DOCSLIB.ORG

Detection of Dark Matter at Neutrino Detectors Nirmal Raj TRIUMF

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Detection of Dark Matter at Neutrino Detectors Nirmal Raj TRIUMF Direct(ional) Detection of Dark Matter at Neutrino Detectors Nirmal Raj TRIUMF with Joe Bramante, Ben Broerman (PICO), Jason Kumar, Rafael Lang (XENON1T), Maxim Pospelov and DEAP-3600 analysis: Walter Bonivento, Shivam Garg, Michela Lai, Ashlea Kemp, Shawn Westerdale + others Neutrino Theory Mini-Workshop, 23 Sep 2020 Structure of the talk uncover direct detection regions 1 well-loved paradigms lots of room to explore on just this space! simple new search strategies — go to optically thick limit 2 enlist neutrino detectors! 3 measure DM velocity spectrum CMB BULLET CLUSTER Dark reality v LARGE SCALE STRUCTURE r GALACTIC ROTATION CMB BULLET CLUSTER 3 Direct detection status after 1000 kg-yr exposure cross section for dark matter cross for dark section matter nucleons hitting (cm2) dark matter mass 4 (GeV) Bird’s-eye view 10-11 10-21 10-31 ? ? 10-41 6 10 14 18 cross section for dark matter cross for dark section matter nucleons hitting 0.01 100.00 10 10 10 10 (cm2) dark matter mass 5 (GeV) All the Earth-based constraints 10-11 WEARY SKYLAB -21 RARE 10 XQC IMP CDMS-I DAMA X1T -31 CRESST surface 10 POWERLESS CRESST-III XENON1T Drawn in 1999! -41 10 GHOSTLY 6 10 14 18 cross section for dark matter cross for dark section matter nucleons hitting 0.01 100.00 10 10 10 10 (cm2) dark matter mass 6 (GeV) Hunting even rarer dark matter 10-11 WEARY SKYLAB -21 RARE 10 XQC IMP CDMS-I DAMA X1T -31 CRESST surface 10 POWERLESS CRESST-III XENON1T Drawn in 1999! -41 10 GHOSTLY 6 10 14 18 cross section for dark matter cross for dark section matter nucleons hitting 0.01 100.00 10 10 10 10 Is dark matter here? (cm2) dark matter mass 7 (GeV) Theoretical appeal Super-heavy states appear in theories α of grand unification of forces. 3 α2 α 1 µ Can make them in early universe: * Hawking radiation from primordial black holes Hooper, Krnjaic, McDermott (2019) * Gravitationally @ final stages of inflation Chung, Crotty, Kolb, Riotto (2001), Harigaya, Lin, Lou (2016) * Pre-heating: parametric resonance —> rapid decay of inflaton Giudice, Peloso, Riotto, Tkachev (1999), Bai, Korwar, Orlofsky (2020) * Thermally! Kim, Kuflik (2019) 8 Heavy, strong, stable: recent wave Electroweak symmetric monopoles Bai, Korwar, Orlofsky 2005.00503 Electroweak symmetric solitons Bai, Jain, Ponton 1906.10739 Charged primordial black holes Lehmann, Johnson, Profumo, Schwemberger Asymmetric dark matter nuggets 1906.06348 Coskuner, Grabowska, Knapen, Zurek 1812.07573 Dark blobs Grabowska, Melia, Rajendran 1807.03788 Colored relics Gross, Mitridate, Redi, Smirnov, Strumia Heavy dark baryons 1811.08418 Davoudiasl, Mohlabeng 1809.07768 Heavy dark skyrmions Berezowski, Dick Why now? Sep 2019 Can detect them now! 9 Today’s dark matter detectors DAMA 1999 10 cm (Q1) Can current DM detectors hunt the rarest huntable? max mDM 10 cm = 1016 GeV B. Broerman, J. Bramante, R. Lang, N. Raj Phys.Rev.D. (2018) 100 cm 130 cm 50 cm XENON1T/ DEAP-3600 PICO-40L LUX/ PANDAX-II 10 Multiscatter signatures essential # scatters per transit = � x target number density x path length