Dark Matter

1
Dark Matter

• Expect Unexpected outside LHC

Jingsheng Li
2
Introduction

• SM is confirmed precisely?
• NO!
• Dark Matter is OUT THERE!!
• SCSMmore
• ?(New Phyptcint)
  unexpected
• 
  ?astrophy effect?
• 
  ? modify gravity?

3
Outline

• Standard Cosmology
• Evidence for Dark Matter
• Relic Density
• Candidates
• Dark Matter Detection

4
Standard Cosmology

• Smooth Universe
• Friedman Eqn
• Content ( w?/P, )
• baryon w0 radiation
  w1/3 c.d.m. w0 c.c.
  w-1

5
A Brief History of Universe

6
Properties of DM

• Dark (rotation curve, gra. lensing)
• Cold (Structure formation)
• Weakly Interacting (rotation curve, Bullet
  Cluster)
• ?b/?m1/6 (BBN, CMB, Bullet Cluster 1E0657-558)

7
Evolution of CDM

• Boltzmann Eqn (12?34)
• Note
• Eq (Tgtm), freeze out (Tltm)

8
Relic Density

9
Lee-Weinberg Bound

• Anti-baryon
• 45GeV ?L
• Scalar DM Higgs exchange, even weaker,
  expect for Boehm, Fayet
  (N2)

• Lee-Weinberg is good for gtGeV range

10
Candidate VS Test
Gra Lensing Lee-WeinbergZ width Direct Search PAMELA/ATIC
MACHOs X
Anti-Baryon X
SM ?L X
MSSM X
Neutralino ? X?
Gravitino -- ?
Axion -- ?
UED w/ KK-parity, LH w/ T-parity, Techni Baryon,
monopole, ?R.
11
SUSY WIMP

• SUSY w/ R-parity provides LSP
• Spctrum depends on Mediation Scheme
• Hidden Sector
• GMSB gravitino as LSP, cosmo constraint
  
• NLSP decay, BBN and CMB constraints
• Gravity Mediated , decay, BBN
  constraint
• Neutralino as LSP In Lee-Weinberg bound

12
Neutralino

• Decay channels
• ?univ10Gyr, set upper bound for ?Mh2lt0.3,lower
  bound for ?, upper bound for mint.
• Cosmology set upper bound on superpartner, good
  for LHC?

13
Axion (non-thermal CDM)

• PQ SSB?Axion
• PQ EB ?
• Coupling to Nucleon
• Red Giant emission bound
• SN1987A bound
• Oscillation energy
• Critical density bound
• Search

14
Detection

• MET
• Direct Detection
• Indirect Detection

15
Direct Detection
Type Scintillator Cryogenic Crystal Noble Liquid
matterial NaI, CsI Ge, Si Ar, Xe
Pro Normal T Distinguish e / N New tech, potential
Con Background ? Low T,
Exp DAMA CDMS XENON
Result Solar modulation
16
Indirect Detection
Annihilation at Center of Sun Galaxy Center Halo
in to ? ? e
detected by AMANDA, IceCube GLAST, HESS, INTEGRAL AMS, HEAT, PAMELA, ATIC
Result 511KeV from bulge excess
17
Result from indirect detection

• e excess beyond prediction10 GeV 100GeV
  (PAMELA), ee- excess upto TeV (ATIC)
• ATIC sharp falling _at_ 600GeVno astrophy
  explaination
• SUSY needs 10TeV for PAMELA
• No p- excess
• Usual Neutralino cant explain
• Very large lt?vgt, conflicts with required relic
  density.

18
Solution?

• New interaction to annihilate ?
• Sommerfeld enhancement (Arkani-Hamed)Breit-Wigner
  enhancement (Murayama)Nonthermal production
  (Kumar)
• DM decay