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

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 WhitmoreAni Aprahamian, Jon

Kotcherat P5 Meeting at Fermilab

September 24-25, 2007


PNA funding by topic

Neutrinos3%

UHE Gamma Rays20%

Solar neutrinos11%

Nucl Astro5%

Neutrino mass1%

Double beta decay5%

Cosmic Rays26%

Dark Energy1%

IceCube8%

Dark Matter20%

Note: in $kNote: all of these values include base group funding

DM CR DE IceCube

Neutrino

UHE mass

Solar

NA DBD Total

3,096

4,015

132

1,226 390 3,064 107 1,603 770

749 16,080

NSF PNA Funding in FY07


DMSAG ReportJuly 5, 2007


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

Topic FY02 FY03 FY04 FY05 FY06 FY07

Dark Matter $1,338,986 $1,936,914 $2,314,089 $2,785,851 $3,595,864 $3,096,327


WIMP-detection Experiments Worldwide

SUF CDMS I

LiFElegant V&VI

IGEX

Gran SassoDAMA/LIBRACRESST I/IIGenius TFCUORICINOXENONWArP

CanFrancIGEXROSEBUDANAIS

LSMEDELWEISS I/II

BoulbyNaIADZEPLIN I/II/IIIDRIFT 1/2

Soudan CDMS II

XMASSKIMS

ORPHEUS

FNAL COUPP

SNOLABPicassoDEAPSuperCDMS

ArDM

DUSELLUXCLEANSIGN

Funded NSF

Figure from D. Bauer, TAUP


DMSAG Report

= NSF funding

Figure from S. Elliott, HEPAP, Feb 07


Removing Muon-induced Neutron Background

• Neutrons from cosmic rays are irreducible background

• At SUF 17 mwe 0.5 n/kg-d

• At Soudan 2090 mwe 0.5 n/10kg-y

• At SNOLab 6060 mwe 0.2 n/ton-y

Log 10

(Muo

n Fl

ux) (

m-2s-1

)

Depth (meters water equivalent)

CDMS I - Stanford

CDMS II - Soudan

PICASSO, SuperCDMS

XENON10,WArP

Figure from D. Bauer, TAUP

ZEPLIN, DRIFT


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


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


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 cm2 at 60 GeV


Large A best since for SI s ~ A2 for low nuclear recoil energy

Xe “easy” cryogenics at ~165K

DARK MATTER SEARCHES


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



DARK MATTER: XENON10

• NSF has funded $5.59M (FY02-07)

• With 136 kg-day exposure:

• 4.5x10-44 cm2 at 30 GeV

• XENON10 (with DOE, Germany) at LNGS• 2-phase Xe 5.4 kg fiducial mass• 3-D position sensitive TPC


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 cm2 at 65 GeV

from 225 kg-day exposure


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 cm2 at 100 GeV with 3.2

Kg and 96.5 kg-day exposure

140 kgOperati

onin early

2008


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


DARK MATTER: COUPP• COUPP (with DOE/Fermilab)• Room temperature bubble chamber• 1.5 kg of superheated CF3I (350 ft

deep NUMI tunnel at Fermilab)

• NSF has funded $640k (FY03-07)

• pe rejection 10-10 for Er ~ 10 keV

• 52 kg-day run• SD limit 2.6x10-37 cm2

@ 50 GeV

http://collargroup.uchicago.edu/news/images/coupp-3_large.jpg


DARK MATTER: DRIFT-II• DRIFT-II (with PPARC)• a low pressure gaseous TPC• target carbon disulphide (CS2) • 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


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


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


DUSEL R&D for FY07

Double beta decay19%

Solar neutrinos11%

R&D Facilities14%

Dark Matter56%

Dark Matter

Double Beta Decay

Solar Neutrinos

Facilities

SCDMS CUORE e-bubble Undergnd Ar*

COUPP EXO LENS Screening

DRIFT MAJORANA Beta cage

SIGN n-meter

LXe / LNe

DUSEL R&D FY07

Total (NSF/

DOE-HEP/DOE-NP)$3.7M

*(39Ar/Ar)und / (39Ar/Ar)atm = 0.00±0.05


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

levelB) 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 FY07iii) The next stage of the CLEAN Argon/Neon detector

development. We have no involvement with DEAP/CLEAN at present

DMSAG Report


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


Summary of DM projectsProject (FY05-

07)NSF $k

Technique

Location

Sensitivity

to date (cm2)

MassGeV

XENON10

3,435 2-phaseXenon

LNGS 4.5x10-44 30

CDMS 3,049 CryogenicGe and Si

Soudan

1.7x10-43 60

Zeplin-II 330 2-phase Xenon

Boulby 6.6x10-43 65

WARP 945 2-phase Argon

LNGS 7x10-43 100

COUPP 400 BubbleChamber

Fermilab

2.6x10-37

Spin Depend.

50

DRIFT-II 983 TPC Boulby --- ---

Other 335 --- --- --- ---


NSF PNA Program

Topic FY02 FY03 FY04 FY05 FY06 FY07

Dark Matter $1,338,986 $1,936,914

$2,314,089 $2,785,851

$3,595,864

$3,096,327

Cosmic Rays 1,896,668 3,372,659 3,181,361 3,387,193 4,302,715 4,014,807

UHE Gamma Rays

2,475,414 3,323,542 4,257,015 3,730,292 2,886,059 3,063,731

IceCube 738,439 592,383 478,426 383,618 730,959 1,225,906

Neutrinos, p decay

234,975 369,358 352,708 195,005 97,200 390,000

Solar neutrinos 1,295,189 1,177,688 996,336 1,250,000 1,460,000 1,603,000

Double Beta Decay

137,900 0 32,858 319,990 320,000 749,016

Neutrino mass 0 0 4,903 51,289 57,887 107,207

Dark Energy 0 0 0 0 0 132,000

DUSEL R&D 0 0 0 0 0 3,110,720

Nucl. Astrophysics

855,644 855,643 825,000 730,000 730,000 770,000

AST/Cosmol/Conf.

832,954 261,482 241,834 1,856,352 1,672,002 928,002

Totals 9,806,169 11,889,669

12,684,530 14,689,590

15,852,686

19,190,716Note: all of these values include base group funding


NSF PNA Program

BACKUP SLIDES


Summary of DM Projects

(From P. Belli, TAUP2007)


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)


Summary of DM projects

(From E.Aprile, TAUP2007)

Projections:

CDMS Soudan 2007

S-CDMS 25 Kg (7-ST)XENON 100 (2008)


Summary of DM projects

(From K.Abe, TAUP2007)

Projections:

XMASS 800 kg1-ton LXe,DM search 10-45 cm2

Status:•Budget funded this year•2-year construction•Start measurements in 2009


DARK MATTER: COUPP

• SD limit 2.6x10-37 cm2 @ 50 GeV• SI limit not competitive at present

http://collargroup.uchicago.edu/news/images/coupp-3_large.jpg


Depth vs Volume Underground

DUSEL expectationFirst suiteextensions

From Deep Science (2006) Report

DR

IFT,

ZEP

LIN

-II

XEN

ON

10

, W

AR

P

CD

MS CO

UP

PFerm

ilab

PIC

AS

SO

Documents

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