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Dark Matter Direct Detection: Experiment, Prospects for WIMPs and Beyond… Jocelyn Monroe, Royal Holloway University of London XLV International Meeting on Fundamental Physics University of Granada, Spain April 27, 2017 Outline Experimental Considerations in Direct Detection Searches Status and Prospects of Experiments Beyond WIMP Dark Matter in Direct Detection Experiments Jocelyn Monroe April 27, 2017 / p. 2 Dark Matter Direct Detection Signal:χN ➙χN χ χ Backgrounds: γ e- ➙ γ e- n N ➙ n N N ➙ N’ + α, e- ν N ➙ ν N detector requirements: particle ID for recoil N, e-, alpha, n (multiple)γ final states γ Jocelyn Monroe April 27, 2017 / p. 3 1 E = m v2 WIMP Scattering χ D 2 D χ kinematics: v/c ~ 8E-4! q2 = 2m E recoil angle strongly correlated T recoil 4mDmT with incoming WIMP direction r = 2 (mD + mT ) N N (1 cosq) E = E r − recoil D 2 Spin Independent: χscatters coherently off of the entire nucleus A: σ~A2 D. Z. Freedman, PRD 9, 1389 (1974) Spin Dependent: mainly unpaired nucleons contribute to scattering amplitude: σ~ J(J+1) detector requirements: measure recoil energy, time, +angle Jocelyn Monroe April 27, 2017 / p. 4 100 GeV/c2 WIMP mass Observable: Recoil Energy 1E-45 cm2 WIMP-nucleon SI σ χ 10 Scintillation χ Heat 1 Ionization 0.1 ~ detector requirements: ~1-10s of keV energy threshold, very low backgrounds Jocelyn Monroe April 27, 2017 / p. 5 Detection Signature PICO Cogent COUPP Picasso Newage ArDM DRIFT Xenon100 Ionization! CDMS DarcSide EDELWEISS LUX CoGeNT Panda-X DMTPC Heat! ANaIS Scintillation! XMASS DEAP/CLEAN CRESST KIMS CRESSTII Dama/LIBRA ROSEBUD existing detectors: many targets (Xe, Ge, Ar, NaI, CsI, CaWO4, CF3I, C3F8, F ...) Jocelyn Monroe April 27, 2017 / p. 6 Around the World Kamioka: XMASS, NEWAGE SNOLAB: CJPL: PANDA-X, CDEX DEAP, PICO, DAMIC Y2L: KIMS SuperCDMS DMTPC NEWS Boulby: DRIFT DM-ICE SURF: LUX Gran Sasso: LZ DAMA/LIBRA CRESST DarkSide Soudan: XENON CDMS COGENT Modane (LSM): EDELWEISS S. Pole: MiMAC DM-ICE CanFranc: ArDM, ANAIS Jocelyn Monroe April 27, 2017 / p. 7 Backgrounds ? N Gamma ray interactions: electron recoil final states rate ~ Ne x (gamma flux), O(1E7) events/(kg day) mis-identified electrons mimic nuclear recoils Contamination: 238U and 232Th decays, recoiling progeny and mis-identified alphas, betas mimic nuclear recoils Neutrons: Nuclear recoil final state. (alpha,n), U, Th fission, cosmogenic spallation μ μ γ N* N n D. Malling, UCLA DM’16 + discrimination between e- vs. N Jocelyn Monroe April 27, 2017 / p. 8 Backgrounds ? N Gamma ray interactions: electron recoil final states rate ~ Ne x (gamma flux), O(1E7) events/(kg day) mis-identified electrons mimic nuclear recoils Contamination: 238U and 232Th decays, recoiling progeny and D.-M. Mei, A. Hime, PRD73:053004 (2006) mis-identified alphas, betas mimic nuclear recoils Neutrons: Nuclear recoil final state. (alpha,n), U, Th fission, cosmogenic spallation μ μ γ N* N n + discrimination between e- vs. N Jocelyn Monroe + large, active neutron shielding April 27, 2017 / p. 9 Irreducible Backgrounds impossible to shield a detector from coherent neutrino scattering! Φ(solar B8) = 5.86 x 106 cm-2 s-1 ν ν JM, P. Fisher, PRD76:033007 (2007) Z N N nuclear recoil final state neutrino bound at 10-46-10-48 cm2 in zero-background paradigm unless you measure the direction! Jocelyn Monroe April 27, 2017 / p. 10 Irreducible Backgrounds impossible to shield a detector from coherent neutrino scattering! Φ(solar B8) = 5.86 x 106 cm-2 s-1 ν ν neutrino backgrounds from 8B becoming important in current experiments! Z XENON 1T example: N N Aprile et al., JCAP04 (2016) 027 nuclear recoil final state neutrino bound at 10-46-10-48 cm2 in zero-background paradigm unless you measure the direction! Jocelyn Monroe April 27, 2017 / p. 9 Modulation Signatures Annual event rate modulation: June-December asymmetry ~2-10%. Drukier, Freese, Spergel, Phys. Rev. D33:3495 (1986) Sidereal direction modulation: asymmetry ~ 20-100% in forward-backward event rate. Spergel, Phys. Rev. D36:1353 (1988) detector requirements: achieve + measure stability vs. time to a very high level! Jocelyn Monroe April 27, 2017 / p. 12 Outline Experimental Considerations in Direct Detection Searches Status and Prospects of Experiments Beyond WIMP Dark Matter in Direct Detection Experiments Jocelyn Monroe April 27, 2017 / p. 13 Model Space Wide range of parameters! Direct detection searches generally optimised for WIMP sensitivity... Baer et al., arXiv:1407.0017 Jocelyn Monroe April 27, 2017 / p. 14 CRESST II (2015) SuperCDMS (2014) Model Space PICO50 CRESST III excluded* at 90% confidence level Wide range of parameters! DAMA SuperCDMS @SNOLAB CRESST (2012) DEAP-3600 Direct detection searches generally optimised for WIMP sensitivity... LUX (2016) coherent neutrino scattering PandaX (2016) SuperCDMS @SNOLAB LZ Xenon 1T LZ DarkSide 20k coherent neutrino scattering Baer et al., arXiv:1407.0017 Jocelyn Monroe April 27, 2017 / p. 14 Model Space Wide range of parameters! Direct detection searches generally optimised for WIMP sensitivity... but starting to look for axions/ALPs too! axion model space dark matter = axions Baer et al., arXiv:1407.0017 Jocelyn Monroe April 27, 2017 / p. 13 The Low-Background Frontier: Prospects 1 event/ Low Mass, Large σ kg/day 1 event/ kg/year Canonical MSSM Mass, σ > Neutrino Bound 1 event/ kg/century High Mass, Tiny σ or Large # Events so far: ~3 years / order of magnitude Jocelyn Monroe April 27, 2017 / p. 15 The Low-Background Frontier: Prospects 1 event/ kg/day 1 event/ kg/year 1 event/ kg/century so far: ~3 years / order of magnitude Jocelyn Monroe April 27, 2017 / p. 15 Key Experimental Consideration: Quenching (material courtesy L. Baudis) Current status of measurements of visible/recoil energy in -ionization on Ge -scintillation on Xe, Ar Impact of uncertainties up to x5-10 in dark matter limits, particularly at low mass! measurement in the experiment energy region of interest required Jocelyn Monroe April 27, 2017 / p. 16 Key Experimental Consideration: Quenching (material courtesy L. Baudis) Current status of measurements of visible/recoil energy in -ionization on Ge -scintillation on Xe, Ar Impact of uncertainties up to x5-10 in dark matter limits, particularly at low mass! measurement in the experiment energy region of interest required Jocelyn Monroe April 27, 2017 / p. 16 Low Mass, Bolometers Large σ phonon, ionisation or scintillation readout of crystals at O(10 mK), using Ge, Si, CaWO4 Phonon rails: 1400 gm (SuperCDMS) or 800 gm (EDELWEISS) Ge, TES for Erecoil & R (timing) h+ EDELWEISS: interleaved electrodes reduce e- reduce surface backgrounds by x105 Charge electrodes: biased at +/- 2V, measure Erecoil, configuration optimised to reject surface events Scintillation side: Si absorber on 300 gm CaWO4, tungsten TES readout for particle ID Ionization/Phonon yield Phonon side: TES readout to measure Erecoill Jocelyn Monroe E recoil (keV) April 27, 2017 / p. 17 Low Mass, EDELWEISS (thanks to J. Gascon) Large σ EDELWEISS! • Largest operating cryogenic Ge array (20 kg) for Direct DM search" • Latest results: arXiv:1603.05120" • 2017 goal @ LSM: optimizing sensitivity to 1-10 GeV WIMPs" • Beyond: completing the exploration of the low-WIMP CRESST 2012! mass region with a ~100 kg array of EDELWEISS detectors EDELWEISS in would require the environment SuperCDMS -EURECA projected for EURECA/ " SuperCDMS" Jocelyn Monroe April 27, 2017 / p. 18 Low Mass, CRESST (thanks to F. Petricca) LargeCRESSTCRESST σ CRESST- II 300g scintillating CaWO4 crystals Measured nuclear recoil threshold ~300eV ● Leading sensitivity in low mass region ● Explore masses in the sub-GeV/c2 range CRESST – III arXiv:1503.08065 C R C E R S ES S 25g CaWO4 crystals S T T I II I Optimized for nuclear recoil threshold <100eV ( (2 20 0 1 1 5 4 ) ) CR Phase 1 ES ST - ● Mounting of 10 modules completed III Ph ● as Cool down in 2016the next weeks C e 1 RE ● 1 year of running ~50 kg days (2017) SS T- III Ph as e 2 Phase 2 ● 100 modules with improved background to approach the neutrino floor in the LNGS setup Jocelyn Monroe CRESST April 27, 2017 / p. 19 Low Mass, Large σ Annual Modulation Tests predicted modulation A~0.02-0.1, t0=152.5 days t0 = DAMA/LIBRA: measure (0.0112±0.0012) cpd/kg/keV, t0 = (144±7) d in 1.33 T-yr. XENON100: Xe, 4.8σ exclusion of DAMA, test of leptophilic dark matter arXiv:1507.07748 CoGeNT (dashed line) XMASS: Xe, 833 kg in Kamioka, model-independent analysis modulation result reported arXiv:1511.04805 CDMS (solid points) Jocelyn Monroe February 22, 2016 / p. 11 Low Mass, Large σ Annual Modulation Tests predicted modulation A~0.02-0.1, t0=152.5 days t0 = DAMA/LIBRA: measure (0.0112±0.0012) cpd/kg/keV, t0 = (144±7) d in 1.33 T-yr. XENON100: Xe, 4.8σ exclusion of DAMA, test of leptophilic dark matter arXiv:1507.07748 CoGeNT (dashed line) XMASS: Xe, 833 kg in Kamioka, model-independent analysis modulation result reported arXiv:1511.04805 CDMS (solid points) Jocelyn Monroe February 22, 2016 / p. 11 Low Mass, Large σ Annual Modulation Tests predicted modulation A~0.02-0.1, t0=152.5 days t0 = DAMA/LIBRA: measure (0.0112±0.0012) cpd/kg/keV, t0 = (144±7) d in 1.33 T-yr. XENON100: Xe, 4.8σ exclusion of DAMA, test of leptophilic dark matter arXiv:1507.07748 CoGeNT (dashed line) XMASS: Xe, 833 kg in Kamioka, model-independent analysis modulation result reported arXiv:1511.04805 CDMS (solid points) Jocelyn Monroe February 22, 2016 / p. 11 Low Mass, (thanks to J. Villar) Large σ Annual Modulation Prospects +ANAIS (Canfranc), DM-Ice+KIMS = COSINE (YangYang), SABRE (AU) COSINE data, Lake Louise 2017 Jocelyn Monroe April 27, 2017 / p.
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  • Dark Matter Direct Detection

    Dark Matter Direct Detection

    Dark Matter Direct Detection Jocelyn Monroe, Royal Holloway University of London PPAP Community Meeting University of Birmingham September 18, 2012 Outline 1. Dark Matter Direct Detection Overview • What are the top scientific challenges in Particle Physics to be solved in the next 20-30 years? 2. Current and Future UK Efforts 3. DMUK Collaboration Input to PPAP • What current and future facilities will be needed for the UK to make significant contributions to these areas? • What are the technology needs for each key priority? • What is the appropriate programmatic balance between construction, operations, exploitation, and R&D? 4. Conclusions (my opinions) The Standard Model of Cosmology E. Komatsu et al., Astrophys. J. Suppl 192 (2011) 18 evidence from CMB, galaxy clusters, large scale structure, supernova data, distance measurements, gravitational lensing Dark Matter is ~25% of the universe. RHUL Jocelyn Monroe Sept. 18, 2012 We only understand 4% of the universe! E. Komatsu et al., Astrophys. J. Suppl 192 (2011) 18 No good Standard Model dark matter particle candidates... new physics ? required. ?? (NASA) Dark matter is globally acknowledged to be one of the top scientific challenges in Particle Physics to be solved in the next 20-30 years, perhaps the top challenge. RHUL Jocelyn Monroe Sept. 18, 2012 Direct Dark Matter Detection χ Signal: χN ➙χN’ Scintillation χ Heat Ionization Backgrounds: n N ➙ n N’ γ e- ➙ γ e-’ N ➙ N’ + α, e- ν N ➙ ν N’ RHUL Jocelyn Monroe Sept. 18, 2012 Around the World KIMS NEWAGE XMASS, PANDA-X DEAP/CLEAN Picasso COUPP DRIFT LUX CDMS Xenon100 DAMA CRESST DMTPC DarkSide DM-ICE Confirmation of EDELWEISS signal from multiple SIMPLE, ANAIS technologies required.