Towards One Tonne WIMP Direct Detectors: Have we got what it takes?
|
|
- Annabella Pearson
- 5 years ago
- Views:
Transcription
1 Towards One Tonne WIMP Direct Detectors: Have we got what it takes? Center for Particle Astrophysics UC Berkeley source at Gaitskell
2 Future Reach / Lower limit on quark σ Genino 100 kg Ge in 5 m tank LN2 Genius 100 kg Ge in 14 m tank LN2 Shaded regions: Unconstrained MSSM ~1 event/kg/d CDMS Latest Feb 2000 Now limited by shallow site CDMS II 5 kg Ge at Soudan ZEPLIN 6 kg Xe at Boulby ~1 event/kg/yr 0 < M 3 < 1000 GeV msugra & Naturalness 95 < m 0 < 1000 GeV Mandic, Gondolo, < A 0 < 3000 GeV Murayama, Pierce 1.8 < tan(β) < 25 sign of µ < Ω h 2 < 1 CryoArray 1 tonne event by event discrim. ~ 1 event/100 kg/yr see also Ellis et al. hep-ph
3 Direct Detection: History & Future 90% CL Limit on Cross section for 60 GeV WIMP (scalar coupling) Homestake (87) Oroville (88) [m=20 GeV] ~1 event kg -1 day -1 Edelweiss (98) Heidelberg-Moscow (94) UKDMC (96) [m=100 GeV] DAMA (98/00) Heidelberg-Moscow (98) DAMA (96) CDMS SUF (99) CDMS SUF (00) NOW CDMS SUF (T) Ge NaI Cryodet Liq Xe (T) Target Signal ~1 event kg -1 yr -1 Different Colours Indicate Different Technologies GENINO (T) 100 kg Ge Diode CDMS Soudan (T) 7 kg Ge+Si Cryodet [m =?? GeV - if significantly better limit obtained at LHC ~1 event 100 kg -1 yr -1 different mass] GENIUS (T) 100 kg Ge Diode CryoArray (T) tonne Cryodet Not meant to be a complete list - see rjg
4 Achieving Detector Mass Scale up to 1 tonne (not accounting for gain/loss due to Form Factor- threshold relationship) LiqXe 300 litres fiducial PMT coverage for 3-6 m 2 Ge Diode ~400 x 2.5 kg Ge Semiconductor [~$6M/tonne (unenriched)] Cryogenic Typical crystals kg; detectors Industrial Fab cost yet to be established (CUORE proposal) Gas TPC 10,000 m 3 gas 1 m 40 torr is 2.3 g x RMM (e.g. Ar is 92 g/m 3 )
5 Problem: Performance -> Production Mass Recent challenge has been to demonstrate discrimination techniques Now it is time to solve some of problems of scale up Production issues (scales of collaboration) Good experience of running technology underground
6 Misidentified events Inverted Rare Event Search Inverted approach: apply rare event search techniques to background Looking for anomalous events becomes like a rare event search (Dave Wark, SNO) in amongst signal Importance of having as many handles on events as we can muster Finite ranges for ratios of coincident Large separation Not decay times (event by event difficult) Events must stay above noise in all channels Tendency to confuse events Tell-tale signal for DM Ann. mod - tough <5% mass, systematics require lower background Directionality - tough to achieve mass in gas Kinematics (Recoil spectra in different target material) We need a number of experiments!!
7 Misidentified events Inverted Rare Event Search (2) It is clear that we will need to go through a period of seeing nothing Before we are ready to see something Ladder - we need to make transition to extended periods of seeing nothing before can justify building a bigger version. Challenge: Publication of paper with no events. (Offer of a keg of beer to experimentalists who set new (best) limit using no events) I sometimes envy the theorists 15 orders of magnitude on scale Improvements in experimental reach (2 orders of magnitude has been hard fort)
8 2nd Kind of Limit on Threshold of Discrimination Background (e.g. Gamma or Surface Betas) Lateral spread of lines simulates noise x 2 x 2 For 1st case - (see CDMS talks on surface electron confusion with nuclear recoils) 1st Kind Signal (Nuclear Recoil) 2nd Kind In 2nd case - will single event in x 1 only be background free? Effective threshold raised due to event-by-event discrimination confused by noise x 1 In this region x 2 channel for signal events are buried in noise: Example where 2nd limit on discrimination may be relevant: CRESST x1(phonon) x2(photon) CaWO 4 Gamma: x1=50 kevee x2~350 evdet [based on current # s - see CRESST II talk] Neutron: x1=50 kevee&r x2~50 evdet (close to noise threshold) Assumes 0.7% energy of electron recoil signal detected in photons for gamma event and QF (established for O nuclei recoils relative to gammas) is 14% x 1
9 Influence of Coherence & Form Factor (q=0) Rate~A Xe, 127 I (σ= cm 2, m=300 GeV) 73 Ge Rate kg -1 day Ar,~ 32 S Ge=15 kevee (30%QF) Xe=10 kevee (20%QF) I=4.5 kevee (9%QF) Solid line is integrated rate above threshold (dotted is differential rate) Recoil Energy Threshold [kevr]
