Latest Results on Direct Detection of Dark Matter WIMPs - CDMS & SuperCDMS
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1 Latest Results on Direct Detection of Dark Matter WIMPs - CDMS & SuperCDMS TeV 2006, Madison - August 30, 2006 Blas Cabrera Co-Spokesperson CDMS & Spokesperson SuperCDMS Summary of current status of Direct Detection CDMS-II, EDELWEISS, ZEPLIN-I, CRESST, WArP DAMA, LIBRA(?), NAIAD Short term perspectives (< 5 years) SuperCDMS, EDELWEISS-II, CRESST-II ZEPLIN-II/III, XENON, WArP, ArDM, CLEAN PICASSO, SIMPLE, COUPP, SIGN, Xe gas Long term perspectives (> 5 years) Page 1
2 Composition of the Cosmos WMAP best fit Dark matter forms structure of universe WIMPs warm Page 2
3 Bullet Cluster demonstrates reality of DM Stars 4% of cluster mass - optical image from Hubble and Magellan telescopes Gas 16% of cluster mass - x-ray image in red from Chandra satellite Dark matter 80% of cluster mass - weak lensing of background galaxies Page 3
4 Numerical simulations for DM Halos The phase-space structure of a dark-matter halo: Implications for dark-matter direct detection experiments, e.g., A. Helmi, S. White, and V. Springel PRD 66, (2002) Solar system moves with respect to zero mean velocity halo at 220 km/s Page 4
5 What is the dark matter? L. Roszkowski Page 5
6 The Signal and Backgrounds Signal (WIMPs) Background (gammas) Nucleus Recoils E r Electron Recoils E r v/c E r 10 s KeV phonons v/c 0.3 ionization Neutrons also interact with nuclei, but mean free path a few cms Surface electrons from beta decay can mimic nuclear recoils χ 0 γ Page 6
7 Cross-section [cm 2 ] (normalised to nucleon) Complementarity between LHC and Direct Detection LCC1 Excluded by Accelerators Excluded by Direct Detection DAMA LHC only WIMP Mass [GeV] CDMS II 2005 EDELWEISS ZEPLIN I ILC only CDMS II 2007 SuperCDMS 25kg CDMS is cross section-limited TeV WIMPs detectable, direct connection to cosmology Page 7 Accelerators are mass-limited spectral info, but often can t see LSP or deduce its relic density
8 Combine Direct Detection and Collider data E.A. Baltz, M. Battaglia, M.E. Peskin, and T. Wizansky, hep-ph/ (120 pages) no direct detection information including SuperCDMS 25 kg experiment Page 8
9 Supersymmetry at Tevatron vs CDMS M. Carena, D. Hooper, P. Skands, hep-ph/ Tevatron 2005 CDMS current results rule out most Tevatron parameter space CDMS 2007 reach can rule out Tevatron reach or find SUSY CDMS 2005 channel would be obtained as long as the Higgsino fraction of the lightest neutralino is greater than about 0.5% and m A is heavier than about 140 GeV (as inferred from Fig. 1 and Eq. 4). On the other hand, evidence for the production of heavy neutral Higgs bosons at the Tevatron, without the observation of 2007 neutralino dark matter at CDMS by 2007, could give very valuable information about the MSSM particle spectrum. In particular, it would suggest that µ is large, e.g. greater than about 800 GeV (see Fig. 2). CDMS 3Tevatron 2007 CAVEATS TeV FIG. Conference 2: The regions 2006 in the M 2 -µ plane in which the possibility of Page discovering heavy, neutral MSSM Higgs boson at the Tevatron (4 fb 1 per experiment) through p p A/H X τ + τ X is excluded due to current CDMS limits (light shaded/green) and the projected 2007 CDMS limits (black). The (blue) shaded region along the bottom of the figure and extending upward for small µ is excluded by LEP The conclusions presented in this letter are subject to a number of assumptions. Most obviously, if the dominant component of our universe s dark matter is not made up of neutralinos, then the constraints 9 Blas Cabrera placed by - Stanford CDMS do not University affect collider searches for supersymmetry. The results from CDMS involve substantial astrophysical uncertainties. Primary among these is the local dark matter density, which we have taken to be 0.3 GeV/cm 3, as im-
