LUX: A Large Underground Xenon detector WIMP Search

Slides:



Advertisements
Similar presentations
1 Aaron Manalaysay Physik-Institut der Universität Zürich CHIPP 2008 Workshop on Detector R&D June 12, 2008 R&D of Liquid Xenon TPCs for Dark Matter Searches.
Advertisements

NEST: Noble Element Simulation Technique Modeling the Underlying Physics of Noble Liquids, Gases Matthew Szydagis, UC Davis UCLA DM 02/28/14 1
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:
KIT – Universität des Landes Baden-Württemberg und nationales Forschungszentrum in der Helmholtz-Gemeinschaft Benjamin Schmidt, IEKP, KIT Campus North,
Dark Matter Searches with Dual-Phase Noble Liquid Detectors Imperial HEP 1st Year Talks ‒ Evidence and Motivation ‒ Dual-phase Noble Liquid Detectors ‒
Report from Low Background Experiments Geant4 Collaboration Workshop 10 September 2012 Dennis Wright (SLAC)
Future of DM Detection Mark Boulay, Los Alamos Mark Boulay CLEAN: A Detector for Dark Matter and Low-Energy Solar ’s Liquid neon as a target for dark matter.
Introduction to Hadronic Final State Reconstruction in Collider Experiments Introduction to Hadronic Final State Reconstruction in Collider Experiments.
The XENON Project A 1 tonne Liquid Xenon experiment for a sensitive Dark Matter Search Elena Aprile Columbia University.
J.T. White, TAMUPPC07 May 16, 2007 SIGN: Potential WIMP Detection using Pressurized Nobles J.T. White Texas A&M University 5/16/07.
PANDAX Results and Outlook
Proportional Light in a Dual Phase Xenon Chamber
Gaitskell XENON Experiment - SAGENAP Factors Affecting Detector Performance Goals and Alternative Photo-detectors Rick Gaitskell Department of Physics.
What’s the Matter in the Universe? Richard Schnee Syracuse University Quarknet Lecture July 13, 2012 The Search for Dark Matter.
ZEPLIN II Status & ZEPLIN IV Muzaffer Atac David Cline Youngho Seo Franco Sergiampietri Hanguo Wang ULCA ZonEd Proportional scintillation in LIquid Noble.
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.
J.T. White Texas A&M University SIGN (Scintillation and Ionization in Gaseous Neon) A High-Pressure, Room-Temperature, Gaseous-Neon- Based Underground.
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.
Dark Matter Detection with Liquid Xenon Masahiro Morii Harvard University Laboratory for Particle Physics and Cosmology 21 August
APS April meeting Jacksonville, 2007 WIMP Search With SNOLAB Chris Jillings SNOLAB Staff Scientist For the DEAP-1 Collaboration.
From CDMSII to SuperCDMS Nader Mirabolfathi UC Berkeley INPAC meeting, May 2007, Berkeley (Marina) CDMSII : Current Status CDMSII Perspective Motivation.
Dark Matter Search with SuperCDMS Results, Status and Future Wolfgang Rau Queen’s University.
SuperCDMS From Soudan to SNOLAB Wolfgang Rau Queen’s University.
J.T. White Texas A&M University SIGN (Scintillation and Ionization in Gaseous Neon) A High-Pressure, Room- Temperature, Gaseous-Neon-Based Underground.
A Study of Background Particles for the Implementation of a Neutron Veto into SuperCDMS Johanna-Laina Fischer 1, Dr. Lauren Hsu 2 1 Physics and Space Sciences.
F August S. Pordes - Fermilab1 Liquid Argon for Direct Detection of Dark Matter Work and Plans at Fermilab.
DarkSide: a Free Background Experiment Maria Bossa LNGS Seminar IPRD13 Oct 10, 2013.
Bei Cai and Mark Boulay For the DEAP-1 Collaboration Queen’s University, Canada Pulse Shape Discrimination (PSD) in Liquid Argon from DEAP-1 APS meeting,
Dan Bauer - CDMS Project ManagerAll experimenters meeting - April 23, 2007 Cryogenic Dark Matter Search (CDMS) Progress at Soudan since last summer Successful.
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)
? At Yangyang beach, looking for something in the swamp of particles and waves. 1 The recent results from KIMS Seung Cheon Kim (Seoul National University)
1/27/2016Katsushi Arisaka 1 University of California, Los Angeles Department of Physics and Astronomy Katsushi Arisaka XAX 10.
DARK MATTER SEARCH Carter Hall, University of Maryland.
I. Giomataris, CEA-Irfu-France
ZEPLIN III Position Sensitivity PSD7, 12 th to 17 th September 2005, Liverpool, UK Alexandre Lindote LIP - Coimbra, Portugal On behalf of the ZEPLIN/UKDM.
Second Workshop on large TPC for low energy rare event detection, Paris, December 21 st, 2004.
Detecting the Directionality of Dark Matter via “Columnar Recombination” (CR) Technique An attractive, natural candidate for Dark Matter is the WIMP –
SuperCDMS From Soudan to SNOLAB Wolfgang Rau Queen’s University 1W. Rau – IPA 2014.
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.
Low Mass WIMP Search with the CDMS Low Ionization Threshold Experiment Wolfgang Rau Queen’s University Kingston.
Scintillating Bubble Chambers for Direct Dark Matter Detection Jeremy Mock On behalf of the UAlbany and Northwestern Groups 1.
18-20 May 2015, Underground Science Conference, SDSM&T 1John Harton, Colorado State University Recent Results from the DRIFT Directional DM Experiment.
5/13/11 FCPA Mini-RetreatDarkSide - S.Pordes1 DarkSide 10 kg Prototype at Princeton Distillation Column for Depleted Argon at Fermilab DarkSide 50 at Gran.
Alex Howard, Imperial College Slide 1 July 2 nd 2001 Underground Project UNDERGROUND PROJECT – Overview and Goals Alex Howard Imperial College, London.
WIMPs Direct Search with Dual Light-emitting Crystals Xilei Sun IHEP International Symposium on Neutrino Physics and Beyond
1 Aaron Manalaysay Physik-Institut der Universität Zürich 2009 UniZH/ETH Doktorandenseminar June 5, 2009 Rubidium 83: A low-energy, spatially uniform calibrator.
From Edelweiss I to Edelweiss II
Dark Matter Direct Detection roadmap strategy
PandaX DM Search Exp Xiangdong Ji (季向东)
UK Dark Matter Collaboration
University of South Dakota
SuperCDMS at SNOLAB Wolfgang Rau Queen’s University for the
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
Neutron Detection with MoNA LISA
杨勇 上海交通大学 On Behalf of the Collaboration 粒子物理数据分析基础和前沿研讨会,2016/9/13
Dark Matter Search with Stilbene Scintillator
XMASS Y. Suzuki (for the XMASS Collaboration) Kamioka Observatory,
LUX: Shedding Light on Dark Matter
Detecting WIMPs using Au-DNA Microarrays
The Estimated Limits For A 5g LE-Ge Detector
Presentation transcript:

