Dark Matter Direct Detection roadmap strategy

Slides:



Advertisements
Similar presentations
MACHe3: Prototype of a bolometric detector based on superfluid 3 He for the search of non-baryonic Dark Matter C. Winkelmann J. Elbs E. Collin Yu. Bunkov.
Advertisements

Status of XMASS experiment Shigetaka Moriyama Institute for Cosmic Ray Research, University of Tokyo For the XMASS collaboration September 10 th, 2013.
EDELWEISS-I last results EDELWEISS-II prospects for dark matter direct detection CEA-Saclay DAPNIA and DRECAM CRTBT Grenoble CSNSM Orsay IAP Paris IPN.
DMSAG 14/8/06 Mark Boulay Towards Dark Matter with DEAP at SNOLAB Mark Boulay Canada Research Chair in Particle Astrophysics Queen’s University DEAP-1:
The PICASSO experiment - searching for cold dark matter
Report from Low Background Experiments Geant4 Collaboration Workshop 10 September 2012 Dennis Wright (SLAC)
Possible merits of high pressure Xe gas for dark matter detection C J Martoff (Temple) & P F Smith (RAL, Temple) most dark matter experiments use cryogenic.
Present and Future Cryogenic Dark Matter Search in Europe Wolfgang Rau, Technische Universität München CRESSTCRESST EURECA ryogenic are vent earch with.
Proportional Light in a Dual Phase Xenon Chamber
30 Ge & Si Crystals Arranged in verticals stacks of 6 called “towers” Shielding composed of lead, poly, and a muon veto not described. 7.6 cm diameter.
What’s the Matter in the Universe? Richard Schnee Syracuse University Quarknet Lecture July 13, 2012 The Search for Dark Matter.
Aldo IanniNNN05 April 8, Status and future prospects of Gran Sasso Aldo Ianni INFN Gran Sasso Laboratory NNN05 Aussois, April 7-9.
DRIFT II & DTM recent work 2010/11 UK: Sheffield, Edinburgh, STFC AIM: Directional Detection of WIMP Dark Matter - Identify a Galactic Signal US: Occidental,
ZEPLIN II Status & ZEPLIN IV Muzaffer Atac David Cline Youngho Seo Franco Sergiampietri Hanguo Wang ULCA ZonEd Proportional scintillation in LIquid Noble.
Status of DRIFT II Ed Daw representing the DRIFT collaboration: Univ. of Sheffield, Univ. of Edinburgh, Occidental College, Univ. of New Mexico Overview.
Dark Matter G. Chardin CEA/Saclay, DAPNIA. Motivations for non-baryonic Dark Matter Search - 1 Astrophysical measurements –“Dark” matter halo around the.
T. Frank for the CRESST collaboration Laboratori Nazionali del Gran Sasso C. Bucci Max-Planck-Institut für Physik M. Altmann, M. Bruckmayer, C. Cozzini,
TAUP2007, Sendai, 12/09/2007 Vitaly Kudryavtsev 1 Limits on WIMP nuclear recoils from ZEPLIN-II data Vitaly A. Kudryavtsev Department of Physics and Astronomy.
NSF Dark Matter Program P5 Meeting, Sept 24-25, Dark Matter Searches Summary of NSF Dark Matter Projects Direct Detection (including co-funds with.
Recommendations for Science at SNOLAB Andrew Hime On behalf of the Experiment Advisory Committee Aug. 17, 2005 SNOLAB Surface Building.
Direct Dark Matter Searches
 Dark matter forms a giant sea, enclosing the milky way. The earth and solar system like a small fish, swimming in it.  Dark Matter particle has a small.
Cryogenic particle detection at the Canfranc Underground Laboratory First International Workshop for the Design of the ANDES Underground Laboratory Centro.
APS April meeting Jacksonville, 2007 WIMP Search With SNOLAB Chris Jillings SNOLAB Staff Scientist For the DEAP-1 Collaboration.
Neutron scattering systems for calibration of dark matter search and low-energy neutrino detectors A.Bondar, A.Buzulutskov, A.Burdakov, E.Grishnjaev, A.Dolgov,
