Dark Matter Direct Detection

Transcription

1 Dark Matter Direct Detection Laura Baudis, UZH Jocelyn Monroe, RHUL Outline 1) Scientific Context 2) Community Input: 5-10 year Horizon for Direct Detection in Europe 3) APPEC GA Considerations for Discussion Financial Context: bottom line in SAC Report to APPEC GA (2014): funding: 9ME/yr currently, ~12ME/yr requested, : ME/yr for G3 experiment(s) construction effort: currently scientists, engineers Jocelyn Monroe April 6, 2016 / p. 1

2 Standard Model of Cosmology Dark Matter is ~30% of the energy density of the universe. Jocelyn Monroe April 6, 2016 / p. 2

3 Searches for Dark Matter Indirect Detection Collider Production jet e-,ν,γ? e+,p,d Direct Detection N Jocelyn Monroe April 6, 2016 / p. 3 N

4 Model Space Wide range of parameters! Direct detection searches generally optimised for WIMP sensitivity... Baer et al., arxiv: Jocelyn Monroe April 6, 2016 / p. 4

5 Model Space Wide range of parameters! Direct detection searches generally optimised for WIMP sensitivity... Baer et al., arxiv: Jocelyn Monroe April 6, 2016 / p. 4

6 Model Space Wide range of parameters! Direct detection searches generally optimised for WIMP sensitivity... but starting to look for axions too! axion model space dark matter = axions Baer et al., arxiv: Jocelyn Monroe April 6, 2016 / p. 4

7 The Low-Background Frontier: Prospects 1 event/ kg/day 1 event/ 100kg/day 1 event/ 100 kg/ 100 days so far: ~3 years / order of magnitude Jocelyn Monroe April 6, 2016 / p. 5

8 The Low-Background Frontier: Prospects Low Mass, Large σ 1 event/ kg/day Canonical MSSM Mass, σ > Neutrino Bound 1 event/ 100kg/day High Mass, Tiny σ or Large # Events 1 event/ 100 kg/ 100 days so far: ~3 years / order of magnitude Jocelyn Monroe April 6, 2016 / p. 5

9 Prospects: Near Term to 10-Year Horizon* CRESST +EDELWEISS =EURECA annual modulation DAMIC + R&D efforts DEAP3600 XENON-1T LZ XENON-nT + others DarkSide+ArDM=ARGO DARWIN R&D for direction sensitivity *=for projects with funding from, or planned for Europe Jocelyn Monroe April 6, 2016 / p. 5

10 Low Mass, Large σ EDELWEISS (thanks to J. Gascon) EDELWEISS! Largest operating cryogenic Ge array (20 kg) for Direct DM search" Latest results: arxiv: " 2017 LSM: optimizing sensitivity to 1-10 GeV WIMPs" Beyond: completing the exploration of the low-wimp mass region with a ~100 kg array of EDELWEISS detectors would require the environment projected for EURECA/ SuperCDMS" Jocelyn Monroe CRESST 2012! EDEL WEIS S in Su percd MS-E UREC A" April 6, 2016 / p. 6

11 Low Mass, Large σ CRESST (thanks to F. Petricca)! "#! $%&' ( )*+,-./, (, #! !!# " 4 + 1, 4 5( (+,7 % % ( 99 5(+7 3 ( +!!# $4 ## 1 8& # Jocelyn Monroe April 6, 2016 / p. 7

12 Low Mass, Large σ EURECA (thanks to K. Eitel) EURECA accomplish low mass goals of EDELWEISS-III and CRESST-III phase 1 by common cryogenic infrastructure with SuperCDMS in SNOLAB by 2019 contribute detectors and tower integration SuperCDMS@SNOLAB CUTE project Queen s test facility at SNOLAB by 2017 to test tower integration & bgd suppression SCDMS design KIT mockup of tower 20 Jocelyn Monroe April 6, 2016 / p. 8

13 Low Mass, Large σ Annual Modulation Searches (thanks to J. Villar) DAMA (LNGS), DM-Ice (S. Pole, Boulby), ANAIS (Canfranc), ++ Jocelyn Monroe April 6, 2016 / p. 9