10 SUSY/Weak Scale Note that LHC is unlikely to give LSP mass directly Can argue that DM direct search can be used to fix this parameter (Tovey) DarkSUSY Clear that channels all Annihilation Rate (Ω m error < factor 2 (?)) However, particular channel branching ratio may have many orders of magnitude range Direct - Cross-section on quarks Indirect - Decay BR -> ν, γ, e & Model of density enhancements Incredible range of experimental techniques that are now/on the verge producing new limits Look outside SUSY? WIMPs - weak scale (framework?) Mass prediction 10 TeV (unitarity)
11 Projected Sensitivity CDMS II Background table Background rejection & Statistical subtraction Based on exposure (counts) 2500 kg-days Assumptions in forecasts formally outlined e.g. Will include projected limit plots posted at & Show same exercise for 1 tonne Extend statistics
12 CDMS II Soudan (2070 mwe depth) Goal: 0.01 evt/kg/day= evt/kg/kev/day Currently Deep site should give this Background source Shielded Muon After detector Veto rejection γ s, external radioactivity Background subtracted Systematics γ s, cosmics in shield Currently 0.05 in best detector Continue to push on surface contamination γ s, internal single scatters % γ rejection Total γ s ~20 kevts ~100 evts subtraction ~16 evts β s, surface contamination % β rejection n s, external radioactivity n s, cosmics in shield n s, cosmics in rock Total neutrons Total background /kg /day Special shield against high energy neutrons Tn = MeV are important ~1 per 0.25 kg detector per year Units: /kg/kev/day at 15 kevr (5kg Ge, 2kg Si kg.days in Ge) rjg
13 Neutrons from Muons Neutron production ~ Muon Flux E µ ~Depth 0.47 means Soudan to x15 (negligible for other ratios) Soudan Site Relative Muon Flux Soudan/WIPP x 20 Boulby x 2 Gran Sasso x 1 Frejus x 1/2 Aglietta et.al. Nuove Cimento 12, N4, page 467
14 Neutron Penetration (Water) Attenuation of High Energy Neutron Flux in water shield Monte Carlo Simulations Performed by Thushara Perera, CWRU using GEANT/MICAP/FLUKA 300 MeV 10 MeV 1 MeV Energy x10 atten x100 atten [MeV] [cm] [cm] (10 events) Typical multiplicity of 1-few Water 300 MeV neutron injected in +z direction
15 Neutron Penetration (Fe vs Water) Summary Fe (KE MeV) 100 cm x10 atten (>1 MeV) 200 cm x10 atten (>10 kev) 300 MeV 100 kev 10 kev (only 1 event shown for clarity) Multiplicity of neutrons generated per event is higher (~20) Fe (10 events) Typical multiplicity of 1-few Water 300 MeV 10 MeV 1 MeV
16 Shielding Eff x Flux - Balanced in range MeV Neutron production (fluxes for Soudan) Energy Wall Flux Pentration Flux inside [MeV] cm wate[/m2/yr] % % % % 0.9
17 Soudan - outer Pb and poly shielding Base sections of lead and polyethylene shields test assembly at UCSB who built shield. Note Poly-Pb-Poly layers
18 Neutron Subtraction WIMP /Neutron Kinematics/Cross-section e.g. Mixed Ge & Si targets Multiple Scattering Position / timing (ns) resolution Neutron Capture (e.g. MACHe3 3H) in bulk
19 CDMS II Soudan (2070 mwe depth) Goal: 0.01 evt/kg/day= evt/kg/kev/day Currently Deep site should give this Background source Shielded Muon After detector Veto rejection γ s, external radioactivity Background subtracted Systematics γ s, cosmics in shield Currently 0.05 in best detector Continue to push on surface contamination γ s, internal single scatters % γ rejection Total γ s ~20 kevts ~100 evts subtraction ~16 evts β s, surface contamination % β rejection n s, external radioactivity n s, cosmics in shield n s, cosmics in rock Total neutrons Total background /kg /day Special shield against high energy neutrons Tn = MeV are important ~1 per 0.25 kg detector per year Units: /kg/kev/day at 15 kevr (5kg Ge, 2kg Si kg.days in Ge) rjg
20 Nuclear Recoil Discrimination - Event by Event Nuclear recoils arise from WIMPs Neutrons NOT A SIMULATION! 1334 gamma events, 616 neutron events Gammas (external source) Electron Recoils arise from photons electrons alphas (Typical Background) Neutrons (external source) Ionization yield ionization/recoil energy strongly dependent on type of recoil Recoil energy Phonons give full recoil energy Phonon Trigger Threshold
21 CryoArray (Sensitivity <1 per 100 kg-yr, s~10-46 cm -2 ) Scale up to 1 tonne detector with target (90%CL) <1 evt per 100 kg-yr (improvement relative to CDMS II figures) Reduce γ/β backgrounds by factor 20 γ > cts/kevee -1 kg -1 day -1 (This compares to kevee -1 kg -1 day kev for HMDS) β > cts/kevee -1 kg -1 day -1 (Challenge to survey surfaces to this sensitivity) Improve γ/β rejection by factor 10 γ 99.5% -> 99.95% (1 in 2000) [Currently showing 99.9%] β 95% -> 99.5% (1 in 200) [Currently showing >95%] For comparison: Without discrimination needs ~10 4 reduction in background from present (HM) levels
