Status and Recent Dark Matter Search Results from the Pandax Experiment
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The Darkside Experiment for Direct Dark Matter Search with Liquid Argon
The DarkSide experiment for direct dark matter search with liquid argon Alexander Kish University of Hawaii on behalf of the DarkSide collaboration 3rd South American Dark Matter Workshop, December 3, 2020 Outline ・DarkSide-50 (DS-50) dual-phase argon TPC and its latest physics results ・Status of the DarkSide-20k (DS-20k) experiment and associated R&D ・Global Argon Dark Matter Collaboration (GADMC) and ARGO ・Coherent neutrino-nucleus scattering (CEνNS) and sensitivity of the future large argon TPCs to core-collapse supernova neutrinos Alex Kish, University of Hawaii DarkSide @ DMW2020, December 3, 2020 2 The DarkSide-50 Experiment Water Cherenkov detector ・stainless steel cylinder (D 11m, H 10m) ・1kT of ultra-pure H20 ・80 PMTs (8”) ➝ passive shield for external radiation ➝ active veto for muons Liquid scintillator detector ・stainless steel sphere (D 4m) ・30t of 10B-loaded liquid scintillator ・110 PMTs (8”) ➝ active gamma and neutron veto Inner argon TPC ・PTFE cylinder with 46kg LAr target ・38 Hamamatsu PMTs (3”, R11065) ・TPB-coated inner surfaces ・fused silica diving bell with 1cm gas pocket ・transparent silica cathode and anode coated by ITO (indium tin oxide) Alex Kish, University of Hawaii DarkSide @ DMW2020, December 3, 2020 3 DarkSide-50 TPC ・38 Hamamatsu PMTs (3”, R11065) ・TPB-coated inner surfaces ・PTFE cylinder with 46kg LAr target ・fused silica diving bell with 1cm gas pocket ・transparent silica cathode and anode coated by ITO (indium tin oxide) Cryogenic pre-amplifier Alex Kish, University of Hawaii DarkSide @ DMW2020, December -
Future Plan of the Pandax Experiment
Future plan of the PandaX Experiment - report at the CJPL International Advisory Committee meeting PandaX Collaboration, 9 Nov., 2016 The PandaX (Particle and astrophysical Xenon) observatory uses xenon as target and detector to search for WIMP particles as well as neutrinoless double beta decay (NLDBD) in 136Xe. At present, the PandaX-II experiment is in operation in CJPL-I. The future PandaX program will pursue the following three main directions: 1. Continue the operation of PandaX-II until a total of 2-year exposure; 2. Develop and operate a multi-ton multi-purpose liquid xenon experiment, PandaX-xT, to push further the dark matter search; 3. Develop and operate a 200-kg (upgradable to ton-scale) high pressure gas TPC (HpgTPC), PandaX-III, to search for NLDBD in 136Xe. Each direction is elaborated below. PandaX-II operation PandaX-II has published the world leading WIMP limit with a 99-day exposure, reaching an upper limit to spin-independent WIMP-nucleon cross section of 2.5x10-46cm2 [1]. The current plan is to maintain stable operation until we have data with a 2-year total live time. Calibration runs will be interleaved to monitor the detector response. The wealth of low background data will allow us to pursue many different physics analyses (in additional to the standard WIMP- nucleon elastic scattering), including constraints to generic WIMP-nucleon operators, light WIMPs, inelastic WIMPs, limits to solar and galactic axions, etc. We will also use the PandaX-II detector to test new technologies for a future multi-ton detector, e.g. online Kr removal, upgrade of the trigger/electronics system to achieve a lower threshold and a higher data bandwidth, alternative electron recoil and nuclear recoil calibrations, etc. -
Gustavo Marques-Tavares, Stanford Institute for Theoretical Physics