14 MSSM Mass, σ > ν bound XENON-100 (thanks to L. Baudis) Ultra-low background and design sensitivity achieved Background: ~ 5 x 10-3 events/(kg d kev) No evidence for WIMP dark matter Upper limits on SI, SD WIMP-nucleon cross sections (PRL 109, PRL 111) Axion, ALPS searches (Phys. Rev. D 90, (2014) Annual modulation search excludes leptophilic DM explanation of DAMA/LIBRA (Science 349, 2015) SD-neutron SD-proton Jocelyn Monroe April 6, 2016 / p. 10

15 MSSM Mass, σ > ν bound XENON-1T / Xenon-nT continues from XENON-10, XENON-100 at LNGS (thanks to E. Aprile) arxiv: , accepted in JCAP XENON-1T: 3.5 Tonnes LXe (1T fiducial). TPC installed Nov. 2015, 1st physics run: summer Sensitivity to 1E-47 cm 2 in 2 Tonne-years. XENON-nT: upgrade to 7T LXe (total), using same infrastructure + new TPC, inner cryostat. From LZ: follow-on to LUX at SURF, 7T LXe (total). Passed CD-1/3a in Sensitivity to 2E-48 cm 2. Jocelyn Monroe April 6, 2016 / p. 11

16 MSSM Mass, σ > ν bound DarkSide-50 (thanks to G. Fiorini) LArTPC (50 kg active, 150kg total) 38 3 PMTs at LNGS Liquid scintillator veto (30 tons) 110 PMTs Water veto (1 ktons) 80 PMTs Demonstrated: β/γ rejection capability better than with atmospheric argon high-performance vetoing scheme and 39 Ar suppression in underground argon by factor over 1,000 Zero background operation: 1,422 kg d AAr (published) 2,616 kg d UAr (published) 8,000 kg d UAr (analysis ongoing) Jocelyn Monroe April 6, 2016 / p. 12

17 MSSM Mass, σ > ν bound ArDM-1t Ton- scale LAr TPC at Canfranc underground Laboratory (LSC, 2500 m.w.e. 850 kg acfve mass, 24 8 PMTs, low background 1st 6- month run in single phase in 2015: to explore features of LAr for DM@ton- scale Now preparing double phase Run II scheduled for and beyond: (a) accumulate stafsfcs + light yield/hardware upgrades (b) depleted argon studies with sensifvity down to 10-5 together with DarkSide. DemonstraFon at the ton- scale is a necessary step towards 10- tons and beyond. Pulse shape discriminafon (thanks to A. Rubbia) Low BG studies Jocelyn Monroe April 6, 2016 / p. 13

18 MSSM Mass, σ > ν bound DEAP-3600 Single Phase liquid Argon detector, a la neutrino detectors like SNO: self-shielding of target, detect scintillation only with 4π PMT coverage DEAP-3600: 3.6 T LAr at SNOLAB. Project <0.6 background in 3 T-years, 1E-46 cm 2 reach. Commissioning since 2015, physics start Spring Single phase: R&D towards the ktonne scale in dark matter detection no electric fields = scale to large masses (a la νs) 1) no pile-up from ms-scale electron drift in TPC 2) no recombination in E field but background discrimination from scintillation only! Trigger rate vs. Fme (shows veto fill) Jocelyn Monroe April 6, 2016 / p. 12

19 High Mass, Large # Events σ < ν bound ARGO (thanks to C. Galbiati) An Integrated Program for the Ultimate DM Search with 39 Ar-suppressed Argon TPCs Ultimate search requires 1,000 T-yr background-free exposure 39 Ar-suppressed Ar TPC can deliver due to β/γ suppression Key enabling technologies R&D funded and ongoing: Cryogenic SiPMs Urania: 100 kg/d procurement of UAr Aria: active isotopic separation of 39 Ar via cryogenic distillation arkside-50 (now) ArDM-1t (now) DarkSide-20k (2020?) Argo (2025?) 100 T-yr background-free search 1,000 T-yr background-free search to reach the neutrino floor precision low-energy solar neutrino measurements Jocelyn Monroe April 6, 2016 / p. 15