10 Present sensitivity 1 kg experiments ZBG σ nw ~ cm 2 Current Status 2T CDMS-II, EDELWEISS, CRESST, ZEPLIN-I XMASS, WArP 2.3 l Page 10
11 CDMS-II SI Results & other experiments DAMA WIMP-nucleon cross-section [cm 2 ] DAMA 99% c.l. CDMS (Soudan) WARP (42 kev) CRESST EDELWEISS WIMP mass [GeV] For further details see PRL 96, (2006) New result from WArP 2.3 liter prototype 96.5 kg-d exposure BUT QF~80% UNCERTAIN OTHERS GET 25% IN AGREEMENT WITH LINDHART Page 11
12 Spin Dependent WIMP limits Spin-sensitivity from 73 Ge (J=9/2, 7.7%) and 29 Si (J=1/2, 4.7%) n scattering p scattering CRESST I CDMS Si CDMS II Si DAMA/NaI PICASSO CRESST I CDMS II Ge PICASSO CDMS II Si ZEPLIN I CDMS II Ge DAMA/NaI NAIAD Majorana ν Super-K Majorana ν For further details see PRD D73, (2006) Page 12
13 Reach of Underground Laboratories Reduce n from μ 2000 mwe 1,000 kg-d ~10-45 cm mwe 10,000 kg-d ~10-46 cm mwe 100,000 kg-d ~10-47 cm 2 Log 10 (Muon Flux) (m -2 s -1 ) Depth (meters water equivalent) Page 13
14 ST1&2 Soudan -> SNOLab like Tower 1 SUF -> Soudan Tower 1 (4 Ge & 2 Si) at SUF then at Soudan 19 neutron events at SUF 0 events at Soudan Page 14
15 Run 118 (1T) & Run 119 (2T) in Soudan Page 15
16 CDMS Active Background Rejection Detectors with excellent event-by-event background rejection Measured background rejection: % for EM backgrounds using charge/heat 99.4% for β s using pulse risetime as well Much better than expected in CDMS II proposal! Tower of 6 ZIPs Tower 1 4 Ge neutrons betas gammas gammas 2 Si betas Tower 2 2 Ge 4 Si neutrons Page 16
17 Energy calibration of Ge ZIP with 133 Ba source Ionization energy in kev Phonon energy (prg) in kev Excellent agreement between data and Monte Carlo Page 17
18 Nuclear recoil calibration: Ge&Si ZIPs w/ 252 Cf QF for Si and Ge ZIPs >90% Nuclear recoils in Ge ZIP Nuclear recoils in Si ZIP Excellent agreement between data and Monte Carlo Page 18
19 How we wet blind cuts from calibration data Show technique with simulated Gaussian distribution Technique works for any distribution Calibration and background distributions must be the same Check with events between gamma and neutron bands Calibration - Gaussian distribution 1000 evts Cut at last event Data - same distribution 100 evts Probability 0.1 of event past cut Cal x10 Data x10 On average area beyond last event = 1 On average area beyond cut = 0.1 Page 19
20 Measurement of beta backgrounds From coincident events between detectors we identify gaps Z1-2, Z2-3, Z3-4, Z4-5, and Z5-6. Correlation of alpha decays (5.3 MeV 210 Po) with beta decays (46 kev sum both sides from 210 Pb). So 210 Pb on surfaces of detectors >75% of our singles beta background. Small contributions from ϒs & radioisotopes, e.g. 14 C, 40 K Page 20 1 evt <=> 0.5x10-3 / cm 2 -d We have reduced Rn exposure for detectors in Towers 3-5 and expect >x2 reduction. We will soon measure alphas & betas.