22 Cosmogenic Tritium Created ~200 3 H kg -1 day -1 at sea level Equilibrium concentration 1.4x10 6 atoms kg -1 Avignone et al. Nucl. Phys. B (Proc. Suppl.) 28A (92) 280 Example: GENIUS Target: 10 days at SL+3 years of cooling 1700 atoms 3 H 11 kev-19 kevee 15 evts kg.yr -1 Would dominate and create effective WIMP threshold 60 kevr Compare with 3x10-2 kev -1 kg.yr -1 Surface contamination 3H less of an issue for p-type contacts (dead regions) cover most of det. surface Counts /kev/day/10 5 atoms 15.5 cts/day/10 5 atoms
23 kevee (Electron Equivalent) -> kevr (Nucl Recoil) DAMA ROM2F/2000/01 Preprint Figure 1 2 kevee 100 kg NaI == 22 kevr 1 count kevee -1 kg -1 day -1 == 0.09 cnt kevr -1 Heidelberg-Moscow 2.7 kg HP Ge CDMS 0.1 count kevee -1 kg -1 day -1 == 0.03 cnt kevr count kev -1 kg -1 day -1 == 0.1 cnt kevr kevee == 40 kevr Already Recoil Energy
24 rjg
25 Direct Detection: History & Future 90% CL Limit on Cross section for 60 GeV WIMP (scalar coupling) Homestake (87) Oroville (88) [m=20 GeV] ~1 event kg -1 day -1 Edelweiss (98) Heidelberg-Moscow (94) UKDMC (96) [m=100 GeV] DAMA (98/00) Heidelberg-Moscow (98) DAMA (96) CDMS SUF (99) CDMS SUF (00) NOW CDMS SUF (T) Ge NaI Cryodet Liq Xe (T) Target Signal ~1 event kg -1 yr -1 Different Colours Indicate Different Technologies GENINO (T) 100 kg Ge Diode CDMS Soudan (T) 7 kg Ge+Si Cryodet [m =?? GeV - if significantly better limit obtained at LHC ~1 event 100 kg -1 yr -1 different mass] GENIUS (T) 100 kg Ge Diode CryoArray (T) tonne Cryodet Not meant to be a complete list - see rjg
Dark Matter. and TPC Technologies
Dark Matter and TPC Technologies The Physics Case for WIMPs Status of the Field:event by event discrimination Elements of a roadmap Bernard Sadoulet Dept. of Physics /LBNL UC Berkeley UC Institute for
More informationSuperCDMS SNOLAB: A G2 Dark Matter Search. Ben Loer, Fermilab Center for Particle Astrophysics On behalf of the SuperCDMS Collaboration
SuperCDMS SNOLAB: A G2 Dark Matter Search Ben Loer, Fermilab Center for Particle Astrophysics On behalf of the SuperCDMS Collaboration A bit of background Astronomical data at all scales indicates dark
More informationTechnical Specifications and Requirements on Direct detection for Dark Matter Searches
Technical Specifications and Requirements on Direct detection for Dark Matter Searches Jin Li THU/IHEP Symposium of the Sino-German GDT Cooperation 04/08/2013 Tübingen Outline Introduction Direct detection
More informationLatest Results on Direct Detection of Dark Matter WIMPs - CDMS & SuperCDMS
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
More informationThe Search for Dark Matter with the XENON Experiment
The Search for Dark Matter with the XENON Experiment Elena Aprile Columbia University Paris TPC Workshop December 19, 2008 World Wide Dark Matter Searches Yangyang KIMS Homestake LUX SNOLAB DEAP/CLEAN
More informationDirect Detection in the next five years: Experimental challenges and Phonon Mediated Detectors
Direct Detection in the next five years: Experimental challenges and Phonon Mediated Detectors Complementarity between Dark Matter Searches & Collider Experiments Miniworkshop before SUSY06 at Irvine -
More informationarxiv:astro-ph/ v1 24 Jun 2004
LATEST RESULTS OF THE EDELWEISS EXPERIMENT arxiv:astro-ph/46537v 24 Jun 24 V. SANGLARD for the Edelweiss collaboration Institut de Physique Nucléaire de Lyon, 4 rue Enrico Fermi, 69622 Villeurbanne, France
More informationMajorana - DM Summary of Issues
Majorana - DM Smmary of Isses Brown University, Department of Physics see information at http://majorana.pnl.gov Gaitskell v8 Projected Sensitivity Basic BG Model Assmptions 5 mdr flat, 1 kev threshold
More informationMeasurement of 39 Ar in Underground Argon for Dark Matter Experiments
Measurement of 39 Ar in Underground Argon for Dark Matter Experiments Jingke Xu Princeton University June 7 th, 2013 1 Evidences for Dark Matter Rotation Curve Gravitational Lensing CMB Power Spectrum
More informationCryogenic Detectors Direct Dark Matter Search. Dark Matter
Cryogenic Detectors Direct Search Matter in the Universe - Composition ν too light => most of the is cold Ωmat = 0.27 0.04 u d of so far unknown weakly interacting, massive particles WIMPs normal baryonic
More informationA survey of recent dark matter direct detection results
A survey of recent dark matter direct detection results I where we stand II recent results (CDMS, XENON10, etc) III DAMA results IV a bit about modulation V issues with DAMA results VI what to look for