Detecting dark particles from Supernovae Gustavo Marques-Tavares, Stanford Institute for Theoretical Physics In collaboration with W. deRocco, P. Graham, D. Kasen and S. Rajendran Dark matter WIMP searches 5 -37 ACKNOWLEDGMENTS 10 -38 10 PandaX-II 2016 10-39 LUX 2016 ) 2 10-40 CDMSLite 2015 CRESST-II 2015 10-41 10-42 -43 10 SuperCDMS Post LHC1 mSUSY constraint 1700 kg-days 10-44 10-45 -46 10 6 t-y PandaX-4T 10-47 XENON1T 2 t-y LZ 15.6 t-y SI WIMP-nucleon cross section (cm XENONnT 20 t-y 10-48 200 t-y xenon (DARWIN or PandaX-30T) 10-49 Neutrino coherent scattering 10-50 1 10 102 103 WIMP mass (GeV/c2) *Figure taken from arxiv:1709.00688 This work is supported by grants from the Na- FIG. 4. The projected sensitivity (dashed curves) on the spin- tional Science Foundation of China (Nos. 11435008, independent WIMP-nucleon cross-sections of a selected num- ber of upcoming and planned direct detection experiments, 11455001, 11505112 and 11525522), a grant from the including XENON1T [34], PandaX-4T, XENONnT [34], Ministry of Science and Technology of China (Grant No. LZ [35], DARWIN [36] or PandaX-30T, and SuperCDMS [56]. 2016YFA0400301), and in part by the Chinese Academy Currently leading limits in Fig. 1 (see legend), the neutrino of Sciences Center for Excellence in Particle Physics ‘floor’ [20], and the post-LHC-Run1 minimal-SUSY allowed (CCEPP), the Key Laboratory for Particle Physics, As- contours [21] are overlaid in solid curves for comparison. The trophysics and Cosmology, Ministry of Education, and di↵erent crossings of the experimental sensitivities and the Shanghai Key Laboratory for Particle Physics and Cos- 2 neutrino floor at around a few GeV/c are primarily due to mology (SKLPPC). -
Light Dark Matter at Boulby Liquid Argon Liquid Xenon MAGIS Dark Matter Summary Comments
Summary of Dark Matter Kimberly Palladino Inputs to the Roadmap Light Dark Matter at Boulby Liquid Argon Liquid Xenon MAGIS Dark Matter Summary Comments ‣ Dark Matter and other new physics are strong physics motivations (STFC C:4) ‣ A quickly growing subfield both in membership in individual projects, and new projects ‣ Input submissions highlight opportunities for leadership if funding is expanded in this area ‣ Difficult to judge purely by numbers of researchers, as existing funding also shapes the field ‣ UKRI Quantum Technology for Fundamental Physics interest and results (recent HEP Forum discussions) highlight this breadth ‣ Boulby Underground Laboratory is a key facility ‣ Summarising 4 inputs now, encourage more! 2 Light DM at Boulby: EFCu and DarkSPHERE ‣ Rare-event search experiments rely upon electroformed copper for their physics goals (dark matter and neutrinoless double-beta decay) ‣ ECUME at SNOLAB, partnered with PNNL, bring experience to Boulby ‣ Low-mass dark matter searches with NEWS-G ‣ Dark Matter search in 0.05 -10 GeV mass range, aiming for the neutrino ‘floor’ ‣ motivated by hidden sectors, asymmetric dark matter, and effective field theory ‣ Cu Spherical Proportional Counter filled with light gas mixtures ‣ SEDINE at LSM 60 cm dia., SNOGLOBE at SNOLAB 1.4 m dia, DarkSPHERE at Boulby 3m dia. ‣ swappable targets, single ionization electron sensitivity, background rejection and fiducialisation 3 Light DM at Boulby: UK spotlight ‣ UK groups: Boulby, KCL, RAL, RHUL, UCL, Birmingham, Liverpool ‣ Build EFCu expertise -
S. Ting June 17, 2014
The Latest Results from The Alpha Magnetic Spectrometer on the International Space Station June 17, 2014 S. Ting AMS: a U.S. DOE led International Collaboration 15 Countries, 44 Institutes and 600 Physicists FINLAND UNIV. OF TURKU RUSSIA ITEP NETHERLANDS KURCHATOV INST. ESA-ESTEC GERMANY NIKHEF RWTH-I. KIT - KARLSRUHE KOREA USA FRANCE EWHA MIT - CAMBRIDGE LUPM MONTPELLIER KYUNGPOOK NAT.UNIV. NASA GODDARD SPACE FLIGHT CENTER LAPP ANNECY CHINA NASA JOHNSON SPACE CENTER LPSC GRENOBLE TURKEY CALT (Beijing) UNIV. OF HAWAII METU, ANKARA IEE (Beijing) UNIV. OF MARYLAND - DEPT OF PHYSICS IHEP (Beijing) YALE UNIVERSITY - NEW HAVEN PORTUGAL SWITZERLAND ETH-ZURICH NLAA (Beijing) LAB. OF INSTRUM. LISBON SJTU (Shanghai) UNIV. OF GENEVA SEU (Nanjing) SPAIN SYSU (Guangzhou) CIEMAT - MADRID SDU (Jinan) I.A.C. CANARIAS. ITALY TAIWAN ASI ACAD. SINICA (Taipei) IROE FLORENCE CSIST (Taipei) MEXICO INFN & UNIV. OF BOLOGNA NCU (Chung Li) UNAM INFN & UNIV. OF MILANO-BICOCCA INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF TRENTO D. Goldin, former NASA Administrator realized the unique potential of ISS for fundamental science and has supported AMS from the beginning May 16, 2011 May 15, 2011 May 09, 1994 NASA support Mr. William Gerstenmaier has visited AMS regularly More than 10 times, at CERN, KSC, ESTEC . Mr. Mike Suffredini and Mr. Rod Jones have also strongly supported AMS. Their support has made it possible for AMS to collect data continuously The construction of AMS was, and AMS operations are, supervised continuously by NASA-JSC team of Trent Martin, Ken Bollweg and many others. 4 Strong support of STS-134 astronauts (Mark Kelly, Gregory H. -
