Latest Results from DEAP-3600 at SNOLAB
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Parallel Sessions
Identification of Dark Matter July 23-27, 2012 9th International Conference Chicago, IL http://kicp-workshops.uchicago.edu/IDM2012/ PARALLEL SESSIONS http://kicp.uchicago.edu/ http://www.nsf.gov/ http://www.uchicago.edu/ http://www.fnal.gov/ International Advisory Committee Daniel Akerib Elena Aprile Rita Bernabei Case Western Reserve University, Columbia University, USA Universita degli Studi di Roma, Italy Cleveland, USA Gianfranco Bertone Joakim Edsjo Katherine Freese University of Amsterdam Oskar Klein Centre / Stockholm University of Michigan, USA University Richard Gaitskell Gilles Gerbier Anne Green Brown University, USA IRFU/ CEA Saclay, France University of Nottingham, UK Karsten Jedamzik Xiangdong Ji Lawrence Krauss Universite de Montpellier, France University of Maryland, USA Arizona State University, USA Vitaly Kudryavtsev Reina Maruyama Leszek Roszkowski University of Sheffield University of Wisconsin-Madison University of Sheffield, UK Bernard Sadoulet Pierre Salati Daniel Santos University of California, Berkeley, USA University of California, Berkeley, USA LPSC/UJF/CNRS Pierre Sikivie Daniel Snowden-Ifft Neil Spooner University of Florida, USA Occidental College University of Sheffield, UK Max Tegmark Karl van Bibber Kavli Institute for Astrophysics & Space Naval Postgraduate School Monterey, Research at MIT, USA USA Local Organizing Committee Daniel Bauer Matthew Buckley Juan Collar Fermi National Accelerator Laboratory Fermi National Accelerator Laboratory Kavli Institute for Cosmological Physics Scott Dodelson Aimee -
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 -
The PICASSO Dark Matter Physics Program at SNOLAB
33RD INTERNATIONAL COSMIC RAY CONFERENCE,RIO DE JANEIRO 2013 THE ASTROPARTICLE PHYSICS CONFERENCE The PICASSO Dark Matter Physics Program at SNOLAB A.J. NOBLE1 FOR THE PICASSO COLLABORATION: S. ARCHAMBAULT2, E. BEHNKE3, P. BHATTACHARJEE4, S. BHATTACHARYA4, X. DAI1, M. DAS4, A. DAVOUR1, F. DEBRIS2, N. DHUNGANA5, J. FARINE5, S. GAGNEBIN6, G. GIROUX2, E. GRACE3, C. M. JACKSON2, A. KAMAHA1, C. KRAUSS6, S. KUMARATUNGA2, M. LAFRENIRE2, M. LAURIN2, I. LAWSON7, L. LESSARD2, I. LEVINE3, C. LEVY1, R. P. MACDONALD6, D. MARLISOV6, J.-P. MARTIN2, P. MITRA6, A. J. NOBLE1, M.-C. PIRO2, R. PODVIYANUK5, S. POSPISIL8, S. SAHA4, O. SCALLON2, S. SETH4, N. STARINSKI2, I. STEKL8, U. WICHOSKI5, T. XIE1, V. ZACEK2 1 Department of Physics, Queens University, Kingston, K7L 3N6, Canada 2 Departement´ de Physique, Universite´ de Montreal,´ Montreal,´ H3C 3J7, Canada 3 Department of Physics & Astronomy, Indiana University South Bend, South Bend, IN 46634, USA 4 Saha Institute of Nuclear Physics, Centre for AstroParticle Physics (CAPP), Kolkata, 700064, India 5 Department of Physics, Laurentian University, Sudbury, P3E 2C6, Canada 6 Department of Physics, University of Alberta, Edmonton, T6G 2G7, Canada 7 SNOLAB, 1039 Regional Road 24, Lively ON, P3Y 1N2, Canada 8 Institute of Experimental and Applied Physics, Czech Technical University in Prague, Prague, Cz-12800, Czech Republic [email protected] Abstract: PICASSO is a dark matter search experiment currently operational at the SNOLAB International Facility for Astroparticle Physics, located 2 km underground in Sudbury, Canada. PICASSO is based on the superheated bubble technique. With good control of radiological backgrounds and a detector design that stabilizes the superheated liquid even when very close to the critical temperature, PICASSO has achieved very low nuclear recoil thresholds. -
Dark Matter the Invisible Material