More informationStatus of Dark Matter Detection Experiments
Status of Dark Matter Detection Experiments Debasish Majumdar Astroparticle Physics and Cosmology Division Saha Institute of Nuclear Physics Kolkata WIMP Hunting Going beyond gravity, three ways to detect
More informationDirect Detection of Dark Matter with LUX
Direct Detection of Dark Matter with LUX we are a collaboration of 50+ scientists, please see http://lux.brown.edu for more information Peter Sorensen Lawrence Livermore National Laboratory DNP October
More informationEsperimenti bolometrici al Gran Sasso: CUORE e CRESST
Esperimenti bolometrici al Gran Sasso: CUORE e CRESST Marco Vignati 24 Ottobre 2011 0νDBD in Theory Nuclear process: (A,Z) (A,Z+2) + 2 e - Can only happen if lepton number is not conserved. The decay probability
More informationSensitivity and Backgrounds of the LUX Dark Matter Search
Sensitivity and Backgrounds of the LUX Dark Matter Search 1 LUX Goal: Direct Detection of Dark Matter WMAP 5-year data (2008) gives matter densities (Ω) based on best fit to Λ-CDM cosmological model: Ω
More informationDown-to-earth searches for cosmological dark matter
Down-to-earth searches for cosmological dark matter Carter Hall, University of Maryland October 19, 2016 Astrophysical evidence for dark matter Galaxy cluster collisions Rotation curves Ω 380,000 years
More informationDirect Dark Matter Search with Noble Liquids
Direct Dark Matter Search with Noble Liquids Marc Schumann Physik Institut, Universität Zürich Recontres de Moriond 2012, Cosmology Session, La Thuile, March 2012 marc.schumann@physik.uzh.ch www.physik.uzh.ch/groups/groupbaudis/xenon/
More informationSuperCDMS: Recent Results for low-mass WIMPS
SuperCDMS: Recent Results for low-mass WIMPS David G. Cerdeño Institute for Theoretical Physics Universidad Autónoma de Madrid for the SuperCDMS Collaboration Hints for low-mass WIMPs in direct detection
More informationCurrent status of LUX Dark Matter Experiment
Current status of LUX Dark Matter Experiment by A. Lyashenko Yale University On behalf of LUX collaboration LUX Large Underground Xenon experiment LUX Collaboration: Yale, CWRU, UC Santa Barbara, Brown,
More informationDirect Dark Matter Searches
Direct Dark Matter Searches Marc Schumann Physik Institut, Universität Zürich What is? Invisibles12, GGI Florence, June 27th 2012 marc.schumann@physik.uzh.ch www.physik.uzh.ch/groups/groupbaudis/xenon/
More informationShedding Light on Dark Matter from Deep Underground with XENON. Kaixuan Ni (Columbia)
Shedding Light on Dark Matter from Deep Underground with XENON Kaixuan Ni (Columbia) University of Maryland, 11-25-2008 A well-known mystery for astronomers Fritz Zwicky, The Astrophysical Journal, 85
More informationBackground Characterization and Rejection in the LZ Detector. David Malling Brown University IDM 2012 July 25, 2012
Background Characterization and Rejection in the LZ Detector David Malling Brown University IDM 2012 July 25, 2012 LZ Construction 2 Background Sources Ti cryostats 1500 kg
More informationResults from 730 kg days of the CRESST-II Dark Matter Search
Results from 730 kg days of the CRESST-II Dark Matter Search Federica Petricca on behalf of the CRESST collaboration: Max-Planck-Institut für Physik, München TU München University of Oxford Universität
More informationNEUTRON BACKGROUND STUDIES FOR THE EDELWEISS WIMP SEARCH
NEUTRON BACKGROUND STUDIES FOR THE EDELWEISS WIMP SEARCH G. CHARDIN AND G. GERBIER FOR THE EDELWEISS COLLABORATION DSM/DAPNIA/SPP, CEA/Saclay. F-91191 Gif-sur-Yvette Cedex, France E-mail: gabriel.chardin@cea.fr
More informationWIMP EXCLUSION RESULTS FROM THE CDMS EXPERIMENT
WIMP EXCLUSION RESULTS FROM THE CDMS EXPERIMENT P.L. BRINK, L. BAUDIS, B. CABRERA, J.P. CASTLE, C. CHANG AND T. SAAB Department of Physics, Stanford University, Stanford, CA 94350, USA R. J. GAITSKELL
More informationLUX: A Large Underground Xenon detector. WIMP Search. Mani Tripathi, INPAC Meeting. Berkeley, May 5, 2007
LUX: A Large Underground Xenon detector WIMP Search Mani Tripathi INPAC Meeting Berkeley, New Collaboration Groups formerly in XENON10: Case Western, Brown, Livermore Natl. Lab (major fraction of the US
More informationLow energy neutron propagation in MCNPX and GEANT4
Low energy neutron propagation in and R. Lemrani a M. Robinson b V. A. Kudryavtsev b M. De Jesus c G. Gerbier a N. J. C. Spooner b arxiv:hep-ex/06030 v1 17 Jan 2006 a DAPNIA-SPP, CEA-Saclay, Gif-Sur-Yvette,
More informationRecent results from the UK Dark Matter Search at Boulby Mine.
