1. Dark Matter Explanation in Singlet Extension of MSSM
Jin Min Yang
杨 金 民
Institute of Theoretical Physics, Academia Sinica, Beijing
中国科学院 理论物理研究所
国立清华大学

2. Outline 1. Dark Matter: Relic Density & Pamela
2. SUSY models: MSSM & Singlet Extension
3. Explanation of Dark Matter in SUSY
& Implication on Higgs Physics
4. Conclusion

3. 1. Dark Matter Relic Density DMh2 ~ 0.1: WMAP
  0.4 H/cm3
V  220 km/s
Cosmic Ray Anomalies: PAMELA
ATIC
Fermi

4. PAMELA _ e+ p

5. ATIC/Fermi
ATIC
Fermi

6. to explain dark matter relic density:
-- thermal production in early universe
to explain PAMELA:
-- dark matter annihilation
-- dark matter decay
-- astrophysical (pulsar …)

7. to explain dark matter relic density:
-- thermal production in early universe
freeze-out
to explain PAMELA:
-- dark matter annihilation
Pamela >> freeze-out
annihilate dominantly to leptons

8. 2. SUSY Models R-conserving SUSY Models · · · ·
MSSM , CMSSM (mSUGRA, …)
NMSSM
nMSSM
· · · ·
NMSSM
MSSM
nMSSM
GMSSM
R-violating SUSY Models

9. MSSM Singlet Extension general singlet extension ( NMSSM, nMSSM, …)
-problem
little hierarchy
general singlet
extension

10. motivated from top-down view ?
E6 models (superstring-inspired)
string scale
SO(10)  U(1)  …
at low energy: S, Hu, Hd + heavy particles

11. MSSM + singlet MSSM + Fields: Spectrum:
One more CP-odd Higgs (A1 or a )
MSSM +
One more CP-even Higgs (h)
One more neutralino
3 CP-even Higgs bosons
2 CP-odd Higgs bosons
5 neutralinos

12. 3. Explain Dark Matter in SUSY
In MSSM: LSP   WIMP :

13. final states: gauge bosons, fermion pairs, …
relic density: -  f A  f
final states: gauge bosons, fermion pairs, …
cross section:
freeze-out (weak)
cannot explain PAMELA (   …) 
Pamela >> freeze-out
annihilate dominantly to leptons

14. To explain relic density + PAMELA:
How about singlet extensions of MSSM ?
Like MSSM,
NMSSM, nMSSM, …. (with discrete symmetry)
can explain relic density but not PAMELA !
Because relic density + other expts
LSP  mass in a narrow range
No particle so light to give Sommerfeld enhance

15. (1) Relic density (WMAP)
(2) Direct bounds: LEP1, LEPII, Tevatron
NMSSM
nMSSM
(3) Precision Electroweak Data
1 , 2 , 3 (S, T, U)
(4) Rb = (Zbb)/  (Zhadrons)
(5)  g-2 a
(6) Stability of Higgs Potential

16. NMSSM
arXiv: , in PRD ( Cao, Yang)  

17. nMSSM
arXiv: , in PRD(R) (Cao, Logan, Yang) 

18. General singlet extension of MSSM:
arXiv: (Hooper, Tait)
arXiv: , in JHEP  (Wang, Xiong, Yang, Yu)  
Final states
h ~ GeV, a < 0.5 GeV
singlet-like
Sommerfeld enhancement

19. h ~ GeV , a < 0.5 GeV
arXiv: , in JHEP  (Wang, Xiong, Yang, Yu)

20. arXiv: 0908.0486, in JHEP  (Wang, Xiong, Yang, Yu)

21. Sommerfeld enhancement
arXiv: , in JHEP  (Wang, Xiong, Yang, Yu)

22. PAMELA
Hooper, Tait

23. Implication on SM-like Higgs decay:
arXiv: , in JHEP  (Wang, Xiong, Yang, Yu)

24. are supressed other visible modes (like )
arXiv: , in JHEP  (Wang, Xiong, Yang, Yu)

25. 4. Conclusion MSSM NMSSM, nMSSM General singlet extension
Precision Electroweak Data Rb
 g-2
Dark Matter Relic Density
General singlet extension
PAMELA
Exotic hSM decay
testable at LHC