B. Broerman, J. Bramante, R. Lang, N. Raj Phys.Rev.D. (2018) RARE MANY SCATTERS ONE SCATTER cross section GHOSTLY dark matter mass Multiscatter signatures essential # scatters per transit = � x target number density x path length B. Broerman, J. Bramante, R. Lang, N. Raj Phys.Rev.D. (2018) RARE MANY SCATTERS ONE SCATTER cross section GHOSTLY Goodman & Witten, 1985: dark matter mass - DAMA ’99 based on this ‘multiple scatters’ signature - Not sought any more. Would double the reach of all current experiments! (Q2) Are there bigger detectors that can join the hunt? B. Broerman, J. Bramante, J. Kumar, R. Lang, M. Pospelov, N. Raj Phys.Rev.D. (2018) + BULLET CLUSTER XENON1T DEAP-3600 PICO-40L 13 recasting MAJORANA DEMONSTRATOR search for lightly ionizing particles ‘Direct Detection Limits on Heavy Dark Matter’ 2009.07909 M. Clark, R. Lang et al 14 Liquid scintillator neutrino detectors XENON1T, DEAP, PICO, … BOREXINO, SNO+, JUNO Direct detection @ liq. scint. neutrino detectors Mass sensitivity: dark matter fluxes at least 100 times greater Cross section sensitivity: Satisfy selection trigger 15 SNO+ mass reach “fiducial area” = 106 cm2 ��-�� - ���������� �� �� ����� ���� ����� � �� ) -�� � �� ���� �� ����� ���� ����� ( � � �� ���� �� χ -�� � �� � σ ������ ������ ������ ������ -�� ������ ���� ���� ���� �� ���� + + ���� + + ��� ��� - ��� �� ��� �� ��� ���� ���� ���� ���� ���� ���� ���� �χ (���) 16 SNO+ signal DM transit = 10 µs Continuous deposition of photoelectrons over transit time Collinearity may be exploited with vertex reconstruction/ timing information 17 Signal vs background windows BOREXINO, 10 µs windows dark matter signal, σnx = 10-28 cm2 (spin-independent) typical windows with dark counts 1 in 100 windows 14C x once in 10 years x x x x x 18 SNO+ cross section reach B. Broerman, J. Bramante, J. Kumar, R. Lang, M. Pospelov, N. Raj Phys.Rev.D. (2019) ��-�� ������ ��� ������� ���� -�� �� ���������� ����� �� - �� ) -�� �� � �� - � �� ( ������ ������ ������ χ -�� � �� ���� σ ���� + �� ���������� ������ ℓ -�� ��� ���������� �������� �� ������� ��� ���������� �������� ������� ��������� ��-�� ���� ���� ���� ���� ���� ���� ���� �χ (���) 19 Reconstructing dark matter velocity vector Image: Borexino 1308.0443 dark matter path PMT “hot spots” with numerous illuminations => dark matter direction & path length + timestamps => dark matter speed J. Bramante, J. Kumar, N. Raj 20 Phys Rev D (2019) VelocityTestingDetector vector dispersion resolutions uncertainties speed J. Bramante, J. Kumar, N. Raj Phys Rev D (2019) (PMT spacing/ path length) ~2 degrees, c.f. Cygnus spanning > 20 degrees VelocityTestingDetector vector dispersion resolutions uncertainties speed J. Bramante, J. Kumar, N. Raj Phys Rev D (2019) (PMT spacing/ path length) (< 1 km/s) detector timing resolution detector uncertainties tiny => smearing negligible => main limitation is statistics! (triumph of experimental progress) 22 Statistics SNO+ could potentially collect these many events J. Bramante, J. Kumar, N. Raj 23 Phys Rev D (2019) Dark astrometry reconstruct velocity vector event-by-event assemble distributions of speed and angle determine halo properties! dispersion speed escape speed anisotropies + bonus: reject backgrounds J. Bramante, J. Kumar, N. Raj 24 Phys Rev D (2019) Pinpointing mean speed galactic frame v0 = circular speed = √(2/3) dispersion speed 1400 v0 = 180 km/s 1200 v0 = 220 km/s 1000 v0 = 260 km/s 800 600 400 200 Distribution in galactic frame 0 0.0000 0.0005 0.0010 0.0015 0.0020 v/c J. Bramante, J. Kumar, N. Raj 25 Phys Rev D (2019) Pinpointing mean speed galactic frame circular speed = 220 km/s J. Bramante, J. Kumar, N. Raj 26 Phys Rev D (2019) Testing velocity anisotropies angular distribution: galactic frame m contribution SPHERICAL HARMONICS l monopole ~ 1 dipole ~ ε quadrupole ~ ε test anisotropy, ε << 1 Benchmark: => J. Bramante, J. Kumar, N. Raj 27 Phys Rev D (2019) Testing velocity anisotropies monopole coefficient dipole coefficient good angular resolution (smearing negligible) poor angular resolution (smearing significant) LESSONS: good statistics => accuracy & precision, J. Bramante, J. Kumar, N. Raj smearing => anisotropies wash out. Phys Rev D (2019) Takeaways Amazing advances in underground detection technology => - metre-scale dark matter experiments (Xenon1T, DEAP, PICO) can discover dark matter [composites, heavy baryons, nuggets, blobs, black holes, monopoles, solitons, …] near/beyond Planck mass, through dedicated multi-scatter signature search. - large-volume neutrino experiments with liquid scintillator (SNO+, JUNO) can join the dark matter “direct detection” program, probe well beyond Planck mass, determine halo properties with unprecedented precision. (dispersion speed, escape speed, velocity anisotropies) 29 THANK YOU! QUESTIONS? (Q1) Identifying multiscatterers DEAP-3600 @ SNOLAB back-of-the-envelope: waveform analysis increasing cross sec PE count t 31 (Q1) Identifying multiscatterers DM transit = 2.5 µs LUX/PANDAX/XENON1T PICO-60 single hit: Train of scintillation pulses + Track of bubbles electroluminescence pulses multi-hit: For multiplicity > 5 (>500), S2 (S1) Stereo cameras can image up to pulses merge into elongated pulses 100 bubbles (mm resolution) - Background ~ 0 (from daughter neutrons of surrounding material & coincident electron recoils) Searches ongoing… 32 (Q2) Large volume neutrino detectors? Organic liquid scintillator (SNO+, Borexino, etc.): well-suited for dark matter search! collect enough light in PMTs => in business Water Cerenkov (Super-K, SNO, etc.) unsuitable: non-relativistic scattering Liquid argon TPCs (DUNE, etc.): threshold too high 33 SNO+ scale model @ SNOLAB PMT selfie 2 km underground 34 SNO+ cross section reach: triggers Existing @ BOREXINO Proposed improvement 50 keV/ 100 ns => 50 PE /100 ns, or 42 PE/ 10 µs. 5000 PE/ 10 µs. The Scintillation Efficiency of Carbon and Hydrogen Recoils in an Organic Liquid Scintillator for Dark Matter Searches Hong, Craig, Graham, Hailey, Spooner, Tovey [Bicron scintillator (BC505)] 35 SNO+ cross section reach: triggers DM transit = 10 µs Existing @ BOREXINO Proposed improvement 50 PE /100 ns, or 5000 PE/ 10 µs. 42 PE/ 10 µs. — Enhance cross section sensitivity by ~100. 36 SNO+ cross section reach: triggers DM transit = 10 µs Existing @ BOREXINO Proposed improvement 50 PE /100 ns, or 5000 PE/ 10 µs. 42 PE/ 10 µs. Dark count rate reported by Borexino (1308.0443): Nbg = 10 PE/ 10 µs. main background — Enhance cross section sensitivity by ~100. 37 SNO+ cross
Load more