Recent results from the UK Dark Matter Search at Boulby Mine. Nigel Smith Rutherford Appleton Laboratory on behalf of the UK Dark Matter Collaboration (Imperial College, Sheffield, RAL) NaI scintillation
More informationDARK MATTER SEARCHES
DARK MATTER SEARCHES N.J.C. SPOONER Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH E-mail: n.spooner@sheffield.ac.uk A brief review is presented
More informationThe GERmanium Detector Array
The GERmanium Detector Array n n ν=v p e - e - p Outline: Exp. issues of 0νββ-decay of 76 Ge Concept of GERDA Status of the experiment Summary and conclusions Kevin Kröninger (Max-Planck-Institut für Physik,
More informationUCLA Dark Matter 2014 Symposium. Origins and Distributions of the Backgrounds. 15 min
S. Fiorucci Brown University UCLA Dark Matter 2014 Symposium Origins and Distributions of the Backgrounds 15 min What is a signal for LUX? Nuclear recoil Single scatter Signal Low energy, typically < 25
More informationDark Matter Detection with XENON100 Accomplishments, Challenges and the Future
Dark Matter Detection with XENON0 Accomplishments, Challenges and the Future http://xenon.astro.columbia.edu Kaixuan Ni Columbia University TeV Particle Astrophysics IHEP, Beijing, Sep.4-8, 008 The Challenges
More informationThe Search for Dark Matter. Jim Musser
The Search for Dark Matter Jim Musser Composition of the Universe Dark Matter There is an emerging consensus that the Universe is made of of roughly 70% Dark Energy, (see Stu s talk), 25% Dark Matter,
More informationBackground Modeling and Materials Screening for the LUX and LZ Detectors. David Malling Brown University LUX Collaboration AARM Meeting February 2011
Background Modeling and Materials Screening for the LUX and LZ Detectors David Malling Brown University LUX Collaboration AARM Meeting February 2011 1 Summary LUX screening program limits background contributions
More informationDirekte Suche nach Dark Matter
Direkte Suche nach Dark Matter WIMP über elastische Streuung an Kernen HDMS Ge 10% energy Ionization Ge, Si Edelweiss, CDMS liquid Xe Zeplin-2, US-Xenon NaI, liqu.xe Target Light 1% energy fastest no surface
More informationLight Dark Matter and XENON100. For the XENON100 Collaboration Rafael F. Lang Columbia University
Light Dark Matter and XENON100 For the XENON100 Collaboration Rafael F. Lang Columbia University rafael.lang@astro.columbia.edu The XENON Collaboration ~60 scientists from 12 institutions: University of
More informationSearch for Low Energy Events with CUORE-0 and CUORE
Search for Low Energy Events with CUORE-0 and CUORE Kyungeun E. Lim (on behalf of the CUORE collaboration) Oct. 30. 015, APS Division of Nuclear Physics meeting, Santa Fe, NM The CUORE Experiment CUORE
More informationDark Matter Detection and the XENON Experiment. 1 Abstract. 2 Introduction
Dark Matter Detection and the XENON Experiment Elena Aprile Physics Department and Columbia Astrophysics Laboratory Columbia University New York, New York 10027 1 Abstract Observations on all fronts strongly
More informationSuperCDMS at SNOLAB. What is CDMS? Technical Progress. Collaboration. Funding. Schedule and Needs. Why is SuperCDMS 25 kg timely?
What is CDMS? SuperCDMS at SNOLAB Why is SuperCDMS 25 kg timely? Technical Progress CDMS II running at Soudan (4.5 kg Ge) Detectors Cryogenics Backgrounds Electronics Infrastructure Collaboration Addition
More informationDirect Search for Dark Matter
Direct Search for Dark Matter Direct Dark Matter Search Dark Matter in the Universe Ω = 0.23 non-baryonic not neutrinos physics beyond the standard model thermal relics from Big Bang weakly interacting
More informationThe Direct Search for Dark Matter
picture: Thomas Tuchan The Direct Search for Dark Matter with special emphasis on the XENON project Rafael F. Lang Purdue University rafael@purdue.edu IPMU Tokyo, March 8, 2013 1 baryon fraction Dark Matter
More informationCDMS and SuperCDMS. SLAC Summer Institute - CDMS. August 2, 2007 Blas Cabrera Co-Spokesperson CDMS & Spokesperson SuperCDMS
CDMS and SuperCDMS SLAC Summer Institute August 2, 2007 Blas Cabrera Co-Spokesperson CDMS & Spokesperson SuperCDMS CDMS-II science results - less than 1 evt / kg of Ge / month Status of CDMS-II 5-Tower
More informationLow Background Experiments and Material Assay. Tessa Johnson NSSC Summer School July 2016
Low Background Experiments and Material Assay Tessa Johnson NSSC Summer School July 2016 Outline How do we detect particles? Some interesting questions relating to particle physics How can particle detection
More informationStudies of the XENON100 Electromagnetic Background
Studies of the XENON100 Electromagnetic Background Daniel Mayani Physik-Institut University of Zurich PhD Seminar PSI, August 26-27, 2015 Searching for elusive particles The main challenge for experiments
More informationDark Matter Searches. Marijke Haffke University of Zürich
University of Zürich Structure Ι. Introduction - Dark Matter - WIMPs Ι Ι. ΙΙΙ. ΙV. V. Detection - Philosophy & Methods - Direct Detection Detectors - Scintillators - Bolometer - Liquid Noble Gas Detectors
More informationSearch for Weakly Interacting Massive Particles with CDMS and XENON
Search for Weakly Interacting Massive Particles with CDMS and XENON Elena Aprile 1,2, Laura Baudis 3,4, Blas Cabrera 5,6 1 Physics Department and Columbia Astrophysics Laboratory, Columbia University,
More informationBackground simulations and shielding calculations
Background simulations and shielding calculations Vitaly A. Kudryavtsev University of Sheffield Contributions from many others Outline Note 1: results are relevant to many experiments and techniques (mainly
More informationDavid Reyna Belkis Cabrera-Palmer AAP2010, Japan
