Axion search with Dark Matter detector
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1 Axion search with Dark Matter detector Paolo Beltrame Durham IPPP, 14th March
2 Direct DM search Dark matter (DM) Milky Way s halo => flux on Earth ~ 10 5 cm -2 s -1 ρχ ~ 0.3 GeV/cm 3 and 100 GeV/c 2 Basic goal: search for nuclear recoil from DM elastic scattering. Simple dynamics: cross section (form-factor) 2 Spin-independent: nucleon form-factor gives rise to A 2 enhancement due to coherence. The dependence on q 2 is also contained in the form-factors. Spin-dependent: form-factor depends on nuclear spin. No coherence enhancement. 2
3 S1, S2 and CES Liquid xenon / dual-phase time projection chamber (TPC) (Ionisation) S2 1 μs (Scintillation) S1 100 ns 3
4 S1, S2 and CES Liquid xenon / dual-phase time projection chamber (TPC) (Ionisation) S2 100 ns 1 μs (Scintillation) S1 4 Combined Energy scale E = 1 S1 L(E) + S2 W g 1 g 2 W = 13.7 ev g1 = Light Collection g2 = Extraction + Light Eff. L(E) = Lindhard Factor Nuclear recoil enhancement of heat relative to electron recoils
5 Nuclear vs. Electron recoil Combination of Scintillation (S1) and Ionisation (S2) event-by-event particle identification Electron Recoil (ER) events Nuclear Recoil (NR) events 2.5 (a) Tritium ER Calibration ER calibration data log10log (S210 /S1) x,y,z corrected b (S2/S1) kevee (b) AmBe and Cf 252 NR Calibration NR calibration data kevnr S1 x,y,z corrected (phe) S1 5 FIG. 3. Calibrations of detector response in the 118 kg fiducial
6 Spin-independent arxiv: cm 2 Z exchange Z pb Higgs exchange h pb Limit on Spin-Independent WIMP-nuclei at 6 x cm 2 at 33 GeV/c 2
7 LZ = LUX + ZEPLIN Counts: 31 Institutions 200 Headcount Center for Underground Physics (Korea) LIP Coimbra (Portugal) MEPhI (Russia) Edinburgh University (UK) University of Liverpool (UK) Imperial College London (UK) University College London (UK) University of Oxford (UK) STFC Rutherford Appleton, and Daresbury, Laboratories (UK) University of Sheffield (UK) 7 University of Alabama University at Albany SUNY Berkeley Lab (LBNL) Brookhaven National Laboratory University of California Berkeley Brown University University of California, Davis Fermi National Accelerator Laboratory Lawrence Livermore National Laboratory University of Maryland Northwestern University University of Rochester University of California, Santa Barbara University of South Dakota South Dakota School of Mines & Technology South Dakota Science and Technology Authority SLAC National Accelerator Laboratory Texas A&M Washington University University of Wisconsin Yale University
8 The detector (LUX): world leading Generation-1 experiment, Sanford Underground Research Facility (SURF), 250 kg of active LXe target Cathode high voltage feedthrough LUX-ZEPLIN (LZ): Generation-2 flagship experiment for Direct Detection in US and UK, 7 tonnes of active LXe target arxiv: Existing water tank Outer Detector Gd-loaded liquid scintillator Outer Detector PMTs 7 tonne active LXe TPC PMTs: 488 Skin PMTs: (192) LXe heat exchanger 8
9 LZ timeline Year Month Activity 2012 March LZ (LUX-ZEPLIN) collaboration formed September DOE CD-0 for G2 dark matter experiments 2013 November LZ R&D report submitted 2014 July LZ Project selected in US and UK 2015 April DOE CD-1/3a approval, similar in UK Begin long-lead procurements (Xe, PMT, cryostat) 2016 April DOE CD-2/3b review 2017 February LUX removed from underground 2017 July Begin surface assembly SURF 2018 May Begin underground installation 2019 April Begin commissioning 2021 Q3FY21 CD-4 milestone (early finish July 2019) 2025 Planning on ~5 year of operations 9
10 Projected sensitivity Simulated LZ experiment (1000 days, 5.6 tonnes fiducial) (arxiv: ) Baseline σsi = 2.2 x cm 2 B-8 = 7 ATM ν = 0.4 Goal σsi = 1.2 x cm 2 B-8 = 220 ATM ν = 3 10
11 Projected sensitivity Simulated LZ experiment (1000 days, 5.6 tonnes fiducial) (arxiv: ) Baseline σsi = 2.2 x cm 2 B-8 = 7 ATM ν = 0.4 Goal σsi = 1.2 x cm 2 B-8 = 220 ATM ν = 3 New sensitivity study performed with updated low E LXe response and with PLR instead of Feldman-Cousins 10
12 Direct detection timeline Ge, NaI no discrimination Ge, w/discrim. ZEPLIN-III LXe, w/discrim. LUX CDMS Darkside SCDMS DEAP XENON 1T LZ cm 2 (XENON nt) 11
13 Axion with DM direct search experiment 12
14 Publications K. Arisaka, P. Beltrame et al., Astroparticle Physics 44 (2013) M. Pospelov et al., Phys. Rev. D 78 (2008), E. Aprile et al. (XENON100), Phys. Rev. D90 (2014),
15 Theory Experimental detection with Invisible axion could be the QCD axion solving the CP violation problem xenon Axions and axion-like particles can couple with electron (gae) Axion-Like Particle, introduced by several extension of the SM, are good Dark Matter candidates Sources: - Solar Axion from Sun - Axion-Like particle slowly moving within our galaxy 14
16 Axio-electric effect Axion-Like particles Experimentally detectable in the Xe exploiting the axion-electric effect (proportional to the photoelectric effect) Ae = pe (E A ) g Ae 2 A 3E A 2 16 em m e 2 1 2/3 A 3! A Z +,e- g Ae e- Z +,e- A.V. Assuming Galactic 15
17 Axio-electric effect (solar) Production from Sun J. Redondo, JCAP12 (2013) 008 Solar flux (gae = 1 x ) Detection within the detector photo-electric cross section for xenon Valid up to 1 kev Ae = pe (E A ) g Ae 2 A 3E A 2 16 em m e 2 1 2/3 A 3! 16
18 17 Astroparticle Physics 44 (2013) 59 67
19 Solar Axion 0 kev mass S2 AXION pdf axioneventdensity 10 Entries kev mass Mean x Mean y 1.393e+04 RMS x RMS y Ae = pe (E A ) g Ae 2 A 3E A 2 16 em m e 2 1 2/3 A 3! S1 0 18
20 Solar Axion Preliminary 19
21 Galactic ALPs S2 S2 AXION pdf axioneventdensity 10 Entries Mean x Mean y 1.533e+04 RMS x RMS y S axioneventdensity 10 Entries Mean x Mean y 6.098e+04 RMS x RMS y 1.038e AXION pdf S2 AXION pdf axioneventdensity 10 Entries Mean x Mean y e+04 RMS x RMS y kev mass 15 kev mass S1 AXION pdf axioneventdensity 10 Entries Mean x Mean y 8.469e RMS x RMS y 1.436e kev mass 35 kev mass S S S1 0
22 Galactic ALPs Preliminary 21
23 Summary Dual-phase Xe DM direct detector are suitable for axion searches Proven by XENON100 (E. Aprile et al. (XENON100), Phys. Rev. D90 (2014), ) Sensitivity to gae Issue: signal sitting exactly where the dominant background is (ER events) 22
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