Dark matter The invisible material Our universe holds everything we know and everything we are still figuring out. For years, physicists around the world have studied our universe to better understand its nature and its future. They have found that we only understand about 4% of the matter and energy in our universe (including stars, planets, and hot gas). The other 96% is invisible to us and 23% of this invisible material is named dark matter. If dark matter is invisible, how do we know it exists? To answer this, we go back to the 1930s when physicist Fritz Zwicky Galaxy cluster* coined the term dark matter while studying galaxy clusters. Galaxy clusters have up to thousands of galaxies (like our Milky Way for example) held together by gravity. When Dr. Zwicky calculated the total visible mass of galaxies in the Coma cluster, he found that it was not enough to create the gravity needed to hold the cluster together (mass causes gravity). He concluded that there must be an invisible material causing the extra gravity: dark matter. Now fast forward to the 1970s when Vera Rubin studied galaxy rotation curves. According to Newton’s laws, when objects rotate around a common centre, the ones furthest from the centre move more slowly Gravitational lens – than those near it. Otherwise, the furthest objects would fly off. Dr. Rubin galaxies look long found that stars in galaxies do not follow this rule. In fact, stars at the and distorted* outer edges of galaxies move at about the same rate as those near the centre. -
Dark Matter and the Early Universe: a Review Arxiv:2104.11488V1 [Hep-Ph
Dark matter and the early Universe: a review A. Arbey and F. Mahmoudi Univ Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, Institut de Physique des 2 Infinis de Lyon, UMR 5822, 69622 Villeurbanne, France Theoretical Physics Department, CERN, CH-1211 Geneva 23, Switzerland Institut Universitaire de France, 103 boulevard Saint-Michel, 75005 Paris, France Abstract Dark matter represents currently an outstanding problem in both cosmology and particle physics. In this review we discuss the possible explanations for dark matter and the experimental observables which can eventually lead to the discovery of dark matter and its nature, and demonstrate the close interplay between the cosmological properties of the early Universe and the observables used to constrain dark matter models in the context of new physics beyond the Standard Model. arXiv:2104.11488v1 [hep-ph] 23 Apr 2021 1 Contents 1 Introduction 3 2 Standard Cosmological Model 3 2.1 Friedmann-Lema^ıtre-Robertson-Walker model . 4 2.2 A quick story of the Universe . 5 2.3 Big-Bang nucleosynthesis . 8 3 Dark matter(s) 9 3.1 Observational evidences . 9 3.1.1 Galaxies . 9 3.1.2 Galaxy clusters . 10 3.1.3 Large and cosmological scales . 12 3.2 Generic types of dark matter . 14 4 Beyond the standard cosmological model 16 4.1 Dark energy . 17 4.2 Inflation and reheating . 19 4.3 Other models . 20 4.4 Phase transitions . 21 5 Dark matter in particle physics 21 5.1 Dark matter and new physics . 22 5.1.1 Thermal relics . 22 5.1.2 Non-thermal relics . -
SNOLAB Construction Status and Experimental Program
M. Chen Queen’s University SNOLAB Construction Status and Experimental Program SNOLAB located 2 km underground in an active nickel mine near Sudbury, Canada it’s an expansion of the underground facility on the same level as the SNO experiment Surface Facility Excavation Status (Today) -Blasting for Phase I Excavation complete. - Shotcrete walls complete - Concrete floors almost finished. BLADDER ROOM BLADDER ROOM SHOWER ROOM SHOWER ROOM DOUBLE TRACKS DOUBLE TRACKS LADDER LABS LADDER LABS CUBE HALL CUBE HALL Phase I - Cube Hall (18x15x15 m) - Ladder Labs (~7mx~7mx60m) Utility Area - Chiller, generator, Lab Entrance water systems Existing SNO - Personnel Areas Facilities -Material Handling -SNO Cavern (30m x 22m dia) - Utility & Control Rms SNOLAB Workshop