David Reyna Belkis Cabrera-Palmer AAP2010, Japan Sandia is a multiprogram laboratory operated by Sandia Corporation, a Lockheed Martin Company, for the United States Department of Energy s National Nuclear
More informationLatest results of EDELWEISS II
Latest results of EDELWEISS II Ana Torrentó CEA/IRFU/SPP Saclay Rencontres de Moriond 2011 «EW and Unified Theories» WIMP search Motivated by the «WIMP miracle» Very small rate of WIMPnucleus scattering
More informationBackground Studies for the XENON100 Experiment. Alexander Kish Physics Institute, University of Zürich Doktorandenseminar August 30, 2010 UZH
Background Studies for the XENON100 Experiment Alexander Kish Physics Institute, University of Zürich Doktorandenseminar August 30, 2010 UZH The XENON dark matter search program Target Volume 62 kg Total
More informationDirect dark matter search using liquid noble gases
Direct dark matter search using liquid noble gases Teresa Marrodán Undagoitia marrodan@physik.uzh.ch Physik Institut Universität Zürich Texas Symposium 2010, Heidelberg, 09.11.2010 Teresa Marrodán Undagoitia
More informationAfter LUX: The LZ Program. David Malling, Simon Fiorucci Brown University APS DPF Conference August 10, 2011
After LUX: The LZ Program David Malling, Simon Fiorucci Brown University APS DPF Conference August 10, 2011 The LZ Program LZ LUX-ZEPLIN LUX (14 U.S. institutions) + new collaborators from ZEPLIN, other
More informationBackground and sensitivity predictions for XENON1T
Background and sensitivity predictions for XENON1T Marco Selvi INFN - Sezione di Bologna (on behalf of the XENON collaboration) Feb 19 th 016, UCLA Dark Matter 016 1 Outline Description of the detector;
More informationDarkSide-50: performance and results from the first atmospheric argon run
DarkSide-50: performance and results from the first atmospheric argon run Yann Guardincerri on behalf of the DarkSide Collaboration August 27th, 2014 1 / 21 DarkSide Direct detection search for WIMP dark
More informationLARGE UNDERGROUND XENON
LARGE UNDERGROUND XENON Cláudio Silva (LIP Coimbra) On behalf of the LUX Collaboration IDPASC Dark Matter Workshop 17 December 2011 1 THE LUX COLLABORATION Collaboration was formed in 2007 and fully funded
More informationPANDA-X A New Detector for Dark Matter Search. Karl Giboni Shanghai Jiao Tong University
PANDA-X A New Detector for Dark Matter Search Karl Giboni Shanghai Jiao Tong University Seminar at KEK, Tsukuba Japan 3 February, 2011 Jin Ping Laboratory Newly constructed deep underground lab In the
More informationDirect Search for Dark Matter
Direct Search for Dark Matter Direct Dark Matter Search Dark Matter in the Universe Ω = 0.23 non-baryonic not neutrinos physics beyond the standard model thermal relics from Big Bang weakly interacting
More informationSensitivity of sodium iodide cryogenic scintillation-phonon detectors to WIMP signals
Journal of Physics: Conference Series PAPER OPEN ACCESS Sensitivity of sodium iodide cryogenic scintillation-phonon detectors to WIMP signals To cite this article: M Clark et al 2016 J. Phys.: Conf. Ser.
More informationThe 46g BGO bolometer
Nature, 3 The g BGO bolometer 1 Photograph of the heat [g BGO] and light [Ge; =5 mm] bolometers: see Fig. 1c for description Current events: Amplification gains: 8, (heat channel) &, (light channel). The
More informationDark Matter Search Results from the Silicon Detectors of the Cryogenic Dark Matter Search Experiment
Dark Matter Search Results from the Silicon Detectors of the Cryogenic Dark Matter Search Experiment Kevin A. McCarthy Massachusetts Institute of Technology On behalf of the SuperCDMS and CDMS Collaborations
More informationDirect Dark Matter and Axion Detection with CUORE
Direct Dark Matter and Axion Detection with CUORE Europhysics Conference on High-Energy Physics 2011 Cecilia G. Maiano on behalf of CUORE collaboration Contents The Bolometric Technique The CUORE experiment
More informationThe XENON Dark Matter Project: Status of the XENON100 Phase. Elena Aprile Columbia University
The XENON Dark Matter Project: Status of the XENON100 Phase Elena Aprile Columbia University 8th UCLA Symposium Marina del Rey, Feb 22, 2008 The XENON Dark Matter Phased Program Detect WIMPS through their
More informationNuclear Recoil Techniques for the Detection of Dark Matter
Nuclear Recoil Techniques for the Detection of Dark Matter Uwe Oberlack Rice University Houston, TX The Cosmic Recipe Astrophysical observations reveal a dark universe. Cosmic Microwave Background. Geometry
More informationNeutron background in underground particle astrophysics experiments
Neutron background in underground particle astrophysics experiments V. A. Kudryavtsev Department of Physics and Astronomy University of Sheffield for ILIAS and the UK Dark Matter Collaboration LRT2006-01/10/2006
More informationCryodetectors, CRESST and Background
Cryodetectors, CRESST and Background A cryogenic detector for Dark Matter with heat (phonon) readout and light (scintillation) readout MPI, TUM, Oxford, Tübingen, LNGS What we re looking for: M W imp =
More information=> Ωmatter >> Ωbaryon
Cryogenic Detectors Direct Search Cryogenic Detectors CRESST Project Cosmic Microwave Background Matter-Density Ωmatter Anisotropy: Angular scale => geometry, Ωtot Wilkinson Microwave Anisotropy Probe
More informationDesign, Construction, Operation, and Simulation of a Radioactivity Assay Chamber
Design, Construction, Operation, and Simulation of a Radioactivity Assay Chamber Wesley Ketchum and Abe Reddy EWI Group, UW REU 2006 Outline Neutrino Physics Background Double Beta Decay and the Majorana
More informationCDMS-II to SuperCDMS