Neutrinoless Double Beta Decay Searches
FLASY2019: 8th Workshop on Flavor Symmetries and Consequences in 2016 Symmetry Magazine Accelerators and Cosmology Neutrinoless Double Beta Decay Ke Han (韩柯) Shanghai Jiao Tong University Searches: Status and Prospects 07/18, 2019 Outline .General considerations for NLDBD experiments .Current status and plans for NLDBD searches worldwide .Opportunities at CJPL-II NLDBD proposals in China PandaX series experiments for NLDBD of 136Xe 07/22/19 KE HAN (SJTU), FLASY2019 2 Majorana neutrino and NLDBD From Physics World 1935, Goeppert-Mayer 1937, Majorana 1939, Furry Two-Neutrino double beta decay Majorana Neutrino Neutrinoless double beta decay NLDBD 1930, Pauli 1933, Fermi + 2 + (2 ) Idea of neutrino Beta decay theory 136 136 − 07/22/19 54 → KE56 HAN (SJTU), FLASY2019 3 ̅ NLDBD probes the nature of neutrinos . Majorana or Dirac . Lepton number violation . Measures effective Majorana mass: relate 0νββ to the neutrino oscillation physics Normal Inverted Phase space factor Current Experiments Nuclear matrix element Effective Majorana neutrino mass: 07/22/19 KE HAN (SJTU), FLASY2019 4 Detection of double beta decay . Examples: . Measure energies of emitted electrons + 2 + (2 ) . Electron tracks are a huge plus 136 136 − 54 → 56 + 2 + (2)̅ . Daughter nuclei identification 130 130 − 52 → 54 ̅ 2νββ 0νββ T-REX: arXiv:1512.07926 Sum of two electrons energy Simulated track of 0νββ in high pressure Xe 07/22/19 KE HAN (SJTU), FLASY2019 5 Impressive experimental progress . ~100 kg of isotopes . ~100-person collaborations . Deep underground . Shielding + clean detector 1E+27 1E+25 1E+23 1E+21 life limit (year) life - 1E+19 half 1E+17 Sn Ca νββ Ge Te 0 1E+15 Xe 1E+13 1940 1950 1960 1970 1980 1990 2000 2010 2020 Year . -
Diurnal Effect of Sub-Gev Dark Matter Boosted by Cosmic Rays
Diurnal Effect of Sub-GeV Dark Matter Boosted by Cosmic Rays Shao-Feng Ge,1,2, ∗ Jianglai Liu,2,1, † Qiang Yuan,3, 4, 5, ‡ and Ning Zhou2, § 1Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai 200240, China 2School of Physics and Astronomy, Shanghai Jiao Tong University, Key Laboratory for Particle Astrophysics and Cosmology (MOE) & Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai 200240, China 3Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China 4School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China 5Center for High Energy Physics, Peking University, Beijing 100871, China We point out a new type of diurnal effect for the cosmic ray boosted dark matter (DM). The DM- nucleon interactions not only allow the direct detection of DM with nuclear recoils, but also allow cosmic rays to scatter with and boost the nonrelativistic DM to higher energies. If the DM-nuclei scattering cross sections are sufficiently large, the DM flux is attenuated as it propagates through the Earth, leading to a strong diurnal modulation. This diurnal modulation provides another prominent signature for the direct detection of boosted sub-GeV DM, in addition to signals with higher recoil energy. Introduction – Overwhelming evidence from astrophys- signals in large neutrino experiments [44–46]. ical and cosmological observations supports the existence For sub-GeV DM, the DM-nucleon scattering cross sec- of dark matter (DM) [1], which is gravitationally interact- tion with a contact interaction can be quite sizable, e.g., ing but invisible via electromagnetic interactions. -
27. Dark Matter