Recommended publications
  • The Gran Sasso Underground Laboratory Program
    The Gran Sasso Underground Laboratory Program Eugenio Coccia INFN Gran Sasso and University of Rome “Tor Vergata” [email protected] XXXIII International Meeting on Fundamental Physics Benasque - March 7, 2005 Underground Laboratories Boulby UK Modane France Canfranc Spain INFN Gran Sasso National Laboratory LNGSLNGS ROME QuickTime™ and a Photo - JPEG decompressor are needed to see this picture. L’AQUILA Tunnel of 10.4 km TERAMO In 1979 A. Zichichi proposed to the Parliament the project of a large underground laboratory close to the Gran Sasso highway tunnel, then under construction In 1982 the Parliament approved the construction, finished in 1987 In 1989 the first experiment, MACRO, started taking data LABORATORI NAZIONALI DEL GRAN SASSO - INFN Largest underground laboratory for astroparticle physics 1400 m rock coverage cosmic µ reduction= 10–6 (1 /m2 h) underground area: 18 000 m2 external facilities Research lines easy access • Neutrino physics 756 scientists from 25 countries Permanent staff = 66 positions (mass, oscillations, stellar physics) • Dark matter • Nuclear reactions of astrophysics interest • Gravitational waves • Geophysics • Biology LNGS Users Foreigners: 356 from 24 countries Italians: 364 Permanent Staff: 64 people Administration Public relationships support Secretariats (visa, work permissions) Outreach Environmental issues Prevention, safety, security External facilities General, safety, electrical plants Civil works Chemistry Cryogenics Mechanical shop Electronics Computing and networks Offices Assembly halls Lab
    [Show full text]
  • THE BOREXINO IMPACT in the GLOBAL ANALYSIS of NEUTRINO DATA Settore Scientifico Disciplinare FIS/04
    UNIVERSITA’ DEGLI STUDI DI MILANO DIPARTIMENTO DI FISICA SCUOLA DI DOTTORATO IN FISICA, ASTROFISICA E FISICA APPLICATA CICLO XXIV THE BOREXINO IMPACT IN THE GLOBAL ANALYSIS OF NEUTRINO DATA Settore Scientifico Disciplinare FIS/04 Tesi di Dottorato di: Alessandra Carlotta Re Tutore: Prof.ssa Emanuela Meroni Coordinatore: Prof. Marco Bersanelli Anno Accademico 2010-2011 Contents Introduction1 1 Neutrino Physics3 1.1 Neutrinos in the Standard Model . .4 1.2 Massive neutrinos . .7 1.3 Solar Neutrinos . .8 1.3.1 pp chain . .9 1.3.2 CNO chain . 13 1.3.3 The Standard Solar Model . 13 1.4 Other sources of neutrinos . 17 1.5 Neutrino Oscillation . 18 1.5.1 Vacuum oscillations . 20 1.5.2 Matter-enhanced oscillations . 22 1.5.3 The MSW effect for solar neutrinos . 26 1.6 Solar neutrino experiments . 28 1.7 Reactor neutrino experiments . 33 1.8 The global analysis of neutrino data . 34 2 The Borexino experiment 37 2.1 The LNGS underground laboratory . 38 2.2 The detector design . 40 2.3 Signal processing and Data Acquisition System . 44 2.4 Calibration and monitoring . 45 2.5 Neutrino detection in Borexino . 47 2.5.1 Neutrino scattering cross-section . 48 2.6 7Be solar neutrino . 48 2.6.1 Seasonal variations . 50 2.7 Radioactive backgrounds in Borexino . 51 I CONTENTS 2.7.1 External backgrounds . 53 2.7.2 Internal backgrounds . 54 2.8 Physics goals and achieved results . 57 2.8.1 7Be solar neutrino flux measurement . 57 2.8.2 The day-night asymmetry measurement . 58 2.8.3 8B neutrino flux measurement .