21 Identification of alphas and betas Page 21
22 1.5 WIMP search data (5 Ge ZIPs ~53 kg-d) Prior to phonon pulse shape timing cuts 10.4 kev Gallium line 1.5 After timing cuts, which reject most electron recoils Z2/Z3/Z5/Z9/Z11 Ionization Yield Z2/Z3/Z5/Z9/Z Recoil Energy (kev) CDMS has demonstrated < 4 evt / kg of Ge / yr Ionization Yield candidate (barely) 1 near-miss Recoil Energy (kev) Background ESTIMATE: 0.37 ± 0.20 (sys.) ± 0.15 (stat.) electron recoils, 0.05 recoils from neutrons expected Page 22
23 Improvements in Surface Event Rejection Significant improvements in our analysis of phonon timing information Surface event rejection improved by x3; kept pace with exposure increase! Cuts are set from calibration data (blind analysis) We still have more discrimination power available as needed Can continue to keep backgrounds < 1 event as more data accumulates This is the real strength of CDMS detectors! Surface Events Optimize background rejection versus nuclear recoil efficiency Neutron Efficiency Neutrons Chi-square (background pulse shape) - Chi-squared (neutron pulse shape) Page 23
24 Strategy for Search Protocols Maximum exposure - Cross-section for direct detection now below cm 2 which corresponds to one event per 30 kg-d with 100% efficiency and 10 kevr threshold. Zero background best for discovery. Insitu calibrations - demonstrating insitu positions and stability of electron recoils versus nuclear recoil events and blinding. Blind analysis - Hide the WIMP search region during the determination of analysis strategy including cuts and software thresholds. Full detector modeling for MCs. Bar is set high as it should be! Page 24
25 Comparisons for SI Sensitivity comparison for all target materials have chosen typical thresholds for a cross section of 1e-8 pb how many kg-d per count on average dr/dq [cts/kev!kg!d] 3 2 1! "n = 1e!44 cm 2 ; m " = 60 GeV 4 x 10!4 Na/Ne(7 kev) 2824 kg!d/ct Si(10 kev) 2031 kg!d/ct Ar(20 kev) 1284 kg!d/ct Ge(10 kev) 313 kg!d/ct I/Xe(16 kev) 309 kg!d/ct W(16 kev) 385 kg!d/ct Recoil Energy [kev] Page 25
26 Technology Complementarity NaI - annual modulation with no discrimination (<6 pe/kev) DAMA signal is suspect because near threshold (systematics) LIBRA kg new installation (still no discrimination) Cryogenic technologies - lowest intrinsic threshold (10 6 phon/kev) (Super)CDMS Ge & Si ionization + phonon + timing (now best) EDELWEISS Ge thermal + ionization (no timing) CRESST CaWO 3 thermal + scintillation (no light for W) Liquid/gas Xe Ar Ne - high threshold (~1 pe/kev) vs large mass ZEPLIN I & XMASS scintillation (uncalibrated result) XENON scintillation + ionization (need demo of threshold & stability) WArP impressive first result but QF?, ArDM, CLEAN Superheated liquids - no energy resolution (counting) PICASSO, SIMPLE, COUPP CF 3 Br & CF 3 I (need demo of stability) TPC DRIFT - good for directionality (near term not enough mass) Page 26
27 Discrimination strategies Most particle physics experience in MeV range Direct detection requires kev scale Scintillation high threshold CRESST Scintillation ~ 1 kev/γ Phonons 10 mev/ph ZEPLIN XENON WArP, ArDM CLEAN Ionization ~ 10 ev/e Sub-K low threshold large mass >$$ CDMS EDELWEISS Initially need both Lq Nobels high threshold but large mass <$$ Page 27
28 Threshold comparison and importance Best resolution from sub-k experiments allows better discovery potential In the end, the tails of the background distributions determine the sensitivity CDMS Ge ZIP gammas XENON Prototype 99% discrimination to below ~10 kev overlap starts at ~50 kev counting statistics for more detail see n-recoils edu/hep/dm06/ talks/shutt.pdf S2 Threshold Page 28
29 EDELWEISS 1 event / 7 kg-d 1.5 EDELWEISS Experiment Phonon runs - Physics EDELWEISS-I GSA1+GSA3+GGA3 (22.7 kg.d) Ionization/Recoil Ratio 1 0.5! bands "=90% "=99.9% Recoil Energy (kev) nuclear recoil bands "=90% Edelweiss-II 320 g Ge Page 29
30 CRESST No light from W CRESST Experiment Page 30
31 Next two years 10 kg experiments ZBG σ nw ~ cm 2 5T CDMS-II, EDELWEISS, CRESST, ZEPLIN-II, XENON-10, WArP-140, ArDM Page 31