1 27. Dark Matter 27. Dark Matter Written August 2019 by L. Baudis (Zurich U.) and S. Profumo (UC Santa Cruz). 27.1 The case for dark matter Modern cosmological models invariably include an electromagnetically close-to-neutral, non- baryonic matter species with negligible velocity from the standpoint of structure formation, gener- ically referred to as “cold dark matter” (CDM; see The Big-Bang Cosmology—Sec. 22 of this Re- view). For the benchmark ΛCDM cosmology adopted in the Cosmological Parameters—Sec. 25.1 of this Review, the DM accounts for 26.4% of the critical density in the universe, or 84.4% of the total matter density. The nature of only a small fraction, between at least 0.5% (given neutrino os- cillations) and at most 1.6% (from combined cosmological constraints), of the non-baryonic matter content of the universe is known: the three Standard Model neutrinos (see the Neutrino Masses, Mixing, and Oscillations—Sec. 14 of this Review) ). The fundamental makeup of the large majority of the DM is, as of yet, unknown. Assuming the validity of General Relativity, DM is observed to be ubiquitous in gravitation- ally collapsed structures of size ranging from the smallest known galaxies [1] to galaxies of size comparable to the Milky Way [2], to groups and clusters of galaxies [3]. The mass-to-light ratio is observed to saturate at the largest collapsed scales to a value indicative, and close to, what inferred from other cosmological observations for the universe as a whole [4]. In such collapsed structures, the existence of DM is inferred directly using tracers of mass enclosed within a certain radius such as stellar velocity dispersion, rotation curves in axisymmetric systems, the virial theorem, gravitational lensing, and measures of the amount of non-dark, i.e. -
Latest Results of Dark Matter Detection with the Darkside Experiment ∗ E
IL NUOVO CIMENTO 43 C (2020) 26 DOI 10.1393/ncc/i2020-20026-3 Colloquia: IFAE 2019 Latest results of dark matter detection with the DarkSide experiment ∗ E. Picciau( ) INFN, Sezione di Cagliari and Dipartimento di Fisica, Universit`a degli Studi di Cagliari Cagliari, Italy received 8 June 2020 Summary. — In this contribution the latest results of dark matter direct detection obtained by the DarkSide Collaboration are discussed. New limits on the scattering cross-section between dark matter particles and baryonic matter have been set. The results have been reached using the DarkSide-50 detector, a double-phase Time Projection Chamber (TPC) filled with 40Ar and installed at Laboratori Nazionali del Gran Sasso (LNGS). In 2018, the DarkSide Collaboration has performed three different types of analysis. The so-called high-mass analysis into the range between ∼ 10 GeV and ∼ 1000 GeV is discussed under the hypothesis of scattering between ∗ ( )OnbehalfofP.Agnes,I.F.M.Albuquerque,A.K.Alton,M.Ave,H.O.Back, G. Batignani, K. Biery, V. Bocci, G. Bonfini, W. M. Bonivento, B. Bottino, S. Bussino, M. Cadeddu, M. Cadoni, F. Calaprice, A. Caminata, N. Canci, A. Candela, M. Caravati, M. Cariello, M. Carlini, M. Carpinelli, S. Catalanotti, V. Cataudella, P. Cavalcante, S. Cavuoti, A. Chepurnov, C. Cical`o, A. G. Cocco, G. Covone, D. D’Angelo, S. Davini, A. De Candia, S.DeCecco,M.DeDeo,G.DeFilippis,G.DeRosa,A.V.Derbin,A.Devoto,F.DiEusanio, M. D’Incecco, G. Di Pietro, C. Dionisi, M. Downing, D. D’Urso, E. Edkins, A. Empl, G. Fiorillo, K. Fomenko, D. -
35. Particle Detectors for Non-Accelerator Physics
1 35. Particle Detectors for Non-Accelerator Physics 35. Particle Detectors for Non-Accelerator Physics 35.1 Introduction . 1 35.2 High-energy cosmic-ray hadron and gamma-ray detectors . 2 35.2.1 Atmospheric fluorescence detectors . 2 35.2.2 Atmospheric Cherenkov telescopes for high-energy gamma ray astronomy . 5 35.3 Large neutrino detectors . 8 35.3.1 Deep liquid detectors for rare processes . 8 35.3.2 Neutrino telescopes . 12 35.3.3 Radio emission from (ultra-)high energy particle showers . 20 35.4 Large time-projection chambers for rare event detection . 27 35.4.1 Dark matter and other low energy signals . 28 35.4.2 0νββ Decay . 31 35.5 Sub-Kelvin detectors . 32 35.5.1 Equilibrium thermal detectors . 32 35.5.2 Nonequilibrium Detectors . 34 35.6 Low-radioactivity background techniques . 36 35.6.1 Defining the problem . 37 35.6.2 Environmental radioactivity . 37 35.6.3 Radioactive impurities in detector and shielding components . 39 35.6.4 Radon and its progeny . 40 35.6.5 Cosmic rays . 41 35.6.6 Neutrons . 42 35.1 Introduction Non-accelerator experiments have become increasingly important in particle physics. These include cosmic ray experiments (with surface, space and underground detectors), neutrino oscilla- tion measurements with solar and atmospheric neutrinos in underground laboratories, searches for neutrino-less double beta decays and dark matter candidates again in underground laboratories, and searches for more exotic phenomena. The detectors are in the majority of the cases differ- ent from those used at accelerators. Even when the detectors are based on the same physics (e. -
