The Low-Radioactivity Underground Argon Workshop a Workshop Synopsis Thomas Alexander1, Henning O
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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 -
European Astroparticle Physics Strategy 2017-2026 Astroparticle Physics European Consortium
European Astroparticle Physics Strategy 2017-2026 Astroparticle Physics European Consortium August 2017 European Astroparticle Physics Strategy 2017-2026 www.appec.org Executive Summary Astroparticle physics is the fascinating field of research long-standing mysteries such as the true nature of Dark at the intersection of astronomy, particle physics and Matter and Dark Energy, the intricacies of neutrinos cosmology. It simultaneously addresses challenging and the occurrence (or non-occurrence) of proton questions relating to the micro-cosmos (the world decay. of elementary particles and their fundamental interactions) and the macro-cosmos (the world of The field of astroparticle physics has quickly celestial objects and their evolution) and, as a result, established itself as an extremely successful endeavour. is well-placed to advance our understanding of the Since 2001 four Nobel Prizes (2002, 2006, 2011 and Universe beyond the Standard Model of particle physics 2015) have been awarded to astroparticle physics and and the Big Bang Model of cosmology. the recent – revolutionary – first direct detections of gravitational waves is literally opening an entirely new One of its paths is targeted at a better understanding and exhilarating window onto our Universe. We look of cataclysmic events such as: supernovas – the titanic forward to an equally exciting and productive future. explosions marking the final evolutionary stage of massive stars; mergers of multi-solar-mass black-hole Many of the next generation of astroparticle physics or neutron-star binaries; and, most compelling of all, research infrastructures require substantial capital the violent birth and subsequent evolution of our infant investment and, for Europe to remain competitive Universe. -
Light Dark Matter in a Minimal Extension with Two Additional Real Singlets
PHYSICAL REVIEW D 103, 015010 (2021) Light dark matter in a minimal extension with two additional real singlets Markos Maniatis * Centro de Ciencias Exactas and Departamento de Ciencias Básicas, UBB, Avenida Andres Bello 720, 3780000 Chillán, Chile (Received 24 August 2020; accepted 12 December 2020; published 8 January 2021) The direct searches for heavy scalar dark matter with a mass of order 100 GeV are much more sensitive than for light dark matter of order 1 GeV. The question arises whether dark matter could be light and has escaped detection so far. We study a simple extension of the Standard Model with two additional real singlets. We show that this simple extension may provide the observed relic dark matter density, does neither disturb big bang nucleosynthesis nor the cosmic microwave background radiation observations, and fulfills the conditions of clumping behavior for different sizes of Galaxies. The potential of one Standard Model–like Higgs-boson doublet and the two singlets gives rise to a changed Higgs phenomenology, in particular, an enhanced invisible Higgs-boson decay rate is expected, detectable by missing transversal momentum searches at the ATLAS and CMS experiments at CERN. DOI: 10.1103/PhysRevD.103.015010 I. INTRODUCTION collisions. In particular, in this way a DM candidate may enhance the invisible decay rate of a SM-like Higgs boson. Recently it has been reported [1] that the NGC1052–DF2 Note that in the SM the only invisible decay channel of galaxy with a stellar mass of approximately 2 × 108 solar the Higgs boson (h) is via two electroweak Z bosons masses has a rotational movement in accordance with its which subsequently decay into pairs of neutrinos (ν), that observed mass. -
Dark Matter Direct Detection with Edelweiss-II
