WIMPs/Neutralinos Direct Detection Maryvonne De Jésus IPN-Lyon/CNRS France [email protected] 1 The budget content of the Universe 2 http://map.gsfc.nasa.gov/m_mm/mr_content.html Cold dark matter Two serious candidates ¾ Axions : pseudoscalar boson solve the strong CP problem 10-5 eV ≤ m ≤ 10-2 eV , few experiments ¾ WIMPs : more than 20 experiments WIMPs Id card : -27 3 -1 Relic density : Ωwimps . < σA v > ~ 10 cm s Æ ~ Weak interaction SUSY candidate : lightest neutralino, LSP in MSSM ~~ ~~ 3 0 0 χχ == aa1ΒΒ ++ aa2WW ++ aa3 HH1 ++ aa4 HH2 3 gaugino higgsino WIMPs/ Neutralinos hunting On Accelerators : LEP limit Æ mχ ≥ 45 GeV Year 200X Æ … Tevatron, LHC, … Off Accelerators WIMP halo, maxwellian velocity distribution -1 -1 -3 v0 = 230 kms ; vesc = 230 kms ; ρ0 = 0.3 GeVcm Indirect detection : Detection of the annihilation products Æ in space : GLAST, AMS, … > 2006 Direct Detection on Earth : Æ on Earth : Amanda, Antares, The detection reaction of neutralinos is elastic scattering Nestor, HESS, HEAT, SuperK, … >2004-2006 off a target nucleus, the nuclear recoil energy is the measured quantity. Very low energy : ER < 100 keV n, χ n, χ Very small interaction rate : 10-5 –10-1 c/kg/day nuclear recoil : signal WIMP Direct Detection Physics Differential rate : vmax dR σρχ = F2(|q|) ⌠ f(v) dv F2(|q|) : spin-dependant and/or spin -independant dE 2 µ2 m R χ ⌡vmin v σ spin-dependant % J(J+1) favours nuclei with spin F,Al,… 2 σ spin-independant % A favours heavy nuclei Ge, W, I, … Experimentally : dR = Signal + Background )exp excluded dER dR ⇒ Exclusion limit in the plot (m , σ ) )exp χ p dER c/kg/keV/d 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 : b E in keV p R ( As low as possible, especially neutron background n o i which produces nuclear recoils simulating t c e WIMP signals S - s s Æ Deep underground sites to minimize cosmic o Cr radiations n Æ Specific shields : Lead, Copper, Polyethylen o e l c Nu dR ⇒ - Background Æ 0 )exp Signal ? P M dE I R 5 W WIMP Mass WIMPsWIMPs OrOr NotNot WIMPsWIMPs ?? Annual Modulation : Sun The solar system moves in the galaxy with a mean velocity of 60 ° Jun ~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 ~30 km/s ~220 km/s they subtract. This seasonnal modulation produces an annual Earth modulation of the wimp interaction rate of the order of 5 to 7 % Dec (the detector moves faster in June than in December) N χ Diurnal modulation ,Directionnality : Asymmetry on the direction of the recoiling nucleus because χ the wimp velocity distribution on the Earth is peaked in the Earth opposite direction of the Earth motion in the galactic halo. The effect is much larger than the seasonal modulation Target dependent : differential rate varies with target atomic mass Example of spin-independent interaction R <E > M A 0 R <E > ~ 2 M 2 v 2 A c/kg/d keV R χ 0 2 H 1 5x10-5 1 (MA + Mχ) Na 23 0.3 11 3 Mχ Si 28 0.5 12 2 N v σp ρχ A R0 ~ 0 2 Ge 73 3 13 1/2 (M + M ) Mχ=50 GeV Π A χ I 127 8 11 v0 = 220 km/s Xe 131 9 11 σ = 7x106-42 cm2 Pb 210 18 8 p WIMP Direct Detection Tools ER CHARGE Superheat Semiconductors : Ge,Si Freon TPC LIGHT HEAT NaI, CsI, CaF2, Liq.Xe Cryogenic detectors : Al2O3, LiF Active Background Rejection Cryogenic detectors LIGHT + PSD CHARGE HEAT LIGHT HEAT NaI, Liq.Xe : UK/NAIAD, DAMA, Ge , Si : CDMS, EDELWEISS CaWO4, BGO : CRESST, Rosebud ZEPLIN-I LIGHT CHARGE + PSD Superheat CHARGE + TPC Liq.