Search for WIMP Dark Matter with the Dual Phase Liquid Argon Detector Darkside-20K
Contribution Prospectives 2020 Search for WIMP dark matter with the dual phase liquid argon detector DarkSide-20k Principal Author: Name: Fabrice Hubaut / Pascal Pralavorio Institution: CPPM Email: [email protected] / [email protected] Phone: 04 91 82 72 51 Co-authors: (names and institutions) - Pierre Barrillon, CPPM - José Busto, CPPM - Olivier Dadoun, LPNHE - Davide Franco, APC - Claudio Giganti, LPNHE - Christian Morel, CPPM - Alessandra Tonazzo, APC Supporters: (names and institutions) people supporting the scientific/technical content of this contribution for the next decade - Yann Coadou, CPPM - Laurent Lellouch, CPT - Jaime Dawson, APC - Steve Muanza, CPPM - Cristinel Diaconu, CPPM - Emmanuel Nezri, LAM - Marie-Hélène Genest, LPSC - Thomas Patzak, APC - Marine Kuna, LPSC - Claude Vallée, CPPM - Bertrand Laforge, LPNHE - Isabelle Wingerter-Seez, LAPP - Julien Lavalle, LUPM Abstract : Dark Matter is one of the main puzzles in fundamental physics and Weakly Interacting Massive Particles (WIMP) are among the best-motivated candidates. As of today, the most sensitive experimental technique to discover WIMPs in the mass range from 2 GeV to 10 TeV is the dual phase TPC filled with ultra-pure argon or xenon. This contribution discusses the potentiality of the next generation of Liquid Argon TPC (DarkSide-20k to be run at Gran Sasso from 2023) in exploring further this mass range. The innovative design of DarkSide-20k offers a high discovery potential, both at low mass using the ionization electron signal as demonstrated by the world-leading result of DarkSide-50, and at high mass, benefiting from the intrinsic pulse shape discrimination power of scintillation signal in liquid argon to reject electronic recoils. -
An Improved Design of the Readout Base Board of the Photomultiplier Tube for Future Pandax Dark Matter Experiments
Prepared for submission to JINST An improved design of the readout base board of the photomultiplier tube for future PandaX dark matter experiments Qibin Zheng,0,2 Yanlin Huang,0 Di Huang,1 Jianglai Liu,1,3 Xiangxiang Ren,4 Anqing Wang,4 Meng Wang,4 Jijun Yang,1 Binbin Yan,1 Yong Yang1 0Institute of Biomedical Engineering, University of Shanghai for Science and Technology, Shanghai 200093, China 1INPAC, Department of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai Laboratory for Particle Physics and Cosmology, Shanghai 200240, China 2Terahertz Technology Innovation Research Institute, University of Shanghai for Science and Technology, Shanghai 200093, China 3Tsung-Dao Lee Institute, Shanghai Jiaotong University, Shanghai, 200240, China 4School of Physics and Key Laboratory of Particle Physics and ParticleIrradiation (MOE), Shandong University, Jinan 250100, China E-mail: [email protected] Abstract: The PandaX project consists of a series of xenon-based experiments that are used to search for dark matter (DM) particles and to study the fundamental properties of neutrinos. The next DM experiment PandaX-4T will be using 4 ton liquid xenon in the sensitive volume, which is nearly a factor of seven larger than that of the previous experiment PandaX-II. Due to the increasing target mass, the sensitivity of searching for both DM and neutrinoless double-beta decay (0aVV) signals in the same detector will be significantly improved. However, the typical energy of interest for 0aVV signals is at the MeV scale, which is much higher than that of most popular DM signals. In the baseline readout scheme of the photomultiplier tubes (PMTs), the dynamic range is very limited.