

6. -- M. E. Peskin
ITP, Beijing, Aug. 2010

7. SUSY Models: · · · · MSSM nMSSM Split-SUSY mSUGRA
So we see exploring SUSY is very important !
Different models give different phenomenology
MSSM
NMSSM
nMSSM
Split-SUSY
mSUGRA
· · · ·
SUSY
Models:
MSSM
SUSY
nMSSM
NMSSM

8. 1.2 SUSY Dark Matter: a miracle !
a byproduct of SUSY  DM ~ 0
(a perfect WIMP ) 1
Perfect candidate for DM
Naturally give correct relic density
A miracle !

9. 1.3 Higgs Bosons ---SUSY is the paradise of Higgs SM
(only one Higgs boson)
Will be found at LHC !

10. h, H, A, H SUSY (more than 5 Higgs) How many can be seen at LHC ?
---depending on parameter space
Which part is chosen by nature ?
---current experimental constr.

11. 2 Experimental Constraints on SUSY
direct bounds (LEPI, LEPII, Tevatron)
EW (S,T,U) Rb
B-decays
muon anomalous a
meet all constraints
at 2- level
dark matter DM
CDMSII/XENON
     

12. 2.1 Collider Constraints (1) Direct Bounds: LEP I LEP II Tevatron

13. b s (2) Precision EW Data S, T, U Rb (3) a   
SUSY
(3) a  
SUSY 
(4) B-decays and mixings b s 

14. Universe cools: n=nEQe-m/T
2.2 Dark Matter Constraints
Relic Density (WMAP)
Thermal equilibrium
  ff
Universe cools: n=nEQe-m/T
(i) Lightest nurtralino
solely composes
cosmic dark matter
Freeze out
(ii) Relic density in 2 range
(not only upper bounded)
1018 秒

15. CDMS-II/XENON Limits:

16. We do not consider Cosmic Ray Anomaly (PAMELA, ATIC, ···)
as constraints on SUSY
Anyway, they can be explained by pulsars

17. Currently Allowed SUSY Parameter Space
Scan over parameter space

18. CDMS-II already make sense in testing SUSY!
Red: CDMS-II covered region
Blue: SuperCDMS(25kg)/XENON100 (6000 kg-day)
Green: beyond SuperCDMS/XENON100
CDMS-II already make sense in testing SUSY!

19. LSP (DM) property
bino-like
singlino-like
CDMS/XENON will push LSP more bino-like

20. CDMS-II push LSP (DM) more bino-like
CDMS/XENON push up  value
higgsino component decrease
bino component increase

21. CDMS/XENON push up chargino (finally 2*LSP)

22. CDMS/XENON push up charged-Higgs

23. SM-like Higgs may decay to DM

24. How about split-SUSY ?

25. 4 Implication for LHC MSSM-Higgs Search
charged-Higgs: almost unaccessible
ATLAS

26. neutral-Higgs (H,A) at LHC
CMS

27. 5. Conclusion
(i) Current CDMS-II/XENON100 limits can exclude some parameter
space which survive the constraints from dark matter relic density
and various collider experiments: push up charged-Higgs, chargino
push LSP more bino-like
(ii) Future SuperCDMS/XENON100 (6000 kg-days exposure) will
significantly tighten the parameter space in case of null results
(iii) Currently, in allowed parameter space:
charged Higgs is hardly accessible at LHC
neutral non-SM Higgs bosons may be accessible in some
allowed region characterized by a large mu
Future SuperCDMS/XENON100 limits will further push away
non-SM Higgs bosons at the LHC
(iv) Interplay of LHC and CDMS/XENON: a good test for SUSY !
Thanks !