32 Five Towers now running in Soudan Tower 1: 4 Ge & 2 Si Tower 2: 2 Ge & 4 Si Tower 3: 4 Ge & 2 Si Tower 4: 4 Ge & 2 Si Tower 5: 5 Ge & 1 Si Page 32
33 Run 123 operating with five Towers All 30 detectors operational with 28 for WIMP search data More than 4 kg of Ge WIMP mass More than 1 kg of Si mass Plan to operate through 2007 Page 33
34 Cross-section [cm 2 ] (normalised to nucleon) Scientific reach of CDMS- II five towers Explore very interesting region which is complementary to LHC SuperCDMS 25 kg Experiment Project DAMA 1 Introduction WIMP Mass [GeV] CDMS II 2005 EDELWEISS ZEPLIN I CDMS II 2007 This proposal requests funding for the Super- CDMS 25 kg Experiment that will improve sensitivity for directlcc1 detection of weakly-interacting massive particles (WIMPs) by 120 beyond the existing sensitivity. The proposed five-year program would (1) continue operation of the five CDMS II towers, (2) fabricate and operate at our existing Soudan facility two SuperTowers, and (3) 10 fabricate -48 and operate at a new SNOLAB facility seven SuperTowers. to nucleon) DAMA EDELWEISS ZEPLIN I SuperCDMS 25kg CDMS II 2005 I 2007 Experiment Cross-section sensitivity CDMS II 2-T (2005) cm 2 CDMS II 5-T (2007) cm 2 SuperCDMS Detectors 2-ST at Soudan (2009) cm 2 SuperCDMS 25 kg 7-ST at SNOLAB (2012) cm 2 Table 1: WIMP-nucleon scattering cross-section goals for CDMS-II and for the proposed SuperCDMS 25 kg Experiment program (see Fig. 1). A WIMP mass of 60 GeV/c 2 is assumed with no background subtraction, where backgrounds are listed in Table 3. The ending dates are shown for completed and expected runs. in Table 1, the SuperCDMS 25 kg Experiment Page 34 program is complementary to explorations of supersymmetry and other physics beyond the Standard Model at the Large Hadron Collider (LHC),
35 In five years 100 kg experiments ZBG σ nw ~ 10 Current Status -45 cm 2 SuperCDMS 25, EDELWEISS-II, CRESST-II, WArP 140, XENON 100,... Page 35
36 SuperCDMS is approved to be sited at SNOLab SuperCDMS at SNOLab We have received strong interest from Canadian collaborators - Queens... New lab space (under construction - ready in 2007) Sudbury, Ont. CA Sudbury Neutron Obs. Page 36
37 Cryogenic System is Cryogen Free 30.00" 16.50" Cryogen-free! dilution fridge Pulse tube! cryocooler OVC-Pb-lid! o" as unit Lid! splits Pb! Shield Inner Poly! Shield 48.00" 64.00" " OVC Inner Pb! Shield IVC 44.00" 60.00" " Page 37
38 SuperCDMS 25 kg detectors Mass from 0.25 kg to 0.64 kg Improve by x100 x2.5 V/S, x2 lower betas x5 improved analysis x2 H passivate, x2 risetime Page 38
39 Data from UCB/Case TFs for Si 1 ZIP First data from 1 Si ZIP showing reconstructed location of 109 Cd events and spectrum Y Delay [μs] X Delay [μs] Number Q in [kevee] Yield Risetime [μs] neutrons Recoil [kev] Yield Page 39
40 Data from UCB/Case TFs for Ge 1 ZIP First data from 1 Ge ZIP showing 241 Am 60 kev gamma events in phonon vs charge Charge Number all events Np x-rays Phonon Q in [kevee] delay cut around source Charge Number Phonon Q in [kevee] Page 40
41 DM Direct Search Advances (2006) 58,000 kg-d ~1 event kg -1 day -1 LAr ~1 event 100 kg -1 yr -1 CRESST 04 CRESST II 230 kg-d WArP 90 kg-d 70 kg-d Need zero bkgd experiments to make progress. SuperCDMS 25 kg WArP 140 SuperCDMS 150 kg / EUREKA Plot updated from that in DM Review Article: Gaitskell, Ann. Rev. Nucl. and Part. Sci. 54 (2004) Page 41 SuperCDMS 25 kg
42 Conclusions Best sensitivity now cm 2 (10-7 pb) sensitivity for spin independent (1 kg detector mass scale); now CDMS-II 2T, soon EDELWEISS, CRESST, ZEPLIN II, WArP 2.3 l, XENON 10. By end of 2007 existing experiments will reach cm 2 (10-8 pb)(10 kg detector mass scale); CDMS-II 5T, EDELWEISS II, CRESST II, ZEPLIN II/III, WArP 140, XENON 10 Within five years next generation to reach cm 2 (10-9 pb) (100 kg detector mass scale); SuperCDMS 25 kg, EDELWEISS II, CRESST II, ZEPLIN IV, XENON 100, WArP, ArDM, CLEAN SuperCDMS 25 EXPERIMENT READY TO START NOW MULTIPLE TECHNOLOGIES ARE NECESSARY WE NEED STRONG ENDORSEMENTS FROM DM SAG & P5 DURING 2006 Page 42
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