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Dark Matters: WIMP and Beyond

Dark Matters: WIMP and Beyond. Shufang Su U. of Arizona SI 2005. Outline. -. Brief introduction of standard cosmology Dark matter evidence New physics and dark matter WIMP candidates: neutralino LSP in MSSM, lightest KK particle in UED

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Dark Matters: WIMP and Beyond

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  1. Dark Matters:WIMP and Beyond Shufang Su U. of Arizona SI 2005

  2. Outline - • Brief introduction of standard cosmology • Dark matter evidence • New physics and dark matter • WIMP • candidates: • neutralino LSP in MSSM, lightest KK particle in UED • direct/indirect DM searches, collider studies • synergy between cosmology and particle physics • superWIMP

  3. Standard cosmology - • Einstein equations • Metrics a(t): scale factor k: -1, 0, 1 for open, flat, close universe • Equations of state

  4. Standard cosmology - Friedmann equation Hubble parameter critical density

  5. We are living through a revolution in our understanding of the Universe on the largest scales For the first time in history, we have a complete picture of the Universe

  6. DM evidence: rotation curves Vc» const NGC 2403 Dark matter in halo Vc» 1/r - Rotation curves of galaxies and galactic clusters Constrain m i=i/c

  7. Dark matter evidence: supernovae - Supernovae Constrain m-

  8. Dark matter evidence: CMB - Cosmic Microwave Background Constrain +m then now

  9. Synthesis - » 0.5% » 0.5% =3% =23% § 4% =73% § 4% • Remarkable agreement • Remarkable precision (~10%)

  10. Dark matter vs. dark energy - We know how much, but no idea what it is.

  11. 富士山 Dark Energy Seven station Dark Matter Five station Ordinary matter

  12. CDM requirements Standard Model - Stable  Non-baryonic  Neutral  Cold (massive) Correct density Gravitational interacting • Not for cosmology observations • Dark Matter • Cosmology constant • Baryon asymmetry … SM is a very successful theoretical framework describes all experimental observations to date No good candidates for CDM in SM

  13. New physics beyond SM - DM problem provide precise, unambiguous evidence for new physics Independent motivation for new physics in particle physics • New physics to protect electroweak scale • new symmetry: supersymmetry • new space dimension: extra-dimension • …

  14. Dark matter in new physics • there are usually many new weak scale particle • constraints (proton decay, large EW corrections) discrete symmetry stability good dark matter candidate - Dark Matter: new stable particle in many theories, dark matter is easier to explain than no dark matter

  15. Dark matter candidates - Many ideas of DM candidates: • superWIMPs • WIMP • primodial black holes • axions • warm gravitinos • Q balls • wimpzillas • self-interacting particles • self-annihilating particles • fuzzy dark matter • branons • … • appear in particle physics models motivated independently by attempts to solve Electroweak Symmetry Breaking • relic density are determined by mpl and mweak • naturally around the observed value • no need to introduce and adjust new energy scale mass and interaction strengths span many, many orders of magnitude

  16. Dark matter freeze out  ff expansion ff - Thermal equilibrium $ ff Boltzmann equation Universe cools: n=nEQe-m/T WIMP =n hvi v.s. H Freeze out, n/s » const • early time  H n ¼ neq • late time H (n/s)today» (n/s)decoupling • at freeze-out ¼H TF» m/25 Approximately, relic/ 1/hvi

  17. Relic density calculations - Boltzmann equation number density at thermal equilibrium entropy

  18. Relic density calculations - Define Long before freeze-out Long after freeze-out

  19. Relic density calculations - Approximately, relic density today ( ) g*: number of relativistic degrees of freedom at the time of freeze out xF: freeze out temperature g: degrees of freedom for dark matter X c: O(1) constant determined by matching the late-time and early-time solutions Or, order of magnitude estimation: Resonance enhancement, coannihilation …

  20. WIMP dark matter - WIMP: Weak Interacting Massive Particle • mWIMP» mweak • an»weak2 mweak-2   h2» 0.3 naturally around the observed value

  21. CDM requirements Minimal Supersymmetric Standard Model (MSSM) - Spin differ by 1/2 SM particle superpartner » » » » Stable » »  Non-baryonic » » »  Neutral  Cold » » » m > 45 GeV » » » Correct density » weak interaction • gravitational interacting » » » » Supersymmetry breaking, m » TeV

  22. super-partners ~ ~ ~ ~ B0, W0, Hd0, Hu0 proton decay Superpartner of gauge bosons Superpartner of Higgs bosons R-parity: SM particle +super-partner - lightest supersymmetric particle (LSP)stable LSP  SM particle, LSP  super particle  neutralinos i0, i=1…4 mass eigenstates Neutralino LSP: 10 as Dark Matter Neutralino LSP as DM - • new weak scale particle • constraints discrete symmetry stability dark matter candidate

  23. /l W/Z /l/q Z ~ ~ ~ ~ ~ ~        /l/q /l W/Z ~ f • light sneutrino: 45-200 GeV  low abundance • heavy sneutrino: 550 – 2300 GeV  0.1    1 • disfavored on theoretical ground • excluded by nuclear recoil direct detection: m¸ 20 TeV ~ Sneutrino Dark Matter - rapid annihilation, hAvi large Sneutrino CDM in MSSM is disfavored

  24. Neutralino relic density f W + ~ ~ 10 10 10 10 10 10 W f ~ ~ f absent for B0 /l/q Z,H /l/q - 0.1 h2  0.3 (pre-WMAP) • t-channel • (dominate) CMSSM • Cosmology excludes much of the parameter space  too big • cosmology focuses attention on particular regions  just right • s-channel important near pole m» mZ,H/2