LUX: A Large Underground Xenon detector WIMP Search Mani Tripathi INPAC Meeting Berkeley, May 5, 2007 May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting New Collaboration Groups formerly in XENON10: Case Western, Brown, Livermore Natl. Lab (major fraction of the US contingent in XENON10) Groups from ZEPLIN II: UCLA, Texas A&M, Rochester (entire US contingent in ZEPLIN-II) New Entrants: UCDavis, LBNL (background in neutrinos/nuclear/HEP) INPAC is a large fraction of this effort. May 5, 2007 Mani Tripathi, INPAC Meeting

Direct Detection Techniques CRESST I CDMS EDELWEISS CRESST II ROSEBUD ZEPLIN II, III XENON LUX WARP ArDM SIGN NAIAD ZEPLIN I DAMA XMASS DEAP Mini-CLEAN DRIFT IGEX COUPP Scintillation Heat -Phonons Ionization Ge, Si Al2O3, LiF CaWO4, BGO ZnWO4, Al2O3 … Xe, Ar, Ne Ge, CS2, C3F8 ~100% of Energy ~20% of Energy Few % of Energy Fig. courtesy H. Sobel NaI, Xe, Ar, Ne May 5, 2007 Mani Tripathi, INPAC Meeting

Noble Liquids as Target WIMP flux on earth: v ~ c/1000, mc ~ 100 mproton flux ~ 105 /(cm2 s) Rate for E> Erecoil (events/Kg/day) Scatter on nuclei: For Xe, useful range is 5Kev<Recoil Energy <50 KeV Scatter coherently from whole nucleus: Erecoil (µ = reduced mass) May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting Liquid Xenon has come out with results in 2007 ZEPLIN-II Jan 2007 s < 6.6 x 10-43 cm2 @ m= 65 GeV May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting Dramatic Improvement in DM Sensitivity CDMS 2004+05 XENON10 April 2007 10 kg fiducial dual phase xenon detector with only 60 days data May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting Two Signal Technique PMT Array (not all tubes shown) Time Gas phase Anode e- EAG Secondary Liq. Surface e- Grid ~1 µs width 0–150 µs depending on depth e- Electron Drift ~2 mm/µs EGC Primary ~40 ns width Liquid phase Cathode Light Signal UV ~175 nm photons EAG > EGC Interaction (WIMP or Electron) May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting Xenon Facts Ionization signal 90% 10% Ionization in liquid: About one electron-ion pair /15 eV of deposited energy 175 nm Scintillation: About one photon/20 eV of deposited energy Ionization/Scintillation ratio changes with interaction type Ion pairs more likely to recombine in the dense tracks generated by nuclear interactions A strong anti-correlation between ionization and scintillation Scintillation signal May 5, 2007 Mani Tripathi, INPAC Meeting