CDMS IIUCSB Direct Dark Matter Detection CDMS, ZEPLIN, DRIFT (Edelweiss) ICHEP 31 Amsterdam July 26, 2002 Harry Nelson Santa Barbara.
Cosmo02, Chicago september 2002 Maryvonne De Jésus 1 DARK-MATTER Direct Detection Maryvonne De Jésus IPN-Lyon/CNRS France
Underground Laboratories and Low Background Experiments Pia Loaiza Laboratoire Souterrain de Modane Bordeaux, March 16 th, 2006.
The EDELWEISS-II experiment Silvia SCORZA Université Claude Bernard- Institut de Physique nucléaire de Lyon CEA-Saclay DAPNIA/DRECAM (FRANCE), CNRS/CRTBT.
Véronique SANGLARD Université de Lyon, UCBL1 CNRS/IN2P3/IPNLyon Status of EDELWEISS-II.
WIMP search Result from KIMS experiments Kim Seung Cheon (DMRC,SNU)
Kamioka Kyoto We feel WIMP wind on the earth NEWAGE Direction-sensitive direct dark matter search with μ-TPC * 1.Dark.
DARK MATTER SEARCH Carter Hall, University of Maryland.
Ray Bunker (UCSB) – APS – April 17 th, 2005 CDMS SUF Run 21 Low-Mass WIMP Search Ray Bunker Jan 17 th -DOE UCSB Review.
I. Giomataris, CEA-Irfu-France
G. Gerbier Chinese-french workshop CPPM Marseille sept 2005 Dark Matter : overview of direct searches G. Gerbier CEA/Saclay, DAPNIA -Dark Matter WIMP.
Detecting the Directionality of Dark Matter via “Columnar Recombination” (CR) Technique An attractive, natural candidate for Dark Matter is the WIMP –
Potential for Dark Matter Direct Searches in Australia Professor Elisabetta Barberio The University of Melbourne.
Results from the LUX experiment and presentation of LUX-ZEPLIN Timothy John Sumner Imperial College London on behalf of the LUX and LZ collaborations Belgian.
Scintillating Bubble Chambers for Direct Dark Matter Detection Jeremy Mock On behalf of the UAlbany and Northwestern Groups 1.
Alex Howard, Imperial College Slide 1 July 2 nd 2001 Underground Project UNDERGROUND PROJECT – Overview and Goals Alex Howard Imperial College, London.
NEXT: A Neutrinoless 2  Experiment with a Gaseous XeTPC Thorsten Lux IFAE Barcelona in behalf of the NEXT Collaboration.
Leo Stodolsky 80th anniversary
From Edelweiss I to Edelweiss II
MIMAC MIcro-tpc MAtrix of Chambers ( 3He + CF4) A Large TPC for non baryonic Dark Matter search Daniel Santos Laboratoire de Physique Subatomique et.
Christopher M. Savage Fine Theoretical Physics Institute
Direct Search for Dark Matter with XENON100
Dark Matter Search With an Ultra-low Threshold Germanium Detector proposed by Tsinghua University Seoul National University Academia Sinica Qian Yue.
Special UCLA High Energy & Astro-Particle (HEAP) Seminar
UK Dark Matter Collaboration
Dark Matter in the Universe physics beyond the standard model
DAMA: an observatory for rare
University of South Dakota
Harry Nelson UCSB DUSEL Henderson at Stony Brook May 5, 2006
CRESST Cryogenic Rare Event Search with Superconducting Thermometers
Irina Bavykina, MPI f. Physik
XAX Can DM and DBD detectors combined?
Direct Dark Matter Searches
Non-Baryonic Dark Matter: From the CMB and axial direct detection
UCLA High Energy & Astro-Particle (HEAP) Seminar
Direct Detection of Dark Matter
Neutral and charged Higgsino as carriers of residual SUSY effects.
The Current and Future Status of the Search for Dark Matter
LUX: Shedding Light on Dark Matter
LUX: A Large Underground Xenon detector WIMP Search
Detecting WIMPs using Au-DNA Microarrays
Yue, Yongpyung, Korea Prospects of Dark Matter Search with an Ultra-Low Threshold Germanium Detector Yue, Yongpyung, Korea
- - Interpreting DAMA with Inelastic Dark Matter:
The Estimated Limits For A 5g LE-Ge Detector
Dark Matter Detection,Models and Constraints
Presentation transcript:

Dark Matter Direct Detection roadmap strategy G. Chardin, J. Jochum, A. Rubbia, N.Smith For the WG5 working group Amsterdam ASPERA Sept. 20-21

Dark Matter and Dark Energy Outstanding question : What is the Universe made of ? Ordinary (baryonic) matter only represents only ≈ 4% of the Universe energy content Amsterdam ASPERA Sept. 20-21

Amsterdam ASPERA Sept. 20-21 Weakly interacting massive particles long lived or stable particles left over from the BB Axions not discussed here thermoequilibrium abundance actual abundance The “WIMP miracle” MW ≈ 50-500 GeV <v> ≈ 300 km/s  ≈ 10-6-10-10 pbarn Amsterdam ASPERA Sept. 20-21

new elementary particles Dark Matter search for physics beyond the Standard Model new elementary particles Supersymmetry ??? Amsterdam ASPERA Sept. 20-21

Natural WIMP : SUSY Lightest particle Stable if SUSY exists and R-parity is conserved Direct detection: WIMP scattering off nuclei gaugino fraction: PMTs PEEK Supports Cathode Grids Waveshifter/Reflector Amsterdam ASPERA Sept. 20-21

Direct detection techniques After Drukier and Stodolsky, PRD 30 (1984) 2295 (and Goodman and Witten (1985) ) Direct detection techniques WIMP Elastic nuclear scattering Ge Ge, Si ≈ 20 % energy Ionization Xe, Ar, Ne Heat Al2O3, LiF • ≈ 100% detected energy • relatively slow • requires cryogenic detectors Light • ≈ few % detected energy • usually fast • no surface effects ? CaWO4, BGO ZnWO4, Al2O3 … NaI, Xe Amsterdam ASPERA Sept. 20-21

Possible WIMP Signatures Nuclear vs electronic recoil discrimination almost required now Annual flux modulation (tricky, most events close to threshold, small effect, Requires > 500 kg Ge target for > 5 years and 5  detection) Diurnal direction modulation (nice signature, but requires low pressure gaseous target, Not convincingly demonstrated yet No multiple interactions (usually only removes limited fraction of background) Recoil energy spectrum shape (exponential, rather similar to background…) Consistency between targets of different nuclei (essential once first signal is clearly identified) Amsterdam ASPERA Sept. 20-21

Experimental challenges Background suppression Deep underground sites Radio-purity of components Active/passive shielding Large target mass required ~ few keV energy threshold Stability and reproducibility Discriminate recoil populations Photons scatter off electrons WIMPs/neutrons off nuclei radon heavy nuclear recoils, alpha tails… Amsterdam ASPERA Sept. 20-21 Expected Energy Spectra for a 100 GeV WIMP, illustrating the importance of the choice of detector material

Main Wimp direct detection experiments • CDMS-II @ Soudan Mine (US project) • EDELWEISS-II (cryo Ge @ Fréjus)  EURECA • CRESST-II (cryo CaWO4, ZnW04) @ Gran Sasso  EURECA • XENON-10 @ Gran Sasso, ZEPLIN-II and -III @ Boulby  ELIXIR • ArDM @ Canfranc, WARP @ Gran Sasso  common Ar-Xe Design Study ? • DRIFT + MIMAC  CYGNUS • LIBRA (NaI) @ Gran Sasso, , NaIAD (Boulby), ANAIS (Canfranc) • IGEX @ Canfranc, HDMS/GENIUS-TF (Ge) @ Gran Sasso • CUORICINO/ CUORE (Te02) @ Gran Sasso • COUPP, SIMPLE, MACHe3, ORPHEUS (Bern) • XMASS, ELEGANT, LiF @Japan • (Future experiments: SuperCDMS, EURECA , XENON-100, GERDA, LUX… ) ZEPLIN-II, NaIAD, DRIFT EDELWEISS IGEX ROSEBUD ANAIS, ArDM CDMS XENON ZEPLIN-II MAJORANA WARP, COUPP DEAP, CLEAN ELEGANT, XMASS CRESST, WARP, XENON, HDMS/GENIUS DAMA/LIBRA CUORICINO/CUORE Amsterdam ASPERA Sept. 20-21

