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Results from the XENON100 Dark Matter Search Experiment

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Results from the XENON100 Dark Matter Search Experiment Results from the XENON100 Dark Matter Search Experiment Dr. Chamkaur Ghag University College London 31st October 2012 1. Very Brief Intro to Dark Matter and Direct Detection 2. The LXeTPC & XENON100 3. Latest Results 4. The Next Generation 1. Very Brief Intro to Dark Matter and Direct Detection 2. The LXeTPC & XENON100 3. Latest Results 4. The Next Generation Early evidence for Dark Matter 1930’s - Fritz Zwicky 1970’s - Vera Ruben Measured rotational velocity of galaxies and observed flat curves rather than expected Keplerian fall-off with distance from galactic centre GALAXIES ARE ROTATING TOO FAST! Andromeda Lots more evidence since then - with little against... -2 Temper + We have a ‘Missing Mass’ Problem! 85% of the mass of the Universe is DARK! -2 Temper + Dark Matter Detection Favoured candidates are Weakly Interacting Massive Particles (WIMPs) •Indirect - observe annihilation products •Accelerator - produce WIMPs •Direct - interact with galactic WIMPs (our Dark Matter!) in ultra-low background terrestrial detectors Direct detection is internationally recognised as one of THE highest priorities in science! High Priority on just about all Roadmaps and Advisory Documents A Growing Field WIMP Detection Techniques Heat and ionisation bolometers: Bubbles and Droplets: CDMS CUOPP EDELWEISS PICASSO Light and heat Bolometers: CRESST ROSEBUD Phonons dE/dx Charge Light Scintillators: Scintillation and ionisation charge detectors: DAMA XENON LIBRA DarkSide XMASS ZEPLIN CLEAN LUX DEAP ANAIS Ionisation detectors: KIMS DRIFT, DMTPC, GENIUS, NEWAGE, HDMS, IGEX 1. Very Brief Intro to Dark Matter and Direct Detection 2. The LXeTPC & XENON100 3. Latest Results 4. The Next Generation Liquid Xenon Time Projec1on Chambers • S1: LXe is an excellent scinllator – Density: 3 g/cm3 – Light yield: >60 ph/keV (0 field) – Scin=llaon light: 178 nm (VUV) – Nuclear recoil threshold ∼5-8 keV • S2: Even beFer ionisaon detector (evt/kg/keV/day) Rate – S1+S2 allows mm vertex reconstruc=on – Sensi=ve to single ionisaon electrons Recoil Energy (keV) – Nuclear recoil threshold ∼1 keV • And a great WIMP target too – Scalar WIMP-nucleon scaering rate dR/dE∼A2 – Odd-neutron isotopes (129Xe, 131Xe) enable spin-dependent sensi=vity – Excellent ionisaon threshold: ‘light WIMP’ searches using S2 only – No intrinsic backgrounds (85Kr can be removed, low rate from 136Xe 2νββ) – Easily scaled with no loss of performance (actually improves!) Photomultiplier Tube Anode Grid Gas Xe Liquid Xe E Cathode Grid S1 e- - - e- e ee-e- e- e- e- top hit pattern: x-y localization - - e e- -e e- - e- ee-ee- S2 Δt : z localization t x Δ 3 Nov 2008 19 Particle Discrimination Light (S1) and charge (S2) depend on recoil dE/dx 30 cm 1. Very Brief Intro to Dark Matter and Direct Detection 2. The LXeTPC & XENON100 3. Latest Results 4. The Next Generation Intrinsic backgrounds LXeTPCs easily identify surface backgrounds, alphas and delayed coincidences with 3D vertex and energy reconstruction And the result..... (Further) Exploiting the Ionisation Channel • Resolution of primary scintillation is dominated by photon generation and photoelectron collection statistics • Single electron detection demonstrated in LXe TPCs • In ZEPLIN-III, single electrons detected within 36 µs timeline and with dedicated runs • Origin: ✤ Photon-induced (post S1): photoionisation and emission from cathode ✤ Spontaneous emission: background related • Application: Electron lifetime measurement (extremely useful for ton and greater 14 7 ★ y 60 scale detectors) 12 6 40 count 10 5 20 8 4 ★Lower thresholds (~1 keV) and superior resolution 0 6 3 -20 4 2 ★Low mass WIMP searches -40 2 1 -60 0 0 -60 -40 -20 0 20 40 60 0 10 20 30 40 50 60 70 80 90 ★Neutrino physics x r WIMPs AXIONS CNNS Journal of High Energy Physics 12 (2011)115 Energyof High Physics Journal http://arxiv.org/pdf/1209.3810.pdf 1. Very Brief Intro to Dark Matter and Direct Detection 2. The LXeTPC & XENON100 3. Latest Results 4. The Next Generation The Next Step: XENON1T High transparency electrodes No top array screening mesh Active LXe veto Three interlocking PTFE panels LXe (2.2 Ton) Titanium cryostat 1 kV/cm drift field and vacuum jacket with external field shaping rings 2 arrays of 121 high No charge QE 3” photodetectors insensitive regions below photocathode Scaleability has been demonstrated repeatedly - gets easier (no performance loss) as we get bigger! 10-39 DAMA/Na ] -40 2 10 CoGeNT DAMA/I CDMS (2011) 10-41 CDMS (2010) -42 10 CRESST (2011) ZEPLIN-III XENON100 (2010) 10-43 EDELWEISS (2011) 10-44 XENON100 (2011) Trotta et al. 10-45 XENON100 (2012) Buchmueller 10-46 et al. WIMP-Nucleon Cross Section [cm Section Cross WIMP-Nucleon XENON1T (2017) 10-47 6 7 8 910 20 30 40 50 60 100 200 300 400 1000 WIMP Mass [GeV/c2] 1 Tonne Fiducial Mass 2 Year Exposure (~2017) Homestake mine South Dakota U L Davis Cavern (5th May 2011) 4850 ft depth World leader in 2013 Sept 5th 2012 Dec 2011 Water Shield and lab ready for LUX! H. Araujo, 59 The ZEPLIN Programme at Boulby ZEPLIN I ZEPLIN II ZEPLIN III Single phase, 3 PMTs, 5/3.1 kg Double phase, 7 PMTs, Double phase, 31 PMTs, Run 2001-04 moderate E field, 31/7.2 kg high E field, 10/6.4 kg Limit: 1.1*10-6 pb Run 2005-06 Run 2009-11 Limit: 6.6*10-7 pb Limit: 3.9*10-8 pb Single-phase The first 2-phase LXe Dark Matter Europe’s most sensitive SI detector! World’s best WIMP-neutron SD ZEPLIN-III LUX350 LZ LUX-ZEPLIN (LZ) Next-generaon LXe experiment 6 kg LXe (fid) 100 kg 5,000 kg building on LUX and ZEPLIN Programmes • Route to detec1on & study: a progressive programme – UK-led ZEPLIN programme pioneered liquid xenon for WIMP searches – LUX (now with UK) about to turn on – expect leading sensi=vity in 2013 – LZ could discover at 10-11 pb or exclude at 10-12 pb with 3 year run • Experimental approach: a low risk and aggressive programme – Background free strategy (self-shielding, modest discriminaon assumed) – Two-phase Xe technology: high readiness level (ZEPLIN, XENON, LUX) – Teams with huge track record in DM searches – Much infrastructure inherited from LUX350 • LXe Provides exci1ng Physics for light & heavy WIMPs (GeV-TeV) – Since we do not yet know what BSM physics looks like! H. Araujo, 62 SANFORD LAB, DAVIS COMPLEX (4850-_) LZ INFRASTRUCTURE 7 tonne LXe TPC to fit LUX water tank Modest increase in linear scale factor from LUX (low risk) But huge increase in sensivity LZ LUX350 120 cm 49 cm H. Araujo, 63 Elasc scaering SI cross-sec1on Results ZEPLIN-III 2011 (magenta) XENON100 2011 (green) XENON100 2012 (grey) EDELWEISS II 2011 (dark blue) CDMS-II 2010 (blue) Projecons LUX (red dash) 100 kg fiducial x 300 live days LUX-ZEPLIN (black dash) 5-tonne fiducial x 1,000 live days LZ Collaboraon (UK/ZEPLIN) • ImPerial College London (ZEPLIN-III, LUX, LZ) – H. Araujo (A), T. Sumner (A), A. Currie (PDRA) • Rutherford ApPleton Laboratory (ZEPLIN-III, LZ) – P. Majewski • Edinburgh University (ZEPLIN-III, LUX, LZ) – A. Murphy (A), J. Dobson (PDRA), L. Reichhart (PG) • University College London (LUX, LZ) – C. Ghag (A), J. Dobson (PDRA) • Daresbury Laboratory (LZ) – J. Simpson (A) • LIP-Coimbra (ZEPLIN-III, LUX, LZ) – M.I. Lopes (A), J. Pinto da Cunha (A), V. Solovov (RF), L. de Viveiros (RA), A. Lindote (RA), F. Neves (RA), C. Silva (RA) • ITEP-Moscow (ZEPLIN-III, RED-100, LZ) – D. Akimov (A), V. Belov, A. Burenkov, A. Kobyakin, A. Kovalenko, V. Stekhanov H. Araujo, 65 Exciting times ahead.... Thank you all for listening!.
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