Ionization/Scintillation Response WIMP or Neutron nuclear recoil electron Gamma or Electron Nuclear recoil: Electrons recombine in the liquid due to higher ionization density - fewer primary electrons Also overall quenching of scintillation relative to electron recoil Gamma recoil: Less recombination in the liquid due to lower ionization density more primary electrons May 5, 2007 Mani Tripathi, INPAC Meeting

Realization of Two Signal Technique Example from XENON10: Plot Log (S2/S1) versus total recoli energy. Electromagnetic recoils Neutron recoils: WIMPs would appear here May 5, 2007 Mani Tripathi, INPAC Meeting

The LUX detector and shield 100 kg ~ 6m diameter Water Cerenkov shield (low cost) Tall dual phase detector Aspect ratio = 1.5 May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting LUX Parameters 300 kg Dual Phase liquid Xe TPC with 100 kg fiducial >99% ER background rejection for 50% NR acceptance, E>10 keVr 3D-imaging TPC eliminates surface activity, defines fiducial Backgrounds: Internal: strong self-shielding of PMT activity / < 7x10-4 /keVee/kg/day, from PMTs (Hamamatsu R8778 or R8520). Neutrons (,n) & fission subdominant External: large water shield with muon veto. Very effective for cavern +n, and HE n from muons Very low gamma backgrouns with readily achievable <10-11 g/g purity. DM reach: 2x10-45 cm2 in 4 months Possible ~5x10-46 cm2 reach with recent PMT activity reductions, longer running. May 5, 2007 Mani Tripathi, INPAC Meeting

Active Water Shield and Veto Veto on incoming muons via Cherenkov light signal. Tag thermalized neutrons generated within the detector Gd (0.2%) in water gives a capture efficiency of > 90% for thermal neutrons, followed by an 8 MeV gamma cascade Xe recoil  ~ 8 MeV Gd t ~ 50 ms n captures on Gd Incident n Xe detector Water shield Studies for SuperK have shown compatibility with standard detector materials (Bob Svoboda et al) May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting LUX Dark Matter Goal ZEPLIN II CDMS II WARP LUX (Proj) SuperCDMS@Soudan LUX - Sensitivity curve at 2x10-45 cm2 (100 GeV) Exposure: Gross Xe Mass 300 kg Limit set with 120 days running x 100 kg fiducial mass x 50% NR acceptance ~1 background event during exposure assuming most conservative assumptions of ER 7x10-4 /keVee/kg/day and 99% ER rejection ER bg assumed is dominated by guaranteed Hamamatsu PMT background. Improvements in PMT bg (and rejection power) will extend background free running period, and DM sensitivity Edelweiss I SuperCDMS@SNOLab Comparison -- SuperCDMS Goal @ SNOLab: Gross Ge Mass 25 kg (x 50% fid mass+cut acceptance) Limit set for 1000 days running x 7 SuperTowers May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting Status Proposal Under review by NSF/DoE. Meanwhile, LUXCore The collaboration is fully active – Technical VideoCons every Week … Construction activity in full swing at all institutions using Univ resources, startup seed funds etc. Construction finished late Summer 07 -- operations at Case: Fall 2007. May 5, 2007 Mani Tripathi, INPAC Meeting

LUX program: exploit scalability LUX detector LUXcore LUX program: exploit scalability LUXcore: Final engineering for large-scale detector Cryostat, >100 kV feedthrough, charge drift, light collection over large distance Full system integration, including ~1m water shield 40 kg narrow “core”, 14 PMTs, 20 cm Ø x 40 cm tall. Radial scale-up requires full-funding. Very good match to early-implementaion DUSEL SNOLAB LOI System scalable to very large mass. May 5, 2007 Mani Tripathi, INPAC Meeting

Mani Tripathi, INPAC Meeting Cryostat Being Installed At Case. May 5, 2007 Mani Tripathi, INPAC Meeting