    [Show full text]
  • 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.
    [Show full text]
  • 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,
    [Show full text]
  • 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.
    [Show full text]
  • BOREXINO - Status and Calibration
    BOREXINO - Status and Calibration International Workshop on "Double Beta Decay and Neutrinos" Osaka, June 12, 2007 Christian Grieb for the Borexino Collaboration Virginia Tech Borexino Collaboration • College de France (France) • Technische Unversität München (Germany) • JINR Dubna (Russia) • Kurchatov Institute Moscow (Russia) • MPI Heidelberg (Germany) • Jagellonian University Cracow (Poland) • INFN – Milano (Italy) • INFN – Genova (Italy) • INFN – Perugia (Italy) • INFN – LNGS (Italy) • Princeton Univeristy (USA) NSF funded • Virginia Tech (USA) } Borexino Christian Grieb, Virginia Tech, June 2007 Borexino • Designed to spectroscopically measure low energy solar neutrinos, especially 7Be • Liquid Scintillator Spectrometer • ν + e - → ν’ + e -’ • Charged Current • Neutral Current Borexino Christian Grieb, Virginia Tech, June 2007 Signal in Borexino 7 +++ −−− →→→ 7 +++ ννν Be e Li e Monochromatic E ννν=862 keV Φ 9 ν 2 SSM =4.8x10 /sec/cm ννν ννν e x Expected rate (LMA) is ~35 counts/day between 0.25-0.8 MeV Borexino Christian Grieb, Virginia Tech, June 2007 Science in Borexino • Measure 7Be solar neutrinos (0.25-0.8 MeV) • Measured vs MSW-LMA predicted event rate • 1/r^2 solar signature • Study CNO and pep (~1-2 pep ev/d) neutrinos (0.8-1.3 MeV) (rejection of 11 C 8B-neutrinos cosmogenic background – proven in CTF (SuperK, SNO) hep-ex/0601035) • Geoneutrinos (10 – 30 ev/year) • Supernova Neutrinos (~120 ev from GC 7 supernova) Be neutrinos (BOREXINO) • Double beta decay with Xenon? (Phys.Rev.Lett. 72:1411,1994) • ... Borexino Christian Grieb, Virginia Tech, June 2007 Publications (since 2002) • The Nylon Scintillator Containment Vessels for the Borexino Solar Neutrino Experiment. • J. Benziger et al. Feb 2007 physics/0702162 • CNO and pep neutrino spectroscopy in Borexino: Measurement of the deep-underground production of cosmogenic C11 in an organic liquid scintillator • H.
    [Show full text]
  • Large Large-Scale Neutrino Detectors No Detectors
    LARGE-SCALE NEUTRINO DETECTORS input for the 2020 update of the European Strategy for Particle Physics from the Institute for Nuclear Research of the Russian Academy of Sciences Contact person: Prof. Leonid Kravchuk, Director, INR RAS, 60th October Anniversary prospect 7A, 117312, Moscow, Russia Tel.: +7 495 8504201 e-mail: [email protected] Abstract: We propose a multi-purpose neutrino observatory comprising two very large detectors solving different problems at the intersection of particle physics, astrophysics and Earth science. Baikal-GVD will work jointly with KM3NET and IceCube in the Global Neutrino Network, aiming at the detection and study of high-energy astrophysical neutrinos. The new Baksan neutrino telescope (NBNT) will inherit from its smaller precursor, Borexino, but will become the only large-scale neutrino detector geographically located in Europe. Thanks to the unique low-background conditions at Baksan, determined by a combination of depth and of location far from artificial nuclear reactors, it will be the best instrument in