-GasXe : ZEPLIN-II Freon : PICASSO,SIMPLE Xe : DRIFT 7 ExamplesExamples ofof ActiveActive BackgroundBackground RRejectionejection LIGHT + PSD CHARGE + TPC Xe : UK/DRIFT ZEPLIN-I/Lliq.Xe(N.Smith, IAU Sydney July 2003) Gamma source 1 recoil discrimination 0.1 gammas 0.01 0.001 C recoils 0.0001 S recoils 0.00001 1 10 100 pulse time constant (ns) Neutron1 source 0.1 alpha discrimination 0.01 gammas 0.001 0.0001 alphas 0.00001 1 10 100 pulse time constant ns S recoil region (>90%) DAMA/NaI,Liq.Xe … UK/NAIAD (N.Smith, IAU Sydney July 2003) 8 CHARGE HEAT LIGHT HEAT CDMS (R.Gaitskell EPS HEP Aachen July 2003) ROSEBUD (P.de Marcillac LTD July 2003) 1334 Photons (external source) 616 Neutrons (external source) Ionization Threshold EDELWEISS (L.Chabert EPS HEP Aachen July 2003) CRESST 9 The Top Five on the highlights in 2003: ¾ DAMA ¾ NaIAD ¾ ZEPLIN ¾ CDMS ¾ EDELWEISS And others : ¾ CRESST ¾ PICASSO ¾ DRIFT ¾ … 10 DAMA NaI Experiment Gran Sasso Underground Laboratory (Italy) 100 kg NaI detector mass (scintillation) 58,000 kg-days exposure (4 years) See annual modulation signal! • Claim model independent evidence for WIMPs in the galactic halo NaI NaI NaI PMT PMT NaI Mχ~52 GeV, σp ~7x10-6 pb 11 http://www.lngs.infn.it/site/meesem/DAMA/DAMA.pdf DAMA/NaI latest results astro-ph/0307403 3more annual cycles acquired 58,000 + 49,800 = 107,800 kg-d 12 7 cycles total DAMA / LIBRA LIBRA : Large sodium Iodide Bulk for RAre processes 250 kg with improved radiopurity ~ 9 Months of Data so far – announcement by end of 2003? Further R&D toward 1-ton NaI(Tl) radiopurification started DAMA/LXe 13 UK/Boulby : NaIAD (NaI Advanced Detectors ) • 8 NaI crystals 6 unencapsulated, 2 encapsulated ~ 60 kg • Direct crosscheck of DAMA results • Data taking continue … 1997 2000/01 (10.6 kg.yrs) 2002 (new 25 kg.yrs) 14 ZEPLIN (UKDM Collaboration, Boulby mine) Xe+ Ionisation +Xe ZEPLIN - I Electron/nuclear recoil + Xe2 • Single-phase detector Excitation +e- Primary scintillation + Pulse shape discrimination (recombination) Xe* Xe** + Xe +Xe • Preliminary results : 290 kg-days in 3.1-kg fiducial Xe * 175nm 2 175nm • Purification of Xe : lower backgrounds Triplet Singlet 27ns 3ns – New data set being analysed 2Xe 2Xe – Other improvements • Trigger efficiency 5kg LXe target (3.1kg fid), 3 PMTs • Neutron calibration in underground site 0.1 data 0.01 gamma cal GD fit 0.001 0.0001 0.00001 1 10 100 fitted time constant ns 1 Ton liquid PXE scintillator Veto 15 (N.Smith, IAU Sydney July 2003) ZEPLIN-II and III under construction ~2.5 m Install mid 2004 Two phase Xenon : liquid and gas (30 kg active) ZEPLIN - II Measure both scintillation and ionisation ~2.5m applying a low E field ZEPLIN – III Active volume 6kg High-field readout 8kV/cm to reduce ionization recombination for nuclear recoils 16 CDMS (Cryogenic Dark Matter Search) •1999 – 3+1 Ge (165g) BLIP detectors at ‘shallow’ site in Stanford NTD thermistors SUF – 17 mwe depth Final results •2001-2002 – 4 Ge (250g) + 2 Si (100g) ZIP detectors at ‘shallow’ site Superconducting thin films of W, Al SUF – 17 mwe depth First results 17 CDMS exclusion results −40 10 http://dmtools.berkeley.edu/ 28.3 kg-day, 13 nuclear recoils, 2 triple scatters Gaitskell&Mandic Nuclear recoils interpreted as neutron bkg by comparison with MC ion ct 1.4 ra ubt −41 s 10 no 3 1.2 ] (normalised to nucleon) 0 3 2 20 0 S 20 S DM 1 C DM C ub /s w 0.8 0.6 Cross−section [cm −42 10 030606161701 1 2 3 10 10 10 Ionization Yield 0.4 WIMP Mass [GeV] 0.2 0 0 20 40 60 80 100 Recoil Energy (keV) 18 Phys.Rev. D66 (2002) 122003, astro-ph/0203500; hep-ex/0306001 CDMS-II in the Soudan mine 2003 and beyond 12 ZIP detectors at ‘deep’ site Soudan Mine – 2090 mwe depth Muon flux reduced by 10000 compared to Stanford shallow site Neutron flux reduced by 400 Tower 1 Tower 2 ~1/kg/day to ~1/kg/year (New dets) First operation April 2003 First ‘dark data’ : few months from now 18 more detectors in fab (4 kg Ge total) improvement : / 100 to 0.01 event/kg-days 19 EDELWEISS (Expérience pour Detecter Les Wimps en Site Souterrain) Modane Underground Laboratory (Fréjus, France) : 4800 mwe muon flux = 4/m2/d neutron flux = 1.6 10-6/s/cm2 • Low radioactivity cryostat • Shield: 30 cm paraffin, 20 cm Pb, 10 cm Cu Roman lead EDELWEISS May 2002 October 2002 3 * 320 g Ge detectors GGA1,GeAl9,GeAl10 GGA3, GSA1, GSA3 Heat and ionisation Ge detectors 3x320g Aluminium electrodes (center + guard ring) Ge or Si amorphous layer 20 NTD sensor on guard ring electrode EDELWEISS – I : “1 kg stage” Gamma and neutron calibration •2000: Exposure of 4.5 kg-d •2002: Increase to 11.7 kg-d •2003: 32 kg-d added A. Benoit, Phys. Lett. B545 (2002) 43 (L.Chabert EPS HEP Aachen July 2003) Two events compatible with neutron induced nuclear recoils. Conservatively considered as real events Incompatibility with DAMA (first 4 seasons) candidate (99.8% C.L.) confirmed with three different detectors and extended exposure August 2003: 21 End EDELWEISS-I EDELWEISS – II Karlsruhe/KARMEN group joins EDELWEISS • 20 cm Pb (~50 tons) • 50 cm polyethylene (~35 tons) • Muon veto 140 m2 plastic scintillator Install EDELWEISS-II : Sept 2003 – 2004 100 litre cryostat 21 × 320 g Ge-NTD detectors + 7 NbSi thin film 200 g Ge detectors Æ 9 kg (ready by fall 2004) capacity 120 detectors 22 Spin independant exclusion limits in august 2003 ???? NaIAD 2002 (new 25 kg.yrs) DAMA july 2003 (SI with 0 SD) 23 CRESST-II/ Gran Sasso/Italy Dilution refrigerator CRESST I : 4x4x4 cm 3 sapphire crystal 262g with a W-thermometer Operating temperature: 12 mK -> energy resolution: 133eV @ 1.5 keV CRESST II : simultaneous detection of phonons and light Absorber materials :CaWO 4 ,PbWO 4 ,BaF, BGO High rejection: - no surface effects 99.7% E > 15 keV 99.9% E > 20 keV - but less energy in light Light- Detector Will have 33x300g modules 300g300g (total mass about 10 kg) CaWOCaWO44 crystalcrystal http://avmp01.mppmu.mpg.de/cresst/Welcome.html 24 PICASSO Sudbury/Canada ¾Small freon droplets in polymerized gel at room T° droplets overheat