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

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Presentation on theme: "Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 1 DARK-MATTER Direct Detection Maryvonne De Jésus IPN-Lyon/CNRS France"— Presentation transcript:

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

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

3 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

4 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 4 How to see Neutralinos ? Accelerators Accelerators : LEP limit  m   45 GeV Fermilab, LHC, … year 200X  … Galactic neutralinos Galactic neutralinos : spherical halo   ~ 0.3 GeV/c 2 /cm 3, v ~ 10 -3 c Indirect detection : Detection of the annihilation products  in space : GLAST, AMS, …  on Earth : Amanda, Antares, Nestor, HESS, HEAT, SuperK, … Direct Detection on Earth : A   R E A The detection reaction of neutralinos is elastic scattering off a target nucleus, the nuclear recoil energy is the measured quantity. Very low energy : E R < 100 keV Very small interaction rate : 10 -5 – 10 -1 c/kg/day

5 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 5 WIMP Direct Detection Physics Experimentally : dR dE R  exp = Signal + Background E R in keV c/kg/keV/d Differential rate Differential rate : dE R 2 m p m  dR  p    F 2 (E R )   f(v) v dv = N T Input paramaters : Astrophysics, particle physics, nuclear physics !!! Energy threshold : As low as possible (in the keV range) due to the quasi exponentially decreasing signal shape as function 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 Background  0 Exclusion limit in the plot ( m ,  p )  < dR dE R  exp dR dE R  th dR Signal ?  dE R  exp WIMP Mass WIMP -Nucleon Cross-Section (pb)

6 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 6 Is the signal a neutralino ? Target dependent : differential rate varies with target mass 11 0.323Na 119131Xe 818210Pb 8127I 13373Ge 120.528Si 15x10 -5 1H keV R 0 c/kg/d A M  =50 GeV v 0 = 220 km/s  p = 7x10 -42 cm 2 ~ 2 M  2 v 0 2 (M A + M  ) 2 MAMA MM 2 N v 0  p    A 3   R 0 ~ Example of spin-independent interaction 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) ~30 km/s 60 ° ~220 km/s Jun Dec Sun Earth 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  N Earth

7 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 7 Some Running Experiments in sept 2002 Boulby, UK ZEPLIN-I CHARGE HEAT LIGHT Sound Exclusion limit < DAMA, 230 kg.d Liq. Xe Exclusion limit < DAMA (~15 kg. d) ( ~ 20 events compatible with n background) Exclusion limit < DAMA, (~15 kg. d) ( 20-200 keV, 1 evt ~8 kg.d) Proof of the principle ~2g C 4 F 10 + C 3 F 8 Montreal, Canada PICASSO Proof of the principle 6 g M  ~52 GeV,  p ~7x10-6 pb, ~58000kg. d 320 gGe Modane, France EDELWEISS-I ~4 kg Ge SUF, US CDMS-I Annual Modulation signal ~ 90 kgNaI Gran Sasso, Italy DAMA Anomalous events not yet understood ~10 kgNaI Boulby, UK UKDMC Large background 210 Pb contamination 620 kgNaI Oto-Cosmo, Japan ELEGANTS V 15-25 keV ~0.5 c/kg/d/keV, 1.5 kg. d 262 g Gran-Sasso, Italy CRESST Proof of principle 54 gCaWO 4 50 gAl 2 O 3 Background problems 67 gGe Canfranc, Spain ROSEBUD 11-100 keV 0.2 – 0.07 c/kg/d/keV, ~27 kg.d 200 gGe Gran Sasso, Italy HDMS 10-40 keV 0.1 - 0.04 c/kg/d /keV, ~100 kg.d 2 kgGe Canfranc, Spain IGEX MassMaterialTechnique Laboratory Experiment PSD 4x165g Background problems Al 2 O 3 CaWO 4

8 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 8 WIMP Direct DetectionTechniques ERER Active Background Rejection NaI, CsI, CaF 2, Liq.Xe LIGHT Semiconductors : Ge,Si CHARGE TPC HEAT Cryogenic detectors : Al 2 O 3, LiF Superheat Freon Superheat Freon : PICASSO,SIMPLE HEAT Ge, Si : CDMS, EDELWEISS CHARGE CaWO 4, BGO : CRESST, Rosebud LIGHT HEAT Cryogenic detectors + PSD LIGHT NaI, Liq.Xe : UK/NAIAD, DAMA, ZEPLIN-I CHARGE + TPC Xe : DRIFT Liq.-GasXe : ZEPLIN-II LIGHT CHARGE + PSD

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

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

11 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 11 Liq. Xe Boulby, UK ZEPLIN-I CHARGE HEAT LIGHT Some Running Experiments in sept 2002 Sound Exclusion limit < DAMA, 230 kg.d

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

13 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 13 Near Future (2003-2006) projects for WIMP direct detection CHARGE HEAT LIGHT  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 goals for the next years : 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 TechniqueMassMaterialLab 1 kgLiq. Xe KAMIOKA-Xe 40 kgLiq. Xe PSD Boulby, UKZEPLIN-II 730 kgCaF2Otho-Cosmo, JaponELEGANT-VI 7 x (4x250+3x100) g Ge, SiSoudan, USCDMS-II 250 kgNaIDAMA-LIBRA 760 kgTeO2Gran Sasso, ItalyCUORE 21  120 x 320 g GeModane FranceEDELWEISS-II 5 0 kgNaIBoulby, UK NAIAD Experiment ~7 kgLiq. XeGran Sasso, ItalyDAMA/LXe 33 x 300 g 40  100 kg CaWO4Gran Sasso, ItalyCRESST-II GeGran Sasso, Italy PSD DRIFT-I GENIUS TF- 100 TPC Xe1 m 3 PSD Boulby, UK TPC Sound PICASSO Sudbury, Canada Freon 1-10 kg

14 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 14 WIMP Mass (GeV/c 2 ) Spin independent Interaction 10 -5 10 -6 10 -7 10 -8 10 -9 WIMP-Nucleon Cross-Section (pb) 10 2 10 3 Projected limit CDMS 2002 ZEPLIN 2002 EDELWEISS 2002 DAMA 2002 Kim et al.,hep-ph/0208069

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

16 Cosmo02, Chicago 18-21 september 2002 Maryvonne De Jésus 16 LIGHTHEAT CaWO 4 Dilution refrigerator 300g CaWO 4 crystal 300g CaWO 4 crystal Light- Detector CRESST-II/ Gran Sasso/Italy

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

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

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

20 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 thousands in 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

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