V, 21 August 2006 Phase II -Cryopit Phase I (15m x15m dia) - Cube Hall (18x15x15 m) - Ladder Labs (~7mx~7mx60m) Utility Area - Chiller, generator, Lab Entrance water systems Existing SNO - Personnel Areas Facilities -Material Handling -SNO Cavern (30m x 22m dia) - Utility & Control Rms Rectangular Hall Control Rm Utility Drift Staging Area Rectangular Hall 60’L x 50’W 50’ (shoulder) 65’ (back) SNOLAB Workshop IV, 15 Aug 2005 Ladder Labs Wide Drift Electrical, 20’x12’ AHUs (19’ to back) Wide Drift 25’x17’ (25’ to back) Access Drift 15’x10’ (15’ to back) Chemistry Lab SNOLAB Workshop IV, 15 Aug 2005 SNOLAB Experiments z Some 20 projects submitted Letters of Interest in locating at SNOLAB. Of these, 10 have been encouraged by the Experiment Advisory Committee as being both scientifically important and particularly suited to the SNOLAB location. z The experimental physics program includes − Neutrinos: Low energy solar neutrinos, geo-neutrinos, reactor neutrinos, supernova neutrino detection z Tests of neutrino properties, precision measurements of solar neutrinos, radiogenic heat generation in the earth, stellar evolution. -
Recommended Conventions for Reporting Results from Direct Dark Matter Searches
Recommended conventions for reporting results from direct dark matter searches D. Baxter1, I. M. Bloch2, E. Bodnia3, X. Chen4,5, J. Conrad6, P. Di Gangi7, J.E.Y. Dobson8, D. Durnford9, S. J. Haselschwardt10, A. Kaboth11,12, R. F. Lang13, Q. Lin14, W. H. Lippincott3, J. Liu4,5,15, A. Manalaysay10, C. McCabe16, K. D. Mor˚a17, D. Naim18, R. Neilson19, I. Olcina10,20, M.-C. Piro9, M. Selvi7, B. von Krosigk21, S. Westerdale22, Y. Yang4, and N. Zhou4 1Kavli Institute for Cosmological Physics and Enrico Fermi Institute, University of Chicago, Chicago, IL 60637 USA 2School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel 3University of California, Santa Barbara, Department of Physics, Santa Barbara, CA 93106, USA 4INPAC and School of Physics and Astronomy, Shanghai Jiao Tong University, MOE Key Lab for Particle Physics, Astrophysics and Cosmology, Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai 200240, China 5Shanghai Jiao Tong University Sichuan Research Institute, Chengdu 610213, China 6Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm SE-10691, Sweden 7Department of Physics and Astronomy, University of Bologna and INFN-Bologna, 40126 Bologna, Italy 8University College London, Department of Physics and Astronomy, London WC1E 6BT, UK 9Department of Physics, University of Alberta, Edmonton, Alberta, T6G 2R3, Canada 10Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA 94720, USA 11STFC Rutherford Appleton Laboratory (RAL), Didcot, OX11 0QX, UK 12Royal Holloway, -
Ultra-Weak Gravitational Field Theory Daniel Korenblum
Ultra-weak gravitational field theory Daniel Korenblum To cite this version: Daniel Korenblum. Ultra-weak gravitational field theory. 2018. hal-01888978 HAL Id: hal-01888978 https://hal.archives-ouvertes.fr/hal-01888978 Preprint submitted on 5 Oct 2018 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Ultra-weak gravitational field theory Daniel KORENBLUM [email protected] April 2018 Abstract The standard model of the Big Bang cosmology model ΛCDM 1 considers that more than 95 % of the matter of the Universe consists of particles and energy of unknown forms. It is likely that General Relativity (GR)2, which is not a quantum theory of gravitation, needs to be revised in order to free the cosmological model of dark matter and dark energy. The purpose of this document, whose approach is to hypothesize the existence of the graviton, is to enrich the GR to make it consistent with astronomical observations and the hypothesis of a fully baryonic Universe while maintaining the formalism at the origin of its success. The proposed new model is based on the quantum character of the gravitational field. This non-intrusive approach offers a privileged theoretical framework for probing the properties of the regime of ultra-weak gravitational fields in which the large structures of the Universe are im- mersed. -