Dark matter direct detection with Edelweiss-II Eric Armengaud - CEA / IRFU Blois 2008 http://edelweiss2.in2p3.fr/ 1 Direct detection of dark matter : principles . A well-identified science goal: Detect the nuclear recoil of local WIMPs inside some material Target the electroweak interaction scale, m ~ GeV-TeV At least 3 strategies: Search for a global recoil spectrum V(Earth/Sun): Search for a - small - annual modulation V(Sun/Wimp gaz): Search for a - large - forward/backward asymetry Remove backgrounds!!! Go deep underground Use several passive shields Develop smart detectors to identify the remaining radioactivity interactions 2 Direct detection of dark matter . A well-identified science goal: Detect the nuclear recoil of local WIMPs inside some material Target the electroweak interaction scale, m ~ GeV-TeV At least 3 strategies: Search for a global recoil spectrum • Cryogenic bolometers: CDMS, CRESST, EDELWEISS… • Liquid noble elements: XENON, LUX, ZEPLIN, WARP, ArDM… • Superheated liquids: COUPP, PICASSO, SIMPLE… • Solid scintillator (DAMA, KIMS), low- threshold Ge (TEXONO), gaz detector (DRIFT)… A very active field with both R&D and large-scale setups 3 The XENON10 experiment • Quite easily scalable, « high » temperatures • First scintillation pulse (S1) + Second pulse due to e- extraction to the gaz (S2) ⇒ Nuclear recoil discrimination - especially @ low E • Position measurements ⇒ Fiducial cut (~5kg) • Low-energy threshold + Xe mass ⇒ sensitivity to low-mass Wimps Electronic recoils Nuclear recoil region But : not background-free -
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 -
12 Natural Isotopes of Elements Other Than H, C, O
12 NATURAL ISOTOPES OF ELEMENTS OTHER THAN H, C, O In this chapter we are dealing with the less common applications of natural isotopes. Our discussions will be restricted to their origin and isotopic abundances and the main characteristics. Only brief indications are given about possible applications. More details are presented in the other volumes of this series. A few isotopes are mentioned only briefly, as they are of little relevance to water studies. Based on their half-life, the isotopes concerned can be subdivided: 1) stable isotopes of some elements (He, Li, B, N, S, Cl), of which the abundance variations point to certain geochemical and hydrogeological processes, and which can be applied as tracers in the hydrological systems, 2) radioactive isotopes with half-lives exceeding the age of the universe (232Th, 235U, 238U), 3) radioactive isotopes with shorter half-lives, mainly daughter nuclides of the previous catagory of isotopes, 4) radioactive isotopes with shorter half-lives that are of cosmogenic origin, i.e. that are being produced in the atmosphere by interactions of cosmic radiation particles with atmospheric molecules (7Be, 10Be, 26Al, 32Si, 36Cl, 36Ar, 39Ar, 81Kr, 85Kr, 129I) (Lal and Peters, 1967). The isotopes can also be distinguished by their chemical characteristics: 1) the isotopes of noble gases (He, Ar, Kr) play an important role, because of their solubility in water and because of their chemically inert and thus conservative character. Table 12.1 gives the solubility values in water (data from Benson and Krause, 1976); the table also contains the atmospheric concentrations (Andrews, 1992: error in his Eq.4, where Ti/(T1) should read (Ti/T)1); 2) another category consists of the isotopes of elements that are only slightly soluble and have very low concentrations in water under moderate conditions (Be, Al). -
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. -
Jianglai Liu Shanghai Jiao Tong University
Jianglai Liu Shanghai Jiao Tong University Jianglai Liu Pheno 2017 1 If DM particles have non-gravitational interaction with normal matter, can be detected in “laboratories”. DM DM Collider Search Indirect Search ? SM SM Direct Search Pheno 2017 Jianglai Liu Pheno 2017 2 Galactic halo . The solar system is cycling the center of galaxy with on average 220 km/s speed (annual modulation in earth movement) . DM local density around us: 0.3(0.1) GeV/cm3 Astrophys. J. 756:89 Inclusion of new LAMOST survey data: 0.32(0.02), arXiv:1604.01216 Jianglai Liu Pheno 2017 3 1973: discovery of neutral current Gargamelle detector in CERN neutrino beam Dieter Haidt, CERN Courier Oct 2004: “The searches for neutral currents in previous neutrino experiments resulted in discouragingly low limits (@1968), and it was somehow commonly concluded that no weak neutral currents existed.” leptonic