CDMS-II to SuperCDMS WIMP search at a zeptobarn Tobias Bruch University of Zürich 5 th Patras Workshop on Axions,WIMPs and WISPs University of Durham, 13 July 2009 CDMS-II 5 Tower setup 5 Towers a 6 detectors
More informationRecent results from the second CDMSlite run and overview of SuperCDMS SNOLAB project
Recent results from the second CDMSlite run and overview of SuperCDMS SNOLAB project SLAC National Accelerator Laboratory/Kavli Institute for Particle Astrophysics and Cosmology, Menlo Park, CA 94025,
More informationWIMP: direct and indirect detection Results and perspectives
WIMP: direct and indirect detection Results and perspectives G. Gerbier CEA/Saclay, DAPNIA LSM (Fréjus Lab) - Introduction for -not so- pedestrians - Summary of direct detection exp status : few focus
More informationarxiv:astro-ph/ v1 15 Feb 2005
The XENON Dark Matter Experiment Elena Aprile (on behalf of the XENON collaboration) Physics Department and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027 age@astro.columbia.edu
More informationThe next generation dark matter hunter: XENON1T status and perspective
The next generation dark matter hunter: XENON1T status and perspective A. Rizzo a on behalf of the XENON Collaboration Department of Astrophysics, Columbia University in the City of New York, USA Abstract.
More informationThe EDELWEISS DM search Phase II to Phase III
The EDELWEISS DM search Phase II to Phase III Adam Cox Karlsruhe Institute for Technology (KIT) on behalf of the EDELWEISS Collaboration CEA, Saclay (IRFU and IRAMIS) IPNL (CNRS/IN2P3 and Université de
More informationDARK MATTER SEARCH AT BOULBY MINE
DARK MATTER SEARCH AT BOULBY MINE R. LUSCHER on behalf of the Boulby Dark Matter Collaboration (RAL, Imperial College, Sheffield, UCLA, Texas A&M, Pisa, ITEP, Coimbra, Temple and Occidental) Rutherford
More informationChapter 12. Dark Matter
Karl-Heinz Kampert Univ. Wuppertal 128 Chapter 12 Dark Matter Karl-Heinz Kampert Univ. Wuppertal Baryonic Dark Matter Brightness & Rotation Curve of NGC3198 Brightness Rotation Curve measured expected
More informationThe XENON100 Dark Matter Experiment at LNGS: Status and Sensitivity
The XENON100 Dark Matter Experiment at LNGS: Status and Sensitivity Elena Aprile (on behalf of the XENON Collaboration) Columbia University,Physics Department, New York,NY, USA E-mail: age@astro.columbia.edu
More informationSearches for Low-Mass WIMPs with CDMS II and SuperCDMS
Searches for Low-Mass WIMPs with CDMS II and SuperCDMS SuperCDMS Science Coordinator Syracuse University arxiv: 1304.4279 1304.3706 1203.1309 A New Order 0.01% Visible H, He 0.5% ENERGY Metals Dark Matter
More informationTwo Neutrino Double Beta (2νββ) Decays into Excited States
Two Neutrino Double Beta (2νββ) Decays into Excited States International School of Subnuclear Physics 54 th Course: The new physics frontiers in the LHC-2 era Erice, 17/06/2016 Björn Lehnert TU-Dresden,
More informationDirect Dark Matter and Axion Detection with CUORE
Direct Dark Matter and Axion Detection with CUORE Marco Vignati University of Rome La Sapienza & INFN Rome on behalf of the CUORE collaboration Panic 11, July 5, MIT 988 TeO crystals Ton scale bolometric
More informationLOW ENERGY SOLAR NEUTRINOS WITH BOREXINO. Lea Di Noto on behalf of the Borexino collaboration
LOW ENERGY SOLAR NEUTRINOS WITH BOREXINO Lea Di Noto on behalf of the Borexino collaboration Vulcano Workshop 20 th -26 th May 2018 [cm -2 s -1 MeV -1 ] SOLAR NEUTRINOS Electrons neutrinos are produced
More informationDirect Detection of Dark Matter. Lauren Hsu Fermilab Center for Particle Astrophysics TRISEP Summer School, June 10, 2014
Direct Detection of Dark Matter Lauren Hsu Fermilab Center for Particle Astrophysics TRISEP Summer School, June 10, 2014 Direct Detection of Dark Matter Lecture 1 How to detect dark matter Lecture 2 Review
More informationDark Matter and the XENON Experiment
Dark Matter and the XENON Experiment Marc Schumann Physik Institut, Universität Zürich Lunch Seminar, Weizmann Institute of Science, November 4th, 2010 www.physik.uzh.ch/groups/groupbaudis/xenon/ 2 3 95%
More informationDark Matter - III. Workshop Freudenstadt September 30, GRK 1694: Elementarteilchenphysik bei höchster Energie und höchster Präzision
Dark Matter - III GRK 1694: Elementarteilchenphysik bei höchster Energie und höchster Präzision Workshop Freudenstadt 2015 September 30, 2015 Guido Drexlin, Institut für Experimentelle Kernphysik KIT University
More informationOverview of Direct Detection Dark Matter Experiments
Overview of Direct Detection Dark Matter Experiments Southern Methodist University Dallas, TX, USA E-mail: cooley@physics.smu.edu The past year has yielded several new results from the direct detection
More informationDARK MATTER SEARCHES AT CANFRANC: ANAIS AND ROSEBUD: an update INTRODUCTION AND EXPERIMENTAL GOALS SUMMARY OF RECENT ACHIEVEMENTS AND EFFORTS
DARK MATTER SEARCHES AT CANFRANC: ANAIS AND ROSEBUD: an update María Luisa Sarsa (Universidad de Zaragoza) On behalf of ANAIS & ROSEBUD Collaborations OUTLINE ANAIS INTRODUCTION AND EXPERIMENTAL GOALS
More informationXENON100. Marc Schumann. Physik Institut, Universität Zürich. IDM 2010, Montpellier, July 26 th,
XENON100 Marc Schumann Physik Institut, Universität Zürich IDM 2010, Montpellier, July 26 th, 2010 www.physik.uzh.ch/groups/groupbaudis/xenon/ Why WIMP search with Xenon? efficient, fast scintillator (178nm)
More informationTHE CRYOGENIC UNDERGROUND OBSERVATORY FOR RARE EVENTS: STATUS AND PROSPECTS
THE CRYOGENIC UNDERGROUND OBSERVATORY FOR RARE EVENTS: STATUS AND PROSPECTS Eric B. Norman Dept. of Nuclear Engineering Univ. of California, Berkeley, CA U. S. A. Recent results in n physics Neutrinos
More informationLuca Grandi.
