Shufang Su • U. of Arizona Dark Matters Shufang Su • U. of Arizona

For the first time in history, 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 S. Su Dark Matters

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

Dark matter evidence: supernovae - Supernovae then now Constrain m- S. Su Dark Matters

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

Synthesis Remarkable agreement Remarkable precision (~10%) -  » 0.5%  » 0.5% =3% =23% § 4% =73% § 4% Remarkable agreement Remarkable precision (~10%) S. Su Dark Matters

Dark matter vs. dark energy - We know how much, but no idea what it is. Dark matter Dark energy No known particles contribute All known particles contribute Probably tied to mweak » 100 GeV Probably tied to mPlanck » 1019 GeV Several compelling solutions No compelling solutions S. Su Dark Matters

Not for cosmology observations Standard Model - CDM requirements Quarks u c t d s b  Stable  Non-baryonic Leptons e   e    Neutral  Cold (massive)  Correct density Gauge boson (force carrier)  W§,Z g  Gravitational interacting Higgs H 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 S. Su Dark Matters

New physics beyond SM - DM problem provide precise, unambiguous evidence for new physics Independent motivation for new physics in particle physics S. Su Dark Matters

New physics beyond SM - SM is an effective theory below some energy scale  » TeV Hierarchy problem Naturalness problem (1019 GeV)2 H  (100 GeV)2 (mH2)physical ¼ (mH2)0 + 2 mplank 1019 GeV -(1019 GeV)2 precise cancellation up to 1034 order mEW 102 GeV New physics to protect electroweak scale new symmetry: supersymmetry new space dimension: extra-dimension … S. Su Dark Matters

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

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 S. Su Dark Matters

Universe cools: N=NEQ=e-m/T WIMP dark matter - WIMP: Weak Interacting Massive Particle Thermal equilibrium  $ ff Universe cools: N=NEQ=e-m/T WIMP WIMP » 1 hani mWIMP» mweak an » weak2 mweak-2 naturally around the observed value Freeze out, N » const S. Su Dark Matters

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

Others’ Exclusion Contours Direct detection - DM DAMA Signal and Others’ Exclusion Contours CDMS (2004) DAMA CDMS II CDMS EDELWEISS WIMP CDMS Measure nuclear recoil energy detector S. Su Dark Matters

Direct detection: future - Current Sensitivity Near Future Future Theoretical Predictions Baer, Balazs, Belyaev, O’Farrill (2003) S. Su Dark Matters

Indirect detection a place some particles Dark Matter annihilates - DM DM Dark Matter annihilates in to , a place some particles which are detected by . an experiment recipe detector S. Su Dark Matters

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

a place some particles Dark Matter annihilates in galactic center to photons , a place some particles which are detected by GLAST, HESS. an experiment recipe HESS Dark matter density in the center of the galaxy S. Su Dark Matters

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

Minimal Supersymmetric Standard Model (MSSM) - Spin differ by 1/2 SM particle superpartner CDM requirements » » » Squarks u c t d s b »  Stable » »  Non-baryonic » » »  Neutral sleptons e   e    Cold » » » m > 45 GeV » » »  Correct density » Gauginos B0 W§,W0 g weak interaction gravitational interacting » » » » Higgsino (Hu+,Hu0) , (Hd0, Hd-) Supersymmetry breaking, m » TeV S. Su Dark Matters

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

Neutralino relic density - 0.1  h2  0.3 (pre-WMAP) CMSSM Cosmology excludes much of the parameter space  too big cosmology focuses attention on particular regions  just right S. Su Dark Matters

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

Parts per mille agreement for   discovery of dark matter Relic density determination - Feng et. al. ILC cosmology working group ILC LHC (“best case scenario”) Planck (~2010) WMAP (current) LCC1 Parts per mille agreement for   discovery of dark matter S. Su Dark Matters

Comparison of pre-LHC SUSY searches LHC seeach 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 ) S. Su Dark Matters

Synergy Collider Inputs Weak-scale Parameters DM Annihilation DM-N Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs S. Su Dark Matters

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

superWIMP WIMP  superWIMP + SM particles 104 s  t  108 s SM - 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 106 S. Su Dark Matters

Superpartner of graviton superWIMP : an example - change light element abundance predicted by BBN Strong constraints ! SUSY case WIMP  superWIMP + SM particles Charged slepton Superpartner of lepton Gravitino Superpartner of graviton WIMP superWIMP SM particle » 1 mpl2 Decay lifetime  planck mass S. Su Dark Matters

BBN constraints ? Big bang nucleosynthesis - Feng, Rajaraman, Takayama (2003) Cosmological signals: BBN, CMB Big bang nucleosynthesis /10-10 = 6.1 0.4 Fields, Sarkar, PDG (2002) ? S. Su Dark Matters

superWIMP in mSUGRA Usual WIMP allowed region superWIMP allowed region - BBN EM constraints only Stau NLSP Ellis et. al., hep-ph/0312262 Usual WIMP allowed region superWIMP allowed region S. Su Dark Matters

Collider phenomenology - SWIMP Dark Matter no signals in direct / indirect dark matter searches SUSY NLSP: rich collider phenomenology NLSP in SWIMP: long lifetime  stable inside the detector Charged slepton highly ionizing track neutral WIMP missing energy S. Su Dark Matters

SM particle energy/angular distribution …  mG Decay life time SM particle energy/angular distribution …  mG  mpl … ~ SM NLSP Probes gravity in a particle physics experiments! BBN, CMB in the lab Precise test of supergravity: gravitino is a graviton partner ~ G SM NLSP SM NLSP ~ G ~ G SM NLSP SM NLSP ~ G ~ G How to trap slepton? Hamaguchi et. al. hep-ph/0409248 Feng and Smith, hep-ph/0409278 S. Su Dark Matters

Slepton trapping Feng and Smith, hep-ph/0409278 - Slepton could live for a year, so can be trapped then moved to a quiet environment to observe decays LHC: 106 slepton/yr possible, but most are fast. Catch 100/yr in 1 kton water LC: tune beam energy to produce slow sleptons, can catch 1000/yr in 1 kton water S. Su Dark Matters

Conclusion  precise, unambiguous evidence for new physics - We now know the composition of the Universe No known particle in the SM can be DM  precise, unambiguous evidence for new physics New physics  new stable particle as DM candidate WIMP: neutralino LSP in MSSM direct/indirect DM searches, collider studies synergy between cosmology and particle physics superWIMP slepton trapping S. Su Dark Matters