NC hadronic NC v beam Jianglai Liu Pheno 2017 4 Direct detection A = m2/m1 . DM: velocity ~1/1500 c, mass ~100 GeV, KE ~ 20 keV . Nuclear recoil (NR, “hadronic”): recoiling energy ~10 keV . Electron recoil (ER, “leptonic”): 10-4 suppression in energy, very difficult to detect New ideas exist, e.g. Hochberg, Zhao, and Zurek, PRL 116, 011301 Jianglai Liu Pheno 2017 5 Elastic recoil spectrum . Energy threshold mass DM . SI: coherent scattering on all nucleons (A2 Ge Xe enhancement) . Note, spin-dependent Si effect can be viewed as scattering with outer unpaired nucleon. No luxury of A2 enhancement Gaitskell, Annu. Rev. Nucl. Part. Sci. 2004 Jianglai Liu Pheno 2017 6 Neutrino “floor” Goodman & Witten Ideas do exist Phys. -
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. -
DARWIN: Dark Matter WIMP Search with Noble Liquids
DARWIN: dark matter WIMP search with noble liquids Laura Baudis∗† Physik Institut, University of Zurich E-mail: [email protected] DARWIN (DARk matter WImp search with Noble liquids) is an R&D and design study towards the realization of a multi-ton scale dark matter search facility in Europe, based on the liquid argon and liquid xenon time projection chamber techniques. Approved by ASPERA in late 2009, DAR- WIN brings together several European and US groups working on the existing ArDM, XENON and WARP experiments with the goal of providing a technical design report for the facility by early 2013. DARWIN will be designed to probe the spin-independent WIMP-nucleon cross sec- tion region below 10−47cm2 and to provide a high-statistics measurement of WIMP interactions in case of a positive detection in the intervening years. After a brief introduction, the DARWIN goals, components, as well as its expected physics reach will be presented. arXiv:1012.4764v1 [astro-ph.IM] 21 Dec 2010 Identification of Dark Matter 2010-IDM2010 July 26-30, 2010 Montpellier France ∗Speaker. †DARWIN Project Coordinator; on behalf of the DARWIN consortium. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/ DARWIN: dark matter WIMP search with noble liquids Laura Baudis 1. Introduction One of the most exciting topics in physics today is the nature of Dark Matter in the Universe. Although indirect evidence for cold dark matter is well established, its true nature is not yet known. The most promising explanation is Weakly Interacting Massive Particles (WIMPs), for they would naturally lead to the observed abundance and they arise in many of the potential extensions of the Standard Model of particle physics. -
First Results of the EDELWEISS-II Direct Dark Matter Search Experiment
First results of the EDELWEISS-II Direct Dark Matter search experiment. • Dark Matter enigma • EDELWEISS-II experiment • Ge-NTD Data analysis and interpretation Silvia SCORZA Radioactive background understanding Université Claude Bernard- Institut de Physique nucléaire de Lyon WIMP search • New ID-detectors First results CEA-Saclay IRFU + IRAMIS (FRANCE), CNRS/Neel Grenoble (FRANCE), • Perspectives CNRS/IN2P3/CSNSM Orsay (FRANCE), CNRS/IN2P3/IPNL Lyon (FRANCE), CNRS-CEA/Laboratoire Souterrain de Modane (FRANCE), JINR Dubna (RUSSIA), Karlsruhe Institute of Technology (GERMANY), OXFORD University (UK) DM search motivations CDM present at all scales in the Universe… ΩB=0.044±0.004 ΩM=0.27±0.04 Ωtot=1.02±0.02 Ω =0.22±0.02 Galaxy DM Clusters Cosmology DM searches justified : direct (DM elastic scattering off target nuclei) and indirect (DM annihilation signal in galactic halo) → not enough to identify DM nature … and soon, maybe also at LHC (natural candidates arise from New Physics scenarii, such as SUSY) → no direct cosmological test (relic abundance or stability)2 WIMP dark matter (particles) WEAKLY INTERACTING MASSIVE PARTICLE Neutral and weakly interactions: neither strong nor electromagnetic → DM does not collapse to the center of the galaxy Cold enough (non-relativistic) at decoupling era Stable at cosmological scale Relic present today → explanation of Ωm 3 SUSY naturally “predicts” WIMP DM R-parity conserved → LSP stable (particle : R=+1; sparticle : R=-1) NEUTRALINO Spin-Independent Diagrams -11 -5 Interaction cross section: -
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.