Luca Grandi http://warp.pv.infn.it idm2004 - September 2004 Wimp Argon Programme Collaboration R. Brunetti, E. Calligarich, M. Cambiaghi, C. De Vecchi, R. Dolfini, L. Grandi, A. Menegolli, C. Montanari,
More informationThe XENON1T experiment
The XENON1T experiment Ranny Budnik Weizmann Institute of Science For the XENON collaboration 1 The XENON1T experiment Direct detection with xenon The XENON project XENON1T/nT 2 Quick introduction and
More informationDetectors for astroparticle physics
Detectors for astroparticle physics Teresa Marrodán Undagoitia marrodan@physik.uzh.ch Universität Zürich Kern und Teilchenphysik II, Zürich 07.05.2010 Teresa Marrodán Undagoitia (UZH) Detectors for astroparticle
More informationDark Matter Search with XENON
Dark Matter Search with XENON Marc Schumann Physik Institut, Universität Zürich Universität Mainz, Seminar, May 2, 2012 www.physik.uzh.ch/groups/groupbaudis/xenon/ 2 Baryonic Matter Dark Matter? Dark Energy????
More informationThe DarkSide-50 Outer Detectors
The DarkSide-50 Outer Detectors Shawn Westerdale Princeton University (for the DarkSide Collaboration) TAUP 2015 Torino Thursday, Sept 10, 2015 The DarkSide-50 Experiment Located in Hall C of Laboratori
More informationStatus of the ANAIS experiment at Canfranc
Status of the ANAIS experiment at Canfranc J. Amaré, B. Beltrán, J. M. Carmona, S. Cebrián, E. García, H. Gómez, G. Luzón,, J. Morales, A. Ortiz de Solórzano, C. Pobes, J. Puimedón, A. Rodriguez, J. Ruz,
More informationNo combined analysis of all experiments available
Compatibility between DAMA-CDMS CDMS-Edelweiss-Xenon10 - KIMS? No combined analysis of all experiments available However, some trivial considerations: * for m χ 25 GeV capture on DAMA is dominated by the
More informationXMASS: a large single-phase liquid-xenon detector
XMASS: a large single-phase liquid-xenon detector Katsuki Hiraide, the university of Tokyo for the XMASS Collaboration October 3 rd, 2016 IPRD16@Siena, Italy 1 XMASS project XMASS: a multi purpose experiment
More informationDirect and Indirect Searches for WIMP Dark Matter
Direct and Indirect Searches for WIMP Dark Matter Neil Spooner 1 Department of Physics and Astronomy University of Sheffield, Hounsfield Road, Sheffield, S3 7RH, UK I briefly review the present status
More informationThe relevance of XENON10 constraints in this low-mass region has been questioned [15] C.E. Aalseth et al. arxiv: v1
The relevance of XENON10 constraints in this low-mass region has been questioned [15] C.E. Aalseth et al. arxiv:1001.2834v1 Peter Sorensen LLNL on behalf of the XENON10 Collaboration at UC Davis HEFTI
More informationExperiments for double beta decay and dark matter
Experiments for double beta decay and dark matter Ettore Fiorini, NDM2006, Paris September 4, 2006 Je ne loue ni blâme pas, je report seulement (Talleyrand) I am not praising, nor blaming; I anly report
More informationDark matter search with the SABRE experiment
Dark matter search with the SABRE experiment Giulia D Imperio* for the SABRE collaboration *INFN Roma 1 25-07-2017 TAUP 2017 Sudbury, Canada 1 Dark matter detection through annual modulation WIMP is one
More informationEdelweiss-II : status and first results A new generation of background-free bolometers for WIMP search
Edelweiss-II : status and first results A new generation of background-free bolometers for WIMP search From EDWI to EDW II New ID detectors Some current results Outlook G. Gerbier CEA Saclay, IRFU, France
More information