  25. Bulk region and coannihilation region • Other constraints • b ! s  : » 10-4 exclude small m1/2 important for  <0  m» m +X ! +Y in equilibrium  decays into  eventually Co-annihilation:, ,  ~ b s ~ me=99GeV ~ ~ ~ ~ ~ b ! s  - Ellis et. al. (2003) CMSSM 0.1 h2  0.3 0.094 h2  0.129 • muon g-2 th-exp=(26 § 16)£ 10-10 co-annihilation bulk

  26. Focus Point Region (100 GeV)2 - ~ Feng et. al. (2000)

  27. Funnel-Like Region l/q ~ ~ A,H 10 10 l/q / 1/hvi hvi» 1/(4m2 – mA,H2)2 too big   too small - Large tan : m» mA,H/2 Ellis et. al. (2003)

  28. Bulk field: KK tower m2 = n/R2 … SM 3 3/R2 2/R2 2 1 1/R2 0 Extra dimension - • Universal extra dimension: • All SM particles live in the (flat) bulk • unwanted states: orbifold 4D Appelquist, cheng and Dobrescu (2000)

  29. KK modes of SM particle momentum conservation in compactified dimension + orbifolding KK-parity: odd level KK particles - lightest KK state (LKP)stable LKP, likely to be 1st excitation of hypercharge gauge boson B(1) Universal Extra Dimension - • new weak scale particle • constraints discrete symmetry stability dark matter candidate

  30. UED: LKP Dark Matter - Servant, Tait (2002)

  31. Dark matter detection DM DM f f Cross symmetry f f DM DM DM scattering Efficient scattering now direct DM direction Efficient annihilation now indirect DM direction - DM annihilation • / 1/hi Not overclose universe  Efficient annihilation then

  32. Direct detection DM scattering cross section (particle) Number of target nuclei in detector Local WIMP density (astro) - Measure nuclear recoil energy (ionization, photo…) detector

  33. Direct detection DAMA Signal and Others’ Exclusion Contours CDMS DAMA CDMS EDELWEISS CDMS II WIMP CDMS (2004) -

  34. Direct detection: future - Current Sensitivity Near Future Future Baer, Balazs, Belyaev, O’Farrill (2003) B(1) LKP DM Theoretical Predictions

  35. Indirect detection DM DM Dark Matter annihilates in (amplifier) to, a place some particles which are detected by. an experiment recipe - A/nDM2 detector

  36. Dark Matter annihilates in center of the sun to neutrinos , a place some particles which are detected byAMANDA, ICECUBE. an experiment recipe  earth  Dark matter density in the sun, capture rate

  37. Indirect detection: neutrino - MSSM UED icecube Hooper and Wang (2003) Hooper and Krib (2002)

  38. Dark Matter annihilates in galactic center to photons , a place some particles which are detected byGLAST, HESS. an experiment recipe HESS Dark matter density in the center of the galaxy

  39. Indirect detection: gamma ray MSSM EGRET GLAST - UED Hooper and Wang (2003)

  40. Dark Matter annihilates in the halo to positions , a place some particles which are detected byAMS on the ISS. an experiment recipe Dark matter density profile in the halo AMS

  41. Comparison of pre-LHC SUSY searches - LHC search DM search Pre-WMAP Post-WMAP • DM searches are complementary to collider searches • When combined, entire cosmologically attractive region will be explored before LHC ( » 2007 )

  42. Collider study of dark matter Tevatron p - p p p - Can study those regions at colliders LHC ILC Now 2007 Precise determination of new particle mass and coupling  Determine DM mass, relic density

  43. Neutralino DM in mSUGRA - Choose four representative points for detailed study Baer et. al. ISAJET Gondolo et. al. DarkSUSY Belanger et. al. MicroMEGA Feng et. al. ILC cosmology working group

  44. Bulk region LCC1 (SPS1a) - M0, m1/2, A0, tan = 100, 250, -100, 10 ( >o, m3/2>mLSP ) light 10, 20, 1§, slepton • Scan over » 20 most relevant parameters • compute h2, weigh each point by Gaussian distribution for each observable • width of pdf  h2 Weiglein, Martyn et. al. (2004)

  45. Relic density determination: LCC1 LHC (“best case scenario”) ILC WMAP (current) Planck (~2010) - (preliminary) result: / = 2.2% (  h2 = 0.0026 ) LCC1 Battaglia (2005)

  46. Foucs point region: LCC2 ILC Planck WMAP - M0, m1/2, A0, tan =3280, 300, 0, 10 ( >o, m3/2>mLSP ) light neutralino/chargino LCC2 LCC2 Battaglia (2005) (preliminary) result: / = 2.4% (  h2 = 0.0029 )

  47. Coanniliation region: LCC3 ILC Planck WMAP - M0, m1/2, A0, tan =210, 360, 0, 40 ( >o, m3/2>mLSP ) m» mstau LCC3 Battaglia (2005) (preliminary) result: / = 7% (  h2 = 0.0084 )

  48. parts per mille agreement for  discovery of dark matter local DM density and velocity profile eliminate particle physics uncertainty do real astrophysics Synergy - Collider Inputs Weak-scale Parameters DM Annihilation DM-N Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs

  49. Alternative dark matter CDM requirements Stable  Non-baryonic  Neutral  Cold (massive) DM -1  (gravitational coupling)-2 Correct density Gravitational interacting (much weaker than electroweak) • too small • DM too big overclose the Universe - All of the signals rely on DM having EW interactions. Is this required? NO! But the relic density argument strongly prefers weak interactions.  

  50. superWIMP 106 - WIMP  superWIMP + SM particles Feng, Rajaraman and Takayama (2003) 104 s  t  108 s SWIMP WIMP SM superWIMP e.g. Gravitino LSP LKK graviton WIMP • neutral • charged

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