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DARK-MATTER Direct D etection

DARK-MATTER Direct D etection. Maryvonne De Jésus IPN-Lyon/CNRS France dejesus@in2p3.fr. Flat Universe. Ω = Ω Λ + Ω M = 1. 70%. 30%. Dark Energy. Matter. Visible < 1%. < 30%. <5%. DARK. ~25%. Dark Baryons. Exotic Non-Baryons. HOT. COLD. n m?. WIMPs. Axions

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DARK-MATTER Direct D etection

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  1. DARK-MATTER Direct Detection Maryvonne De Jésus IPN-Lyon/CNRS France dejesus@in2p3.fr Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  2. Flat Universe Ω = ΩΛ + ΩM = 1 70% 30% Dark Energy Matter Visible < 1% < 30% <5% DARK ~25% Dark Baryons Exotic Non-Baryons HOT COLD nm? WIMPs Axions ?????? 10-5 eV  m  10-2 eV Neutralino thanks to SUSY!! Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  3. PLAN OF THE TALK  Neutralino Direct Detection  Physics  Techniques Achievements of the most competitive currently running experiments  Prospects and outlook Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  4. c c Very low energy : ER < 100 keV Very small interaction rate : 10-5 – 10-1 c/kg/day A A Galactic neutralinos :spherical halorc ~ 0.3 GeV/c2/cm3, v ~ 10-3 c Direct Detectionon Earth: The detection reaction of neutralinos is elastic scattering off a target nucleus, the nuclear recoil energy is the measured quantity. E R How to see Neutralinos ? Accelerators : LEPlimitmc 45 GeVFermilab, LHC, … year 200X  … Indirect detection : Detection of the annihilation products  in space : GLAST, AMS, …  on Earth : Amanda, Antares, Nestor, HESS, HEAT, SuperK, … Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  5. Differential rate : dR sprc = NT F2(ER) dER2mp mc Input paramaters : Astrophysics, particle physics, nuclear physics !!!   c/kg/keV/d f(v) dv Experimentally : v = Signal + Background exp th exp dR dR dR  Exclusion limitin the plot (mc, sp) ER in keV dER dER dER Background 0 < WIMP-Nucleon Cross-Section (pb) exp dR Signal ?  dER WIMP Mass WIMP Direct Detection Physics Energy threshold :As low aspossible (in the keV range) due tothequasiexponentiallydecreasing signal shape asfunction of recoil energy. Radioactive background : As low as possible, especially neutron background which produces nuclear recoils simulating WIMP signals  Deep underground sites to minimize cosmic radiations  Specific shields : Lead, Copper, Polyethylen Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  6. Annual Modulation : The solar system moves in the galaxy with a mean velocity of ~220 km/s and Earth moves around the Sun with a velocity of ~30 km/s. In summer the two velocities add-up and in winter they subtract. This seasonnal modulation produces an annual modulation of the wimp interaction rate of the order of 5 to 7 % (the detector moves faster in June than in December) Sun 60 ° Jun ~30 km/s Diurnal modulation ,Directionnality : Asymmetry on the direction of the recoiling nucleus because the wimp velocity distribution on the Earth is peaked in the opposite direction of the Earth motion in the galactic halo. The effect is much larger than the seasonal modulation ~220 km/s Earth Dec Earth Target dependent : differential rate varies with target mass Example of spin-independent interaction A R0 c/kg/d <ER> keV H 1 5x10-5 1 2 Nv0 sprcA3 MA Mc R0 ~ Na 23 0.3 11 Mc=50 GeV v0 = 220 km/s sp= 7x10-42 cm2 <ER> ~ 2 Mc2v02 P1/2 c (MA + Mc)2 (MA + Mc)2 Si 28 0.5 12 N Ge 73 3 13 I 127 8 11 Xe 131 9 11 Pb 210 18 8 Is the signal a neutralino ? Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  7. Experiment Laboratory Technique Material Mass IGEX Canfranc, Spain Ge 2 kg 10-40 keV 0.1 - 0.04 c/kg/d /keV, ~100 kg.d HDMS Gran Sasso, Italy Ge 200 g 11-100 keV 0.2 – 0.07 c/kg/d/keV, ~27 kg.d ROSEBUD Canfranc, Spain Ge 67 g Background problems LIGHT Al2O3 50 g Background problems CHARGE CaWO4 54 g Proof of principle CRESST Gran-Sasso, Italy 262 g 15-25 keV ~0.5 c/kg/d/keV, 1.5 kg . d Al2O3 HEAT Sound 6 g Proof of the principle CaWO4 PICASSO Montreal, Canada C4F10+ C3F8 ~2g Proof of the principle ELEGANTS V Oto-Cosmo, Japan NaI 620 kg Large background210Pbcontamination UKDMC Boulby, UK NaI ~10 kg Anomalous events not yet understood PSD PSD PSD DAMA Gran Sasso, Italy NaI ~ 90 kg Annual Modulation signal Mc~52 GeV,sp ~7x10-6 pb, ~58000kg . d Exclusion limit < DAMA (~15 kg . d) ( ~ 20 events compatible with n background) 4x165g CDMS-I SUF, US Ge Exclusion limit < DAMA, (~15 kg . d) ( 20-200 keV, 1 evt ~8 kg.d) EDELWEISS-I Modane, France Ge 320 g ~4 kg Exclusion limit < DAMA, 230 kg.d ZEPLIN-I Boulby, UK Liq. Xe Some Running Experiments in sept 2002 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  8. CHARGE Superheat HEAT Semiconductors : Ge,Si LIGHT Freon TPC Cryogenic detectors : Al2O3, LiF NaI, CsI, CaF2, Liq.Xe Cryogenic detectors LIGHT + PSD NaI, Liq.Xe : UK/NAIAD, DAMA, ZEPLIN-I LIGHT HEAT CHARGE HEAT CaWO4, BGO : CRESST, Rosebud Ge , Si : CDMS, EDELWEISS LIGHT CHARGE + PSD +TPC CHARGE Superheat Liq.-GasXe : ZEPLIN-II Xe : DRIFT Freon : PICASSO,SIMPLE WIMP Direct DetectionTechniques ER Active Background Rejection Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  9. Examples of Active Background Rejection UK/NAIAD(Spooner ) recoil discrimination gammas C recoils S recoils LIGHT NaI + PSD alpha discrimination gammas alphas +TPC CHARGE Xe : UK/DRIFT S recoil region (>90%) DAMA/NaI,Liq.Xe … (Cerulli //session talk) ZEPLIN-I/Lliq.Xe (Wang //session talk) (Snowden-Ifft //session talk) Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  10. (Perera //session talk) Ge ZIP CDMS LIGHT HEAT CHARGE HEAT ROSEBUD (astro-ph/0112272) EDELWEISS (Benoit et al. astro-ph/0206271) Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  11. Experiment Laboratory Technique Material Mass IGEX Canfranc, Spain Ge 2 kg 10-40 keV 0.1 - 0.04 c/kg/d /keV, ~100 kg.d HDMS Gran Sasso, Italy Ge 200 g 11-100 keV 0.2 – 0.07 c/kg/d/keV, ~27 kg.d ROSEBUD Canfranc, Spain Ge 67 g Background problems LIGHT Al2O3 50 g Background problems CHARGE CaWO4 54 g Proof of principle CRESST Gran-Sasso, Italy 262 g 15-25 keV ~0.5 c/kg/d/keV, 1.5 kg . d Al2O3 HEAT 6 g Proof of the principle CaWO4 PICASSO Montreal, Canada C4F10+ C3F8 ~2g Proof of the principle ELEGANTS V Oto-Cosmo, Japan NaI 620 kg Large background210Pbcontamination UKDMC Boulby, UK NaI ~10 kg Anomalous events not yet understood PSD PSD PSD DAMA Gran Sasso, Italy NaI ~ 90 kg Annual Modulation signal Mc~52 GeV,sp ~7x10-6 pb, ~58000kg . d Exclusion limit < DAMA (~15 kg . d) ( ~ 20 events compatible with n background) 4x165g CDMS-I SUF, US Ge Exclusion limit < DAMA, (~15 kg . d) ( 20-200 keV, 1 evt ~8 kg.d) EDELWEISS-I Modane, France Ge 320 g ~4 kg Some Running Experiments in sept 2002 Sound Exclusion limit < DAMA, 230 kg.d ZEPLIN-I Boulby, UK Liq. Xe Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  12. Spin Independent Interaction ZEPLIN-I Preliminary Current Exclusion Limits Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  13. PSD PSD PSD PSD PSD TPC The goals for the next years : • Reach interaction rates ~ 10-3 c/kg/d • Reach interaction cross sections of the order of ~10-8 pb • Reach reasonable Susy models zone The efforts in the next years will be focused on : • Improve active background rejection • Active shielding : muon veto  Control the stability over long periods to accumulate statistics Near Future (2003-2006) projects for WIMP direct detection Experiment Lab Technique Material Mass NAIAD Boulby, UK NaI 5 0 kg ELEGANT-VI Otho-Cosmo, Japon CaF2 730 kg DAMA/LXe Gran Sasso, Italy Liq. Xe ~7 kg LIGHT Gran Sasso, Italy Ge 40 100 kg GENIUS TF- 100 CHARGE CRESST-II Gran Sasso, Italy CaWO4 33 x 300 g CUORE Gran Sasso, Italy TeO2 760 kg HEAT EDELWEISS-II Modane France Ge 21  120 x320 g Sound CDMS-II Soudan, US Ge , Si 7 x (4x250+3x100) g DAMA-LIBRA NaI 250 kg PSD ZEPLIN-II Boulby, UK Liq. Xe 40 kg Liq. Xe 1 kg KAMIOKA-Xe DRIFT-I Boulby, UK TPC Xe 1 m3 Sudbury, Canada Freon 1-10 kg PICASSO Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  14. Projected limit Spin independent Interaction 10-5 CDMS 2002 ZEPLIN 2002 DAMA 2002 10-6 EDELWEISS 2002 10-7 WIMP-Nucleon Cross-Section (pb) 10-8 10-9 102 103 WIMP Mass (GeV/c2) Kim et al.,hep-ph/0208069 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  15. EDELWEISS-II Modane/France 5 m Ge , Si CDMS-II Soudan/US CHARGE HEAT Some Setups Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  16. Dilution refrigerator LIGHT HEAT CaWO4 CRESST-II/ Gran Sasso/Italy Light- Detector 300g CaWO4 crystal Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  17. + PSD LIGHT DAMA/Lxe Gran Sasso/Italy Liquid Xe ~2.5 m CHARGE + PSD LIGHT ZEPLIN-II Boulby/UK Liq-Gas Xe ~2.5m Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  18. CHARGE + TPC : Xe DRIFT-I Boulby/UK Scattered WIMP Recoil Atom Sound PICASSO Sudbury/Canada Ionisation drift Readout Plane Electric Field Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  19. World Wide Wimp Questdirect detection experiments ELEGANTS KAMIOKA Kamioka Oto-Cosmo PICASSO CDMS-II ZEPLIN , DRIFT NAIAD EDELWEISS-II Soudan Sudbury Boulby Modane IGEX , ANAIS GEDEON Canfranc Gran Sasso DAMA , GENIUS TF CRESST , CUORE Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

  20. What is Dark Matter? « In the Oct. 26, 2001 Science, Ruvkun speculates that the number of genes in the tiny RNA world may turn out to be very large, numbering in the hundreds or even thousandsin each genome. Tiny RNA genes may be the biological equivalent of dark matter—all around us but almost escaping detection. » John Travis, Science News, Jan.12, 2002, vol . 161, no. 2 J. Gorman, Science News, Aug 12, 2000, vol. 158, no. 7 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus

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