1. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 1 Dark Matter Searches Summary of NSF Dark Matter Projects Direct Detection (including co-funds with DOE-HEP) Jim Whitmore Ani Aprahamian, Jon Kotcher at P5 Meeting at Fermilab September 24-25, 2007

2. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 2 Note: in $k Note: all of these values include base group funding DMCRDEIceCubeNeutrinoUHE  massSolar NADBDTotal 3,0964,0151321,2263903,0641071,60377074916,080 NSF PNA Funding in FY07

3. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 3 DMSAG Report July 5, 2007

4. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 4 Recommendation 1: Program and Funding To realize this program on an optimal time scale, the committee recommends that DOE and NSF increase funding for the direct detection of dark matter from the present ~$2-3M to ~$10M annually as soon as possible. The prospect of detecting dark matter while the LHC is operating amply justifies this increase. Such a figure is also consistent with the recommendations of P5 and EPP2010. See Table of funding levels since FY2002: We anticipate that the funding level will be increased over the next few years DMSAG Report TopicFY02FY03FY04FY05FY06FY07 Dark Matter$1,338,986$1,936,914$2,314,089$2,785,851$3,595,864$3,096,327

5. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 5 WIMP-detection Experiments Worldwide SUF CDMS I LiF Elegant V&VI IGEX Gran Sasso DAMA/LIBRA CRESST I/II Genius TF CUORICINO XENON WArP CanFranc IGEX ROSEBUD ANAIS LSM EDELWEISS I/II Boulby NaIAD ZEPLIN I/II/III DRIFT 1/2 Soudan CDMS II XMASS KIMS ORPHEUS FNAL COUPP SNOLAB Picasso DEAP SuperCDMS ArDM DUSEL LUX CLEAN SIGN Funded NSF Figure from D. Bauer, TAUP

6. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 6 DMSAG Report = NSF funding Figure from S. Elliott, HEPAP, Feb 07

7. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 7 Removing Muon-induced Neutron Background Neutrons from cosmic rays are irreducible background At SUF u 17 mwe u 0.5 n/kg-d At Soudan u 2090 mwe u 0.5 n/10kg-y At SNOLab u 6060 mwe u 0.2 n/ton-y Log 10 (Muon Flux) (m -2 s -1 ) Depth (meters water equivalent) CDMS I - Stanford CDMS II - Soudan PICASSO, SuperCDMS XENON10,WArP Figure from D. Bauer, TAUP ZEPLIN, DRIFT

8. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 8 Recommendation 2: ADMX The committee recommends that the ADMX collaboration be supported to operate the existing detector and, pending success of phase I, to take the necessary steps to reach greater sensitivity through lower system temperature. NSF has no involvement with ADMX DMSAG Report

9. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 9 Recommendation 3: CDMS If funding is not sufficient for the rest of the program we have outlined, we recommend that the decision to go forward with supertowers 3-7 and installation of SuperCDMS in SNOLAB be considered in the broad context of a full evaluation of the field to be completed by mid-2009. We have agreed to fund CDMS for the completion of CDMS-II; and to fund two S-CDMS super-towers at Soudan (FY07-09), at their requested level, subject to available funding and satisfactory reviews (Review in Fall 2007 – Spring 2008) No commitment (today) for anything further DMSAG Report

10. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 10 DARK MATTER: SCDMS S-CDMS (with DOE, Fermilab) at Soudan Currently approved, subject to a review Fall 07 – Spring 08, for 2 super-towers NSF: $9.88M constr. +$3.0M in FY08-09 Ge: detect low temperature phonons Limit 1.7x10 -43 cm 2 at 60 GeV

11. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 11 Large A best since for SI s ~ A 2 for low nuclear recoil energy Xe “easy” cryogenics at ~165K DARK MATTER SEARCHES

12. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 12 Recommendation 4: Noble Liquid Detectors a) The sub-panel supports the development of one two-phase xenon- based detector at the 100 kg scale and above. b) The sub-panel supports the development of detectors using liquid argon and/or liquid neon technology. WARP and miniCLEAN/DEAP represent two quite different technologies in their application to liquid argon. Both of these techniques should be explored to discover which has greater potential. (a) Xenon “two similar projects” issue: We will fund XENON10+ (upgrade) in FY08 We will consider some funding for the LUX initiative in FY08, in coordination with DOE, following review We support Zeplin-II PIs at the $180k level in FY07 (b) We are funding WARP at the ~$600k level in FY07 and $300K for FY08-09 No current funding to DEAP/CLEAN DMSAG Report

13. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 13

14. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 14 DARK MATTER: XENON10 NSF has funded $5.59M (FY02-07) With 136 kg-day exposure: 4.5x10 -44 cm 2 at 30 GeV XENON10 (with DOE, Germany) at LNGS 2-phase Xe 5.4 kg fiducial mass 3-D position sensitive TPC

15. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 15 DARK MATTER: ZEPLIN-II ZEPLIN-II (with DOE, PPARC) at Boulby (UK) mine 32 kg 2-phase Xenon Measures both primary and secondary scintillation NSF providing $890k over 7 yrs (FY02-08) 6.6x10 -43 cm 2 at 65 GeV from 225 kg-day exposure

16. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 16 DARK MATTER: WArP WArP (with INFN, Poland) 2-phase LAr 140 kg fiducial mass (under const.) At LNGS Pulse shape/ionization/scintillation discrimination NSF is providing $1.55M (FY06-09) Current limit ~ 7x10 -43 cm 2 at 100 GeV with 3.2 Kg and 96.5 kg-day exposure 140 kg Operation in early 2008

17. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 17 Recommendation 5: Superheated Liquids and Directional Sensitivity a) The sub-panel recommends the development of superheated liquid detectors. The program proposed by COUPP appears to be well balanced and has recently been approved by the Fermilab PAC. b) On the basis of the performance and background levels presented by the DRIFT collaboration, the sub-panel recommends the development of a single prototype detector module with the principal goal of demonstrating track reconstruction and directionality determination. We have been supporting the COUPP program with a CAREER award that started in FY03 and the DRIFT program with one that started in FY06 (a) We are currently supporting COUPP at the level of $320k in FY07 (b) We are currently supporting the DRIFT project at the level of $647k in FY07 (incl. DUSEL R&D) DMSAG Report

18. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 18 DARK MATTER: COUPP COUPP (with DOE/Fermilab) Room temperature bubble chamber 1.5 kg of superheated CF 3 I (350 ft deep NUMI tunnel at Fermilab) NSF has funded $640k (FY03-07) pe rejection 10 -10 for E r ~ 10 keV 52 kg-day run SD limit 2.6x10 -37 cm 2 @ 50 GeV

19. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 19 DARK MATTER: DRIFT-II DRIFT-II (with PPARC) a low pressure gaseous TPC target carbon disulphide (CS 2 ) DRIFT is designed for scalable target mass and dE/dx background discrimination. The use of low pressure gas and position sensitive readout means DRIFT is sensitive to the direction of incident particle. at Boulby (UK) mine NSF has provided $2M in FY02-07

20. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 20 Recommendation 6: DUSEL We strongly support the construction of a U.S. Deep Underground Science and Engineering Laboratory (DUSEL), which could host ton-size or greater direct dark matter detection experiments. We agree DMSAG Report

21. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 21 Recommendation 7: Scanning Facilities We recommend additional underground scanning capability to alleviate the impending shortage, increase the sensitivity, and expedite the scanning of materials for the new generations of detectors. Ideally, a comprehensive facility, as described in the DUSEL S1 report, should be located in the DUSEL site. With DUSEL R&D funds, we have supported such activities in FY07 at the $433k level (but at various sites in the US) DMSAG Report

22. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 22 Dark Matter Double Beta Decay Solar Neutrinos Facilities SCDMSCUOREe-bubbleUndergnd Ar* COUPPEXOLENSScreening DRIFTMAJORANABeta cage SIGNn-meter LXe / LNe DUSEL R&D FY07 Total (NSF/ DOE-HEP/ DOE-NP) $3.7M *( 39 Ar/Ar)und / ( 39 Ar/Ar)atm = 0.00±0.05

23. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 23 Recommendation 8: Priorities Following on the above recommendations, if the comprehensive program we have described above is not able to be fully funded, then we recommend that the funding priorities during the next few years be allocated as follows: 1. Equal priorities between (A) and (B): A) Continuing the on-going CDMS and ADMX experiments and the initial construction of SuperCDMS in Soudan with two super-towers. We are supporting CDMS and S-CDMS at the two-supertower level B) Funding the expansion of the noble liquids with priorities i), ii) and iii): i) The expansion of the liquid Xenon experimental efforts to their next level. We are supporting XENON10+; considering other possibilities (LUX) ii) The U.S. participation in the WARP detector development. We are supporting WArP at a $600k level in FY07 iii) The next stage of the CLEAN Argon/Neon detector development. We have no involvement with DEAP/CLEAN at present DMSAG Report

24. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 24 Recommendation 8: Priorities (Cont.) Following on the above recommendations, if the comprehensive program we have described above is not able to be fully funded, then we recommend that the funding priorities during the next few years be allocated as follows 2. The development of superheated liquid detectors and detectors capable of determining WIMP direction. Although these ideas have great promise, they still have significant R&D questions remaining to be answered. We are supporting COUPP and DRIFT-II We believe that many of the questions associated with the longer-term direction of the experimental efforts will be resolved during the next few years, provided that the current support continues and our recommendations are implemented, and that a program review in or around 2009 will be necessary. We are anticipating another Dark Matter field review sometime in the next 1-2 years DMSAG Report

25. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 25 Summary of DM projects Project(FY05-07) NSF $k TechniqueLocationSensitivity to date (cm 2 ) Mass GeV XENON103,4352-phase Xenon LNGS4.5x10 -44 30 CDMS3,049Cryogenic Ge and Si Soudan1.7x10 -43 60 Zeplin-II330 2-phase Xenon Boulby6.6x10 -43 65 WARP9452-phase Argon LNGS7x10 -43 100 COUPP400Bubble Chamber Fermilab2.6x10 -37 Spin Depend. 50 DRIFT-II983TPCBoulby--- Other335---

26. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 26 NSF PNA Program TopicFY02FY03FY04FY05FY06FY07 Dark Matter$1,338,986$1,936,914$2,314,089$2,785,851$3,595,864$3,096,327 Cosmic Rays1,896,6683,372,6593,181,3613,387,1934,302,7154,014,807 UHE Gamma Rays2,475,4143,323,5424,257,0153,730,2922,886,0593,063,731 IceCube738,439592,383478,426383,618730,9591,225,906 Neutrinos, p decay234,975369,358352,708195,00597,200390,000 Solar neutrinos1,295,1891,177,688996,3361,250,0001,460,0001,603,000 Double Beta Decay137,900032,858319,990320,000749,016 Neutrino mass004,90351,28957,887107,207 Dark Energy00000132,000 DUSEL R&D000003,110,720 Nucl. Astrophysics855,644855,643825,000730,000 770,000 AST/Cosmol/Conf.832,954261,482241,8341,856,3521,672,002928,002 Totals9,806,16911,889,66912,684,53014,689,59015,852,68619,190,716 Note: all of these values include base group funding

27. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 27 NSF PNA Program BACKUP SLIDES

28. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 28 Summary of DM Projects (From P. Belli, TAUP2007)

29. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 29 XENON Program : 2007-2008  New detector to replace XENON10 in current shield at LNGS is under construction  150 kg total (70 kg in target) procured. Purification for ppt level of Kr started  Low activity PMTs and cryostat, active LXe veto, cryocooler and feed-throughs outside shield  factor ~100 reduction in total gamma background compared to XENON10  1 inch PMTs for good event XY localization and volume definition  Systematic screening of components with dedicated HPGe at LNGS  Optimized light detection for 5 keVr threshold 150 kg  New measurements of QF from 4- 40 keVr with optimized LXe detector carried out in Summer 07.  Data analysis ongoing. Results to be published shortly. New Collaboration: Columbia, Coimbra, LNGS, Rice, University of Zurich (From E.Aprile, TAUP2007)

30. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 30 Summary of DM projects (From E.Aprile, TAUP2007) Projections: CDMS Soudan 2007 S-CDMS 25 Kg (7-ST) XENON 100 (2008)

31. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 31 Summary of DM projects (From K.Abe, TAUP2007) Projections: XMASS 800 kg 1-ton LXe, DM search 10 -45 cm 2 Status: Budget funded this year 2-year construction Start measurements in 2009

32. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 32 DARK MATTER: COUPP SD limit 2.6x10 -37 cm 2 @ 50 GeV SI limit not competitive at present

33. NSF Dark Matter Program P5 Meeting, Sept 24-25, 2007 33 Depth vs Volume Underground DUSEL expectation First suite extensions From Deep Science (2006) Report DRIFT, ZEPLIN-II XENON10, WARP CDMS COUPP Fermilab PICASSO