Probing the Nature of Dark Matter in the Universe
PROBING THE NATURE OF DARK MATTER IN THE UNIVERSE A Thesis Submitted For The Degree Of Doctor Of Philosophy In The Faculty Of Science by Abir Sarkar Under the supervision of Prof. Shiv K Sethi Raman Research Institute Joint Astronomy Programme (JAP) Department of Physics Indian Institute of Science BANGALORE - 560012 JULY, 2017 c Abir Sarkar JULY 2017 All rights reserved Declaration I, Abir Sarkar, hereby declare that the work presented in this doctoral thesis titled `Probing The Nature of Dark Matter in the Universe', is entirely original. This work has been carried out by me under the supervision of Prof. Shiv K Sethi at the Department of Astronomy and Astrophysics, Raman Research Institute under the Joint Astronomy Programme (JAP) of the Department of Physics, Indian Institute of Science. I further declare that this has not formed the basis for the award of any degree, diploma, membership, associateship or similar title of any university or institution. Department of Physics Abir Sarkar Indian Institute of Science Date : Bangalore, 560012 INDIA TO My family, without whose support this work could not be done Acknowledgements First and foremost I would like to thank my supervisor Prof. Shiv K Sethi in Raman Research Institute(RRI). He has always spent substantial time whenever I have needed for any academic discussions. I am thankful for his inspirations and ideas to make my Ph.D. experience produc- tive and stimulating. I am also grateful to our collaborator Prof. Subinoy Das of Indian Institute of Astrophysics, Bangalore, India. I am thankful to him for his insightful comments not only for our publica- tions but also for the thesis. -
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. -
Search for Dark Matter with Liquid Argon and Pulse Shape Discrimination: Results from DEAP-1 and Status of DEAP-3600
Search for Dark Matter with Liquid Argon and Pulse Shape Discrimination: Results from DEAP-1 and Status of DEAP-3600 P. Gorel, for the DEAP Collaboration Centre for Particle Physics, University of Alberta, Edmonton, T6G2E1, CANADA In the last decade, Direct Dark Matter searches has become a very active research program, spawning dozens of projects world wide and leading to contradictory results. It is on this stage that the Dark matter Experiment with liquid Argon and Pulse shape discrimination (DEAP) is about to enter. With a 3600 kg liquid argon target and a 1000 kg fiducial mass, it is designed to run background free during 3 years, reaching an unprecedented sensitivity of 10−46 cm2 for a WIMP mass of 100 GeV. In order to achieve this impressive feat, the collaboration followed a two-pronged approach: a careful selection of every material entering the construction of the detector in order to suppress the backgrounds, and optimum use of the pulse shape discrimination (PSD) technique to separate the nuclear recoils from the electronic recoils. Using the experience acquired ffrom the 7 kg-prototype DEAP-1, a 3600 kg detector is being completed at SNOLAB (Sudbury, CANADA) and is expected to start taking data in mid-2014. 1 Dark matter detection using liquid argon For decades, liquid argon (LAr) has been a candidate of choice for large scintillating detectors. It is easy to purify and boasts a high light yield, which makes it ideal for low background, low threshold experiments. The scintillating process involves the creation of excimer, either directly or through ionization/recombination.