WG5 Dark Matter (direct detection only) Composition of the Working Group Laura BAUDIS • Pierluigi BELLI Yuryi BUNKOV • Gabriel CHARDIN (coord) Gilles GERBIER • Tom GIRARD Josef JOCHUM • Hans KRAUS Pierre de MARCILLAC • Claudio MONTANARI Fabrice PIQUEMAL • André RUBBIA Daniel SANTOS • Wolfgang SEIDEL Nigel SMITH (ApPEC PRC) • Neil SPOONER Tim SUMNER Nearly all European Dark Matter experiments represented, together with CDMS and XENON Amsterdam ASPERA Sept. 20-21

Amsterdam ASPERA Sept. 20-21 Main meetings of WG5 Valencia Nov. 7-8, 2006 meeting : ASPERA kick-off meeting ApPEC roadmap discussion Paris Feb. 1st, 2007 meeting: all major European groups represented CERN July 13th, 2007 meeting: all major European groups except WARP Amsterdam ASPERA Sept. 20-21

Amsterdam ASPERA Sept. 20-21 Main meetings of WG5 Paris Feb. 1st and CERN July 13th meetings: Presentation and discussion of basically all Direct Detection DM European projects Discussion of European and US roadmaps Definition of strategy and prioritization (CERN meeting) ASPERA Questionnaires + presentations + US and ApPEC roadmaps can be found on ASPERA Plone Website Amsterdam ASPERA Sept. 20-21

Projects discussed in WG5 Cryogenic: CRESST + EDELWEISS  EURECA Xenon TPC: XENON10, 100, ZEPLIN-II, -III  ELIXIR Argon TPC: ArDM, WARP  ? DRIFT + MIMAC  CYGNUS DAMA-1ton, ULTIMA, SIMPLE Underground facility ULISSE Amsterdam ASPERA Sept. 20-21

Edelweiss: event-by-event discrimination Charge + Heat Measurement Neutron + gamma calibration Nuclear recoil discrimination down to 20 keV threshold : -ray rejection > 99.99 % Amsterdam ASPERA Sept. 20-21

Charge + Light Measurement Nuclear recoil AmBe calibration XENON neutron and gamma calibrations Charge + Light Measurement Gamma calibration Nuclear recoil AmBe calibration Amsterdam ASPERA Sept. 20-21 J. Angle et al., astro-ph:0706.0039

“Dirty” liquid WARP 2.3 lt at LNGS Impressive > 107 background rejection factor Procurement of 39Ar depleted argon in future Amsterdam ASPERA Sept. 20-21

Experimental status and strategy Most experiments (below, XENON) are recording background events, and testing strategies to remove them Amsterdam ASPERA Sept. 20-21

Experimental status and strategy Goal ≈ 2018 10-10 pbarn Factor ≈ 300 progress in sensitivity still required compared to best present sensitivities CDMS XENON-10 Amsterdam ASPERA Sept. 20-21

Time evolution of sensitivity Rapid evolution of sensitivity of discriminating experiments (factor > 100 since 2000) (XENON, CDMS, CRESST, EDELWEISS, WARP, ZEPLIN-II…) But goals are still ≈2-3 orders of magnitude beyond present best performances (After Gaitskell) Amsterdam ASPERA Sept. 20-21

Amsterdam ASPERA Sept. 20-21 Experimental status Impressive progress has been realized over the last year by liquid target DM experiments (XENON, WARP, ZEPLIN-II) Cryogenic detector experiments (CDMS, CRESST, EDELWEISS) are progressing rapidly with their 10-kg stages The 10-8 pbarn “ SUSY-rich ” region should be reached within two years Amsterdam ASPERA Sept. 20-21

Experimental status and strategy Today, there exists several approaches towards 10-9 pbarn sensitivity Still, 10-10 pbarn represents ≈ 2.5 orders of magnitude improvement in sensitivity when compared to best present sensitivity (XENON) Important task: identifying a signal as Dark Matter WIMP => requires confirmed detection by more than one nuclear target => We recommend to pursue in parallel three main experimental lines: Ar, Xe, cryogenic detectors Amsterdam ASPERA Sept. 20-21

Experimental status and strategy It is therefore proposed to progress in two stages 1) Next 3-4 years, demonstrate/optimize discrimination strategy and sensitivity at ≈ 10-8 pbarn with 10-100 kg stages Design studies: EURECA, ELIXIR/Liquid Argon ArDM ton-scale detector + WARP-140 2) In ≈2010, decision on two (3?) complementary experiments with sensitivity in the 10-10 pbarn range In parallel, two main R&D activities: Clear demonstration of directional detector: CYGNUS Procurement of 39Ar depleted argon (underground natural gas, isotopic separation) Amsterdam ASPERA Sept. 20-21

Amsterdam ASPERA Sept. 20-21 R&D activities Nobody has demonstrated yet an experimental method able to reach with reasonable certainty 10-10 pbarn sensitivity (that would give access to fair fraction of SUSY models) Continuation of significant R&D activities during the first phase is therefore essential Main goal : improvement of background rejection and identification performances Clear demonstration of directionality and, if possible, of track sense determination would prepare the final stage : demonstration of galactic origin of WIMP signal if observed in “ first detection ” experiments Amsterdam ASPERA Sept. 20-21

Towards experiments at 10-10 pbarn sensitivity Recommendation of common experimental effort on well-equipped neutron scattering facility (e.g. TU-Muenchen, or Amande Grenoble) Precision calibration is necessary to assess the discrimination and energy calibration performances of competing techniques High statistics neutron calibration of small-scale prototypes of all main experiments Calibration of nuclear recoils at low energy of WARP and ZEPLIN, and to lesser extent XENON, not yet clear and should be improved In parallel, design study phase of ultra-low background deep underground laboratory, active rejection and identification of showers (ULISSE) Amsterdam ASPERA Sept. 20-21

Underground facility for DM search Design study phase of ultra-low background deep underground laboratory, active rejection and identification of showers (ULISSE) This Design Study can be used by all Dark Matter direct detection experiments Active shower rejection ULISSE Design Study Underground DM facility Amsterdam ASPERA Sept. 20-21

Funding requests European DM program Design studies (2008-2011) for: cryogenic (CRESST + EDELWEISS  EURECA) liquid noble targets (ArDM, WARP) + (EU XENON + EU ZEPLIN) experiments Unification of same target experiments recommended Importance of ApPEC coordination In parallel to these two main lines, dedicated R&D on directionality (CYGNUS) Overall, 20 M€ investment first stage program over next 3-4 years In ≈ 2010, decision on 2 (if possible 3) DM experiments with total investment budget in the 100 M€ range Amsterdam ASPERA Sept. 20-21

Projects Investment Costs 2008 - 2018 1303 FTE Recommendations: Cryogenic => EURECA Noble Liquid Gases => ELIXIR, WARP, ArDM (unify!) R&D (Cygnus, Ulisse, ..) Amsterdam ASPERA Sept. 20-21

Investment Costs Recommended Projects Amsterdam ASPERA Sept. 20-21

Staff for Recommended Projects Amsterdam ASPERA Sept. 20-21

Conclusions • Progress in two stages (Design, deployment) • Two main techniques • R&D activities • Note: two Design Studies priorities of ApPEC If CTA and EURECA not funded by Europe, fundamental that they are by ApPEC Agreement of CDMS, XENON, CRESST, EDELWEISS to make ntuples (low-background data and calibrations) in open access data after typically one year or 18 month Amsterdam ASPERA Sept. 20-21