20 High Mass, Large # Events σ < ν bound DARWIN UlFmate LXe TPC at LGNS. 50 t (40 t) Lxe in total (in the TPC) ~10 3 photosensors 2.6 m dri] length, 2.6 m diameter TPC Background: dominated by neutrinos WIMP spectroscopy, search + non- WIMP science: axion / ALP search, solar neutrinos, supernova neutrinos, sterile neutrinos, coherent neutrino nucleus sca`ering, 0ν2β decay of 136 Xe. (thanks to L. Baudis) JCAP10 (2015) 016 Update: Newstead et al., PRD D 88, (2013) Jocelyn Monroe Update: Newstead et al., PRD D 88, April 6, (2013) 2016 / p. 16

21 WIMPs are not the only possibility! IAXO (thanks to I. Irastorza) IAXO builds on decade of European axion helioscopes: CAST at CERN. Timeline: Conceptual Design 2013 Letter of Intent to SPSC 2014, received positive recommendation to develop TDR TDR design and prototyping ongoing: IAXO-D0: low background x-ray detectors prototypes, IAXO-X0 : x-ray optics IAXO-T0: superconducting magnet coil Funding path for TDR (almost) clear. complementary reach with cavity searches, + >10x gain in QCD axion reach over current results HB hint Large toroidal 8-coil magnet L = ~20 m 8 bores: 600 mm diameter each 8 x-ray telescopes Rotating platform NDW>1 Axion Enhanced axion helioscope: JCAP 1106:013,2011 Discussion for funding path for IAXO underway includes scenarios with IAXO in sites alternative to CERN Critical moment for the project, with first dedicated funding support from APPEC roadmap very important for the project Jocelyn Monroe April 6, 2016 / p. 17

22 Voltage dark matter identification, σ > ν bound Directional Detection R&D towards DM recoil track direction to identify a signal with the galactic halo arxiv: DMTPC n calibration data, DMTPC MC fit template n calibration data, 50 kevr charge data, nuclear recoil 150 kevr anode grid DRIFT: 1m 3 MWPC, in Boulby since 2001 DMTPC: optical (CCD) and charge readout of CF 4 ; commissioning 1m 3 module. MIMAC: micromegas, in LSM. Low E focus. time (s) R&D: fine-grained emulsions ++ + projects outside Europe DMTPC CYGNUS: global coordination towards a physics-scale directional experiment. Directionality gains up to 10x in sensitivity in the presence of backgrounds (relative to 1D). and there is no neutrino bound for directional detectors. Phys.ReV.D90 (2014) Jocelyn Monroe April 6, 2016 / p. 18

23 APPEC GA Considerations for Discussion Europe should: 1) support and closely follow the development/results of the G2 experiments directly searching for WIMP DM in 1 GeV-10 TeV/c 2 range. 2) APPEC should appoint a scientific and technical committee to work with the European DM community to recommend the technologies for noble-liquid G3 direct detection experiments in synergy/ complementarity with similar detectors in other regions of the world 3) support the participation of European groups in an international large G3 bolometric detector (e.g. EURECA). 4) support R&D and technology to build a directional detector. 5) support non-wimp searches and R&D activities (e.g. axions: ADMX, IAXO; ALPS, hidden sector particles: SHIP, ++) 6) encourage the synergy with indirect searches (e.g. CTA, KM3NET) Jocelyn Monroe April 6, 2016 / p. 19

24 My Comments Europe should: 1) increase the resources in this area. Fraction of the energy density of the universe: 30%. Fraction of astroparticle funding in Europe: <10%. Fraction of European astroparticle physicists working in this area: 25%* 2) Europe has some of the best facilities in the world for this science, with a decade of world-leading results. Should site G3 project(s) here. 3) Dark matter experiment costs are small relative to telescopes, long baseline neutrino oscillations, space missions, etc. A coherent strategy to maximize discovery potential could be to have strong participation in searches at range of WIMP mass scales (low, mid, high). ( coherent doesn t by definition mean only one experiment is funded.) 4) maximize discovery potential through increased participation in searches for other dark matter particle candidates (IAXO, ALPS, SHIP) *=includes people working on multiple projects, with overlap in other areas Jocelyn Monroe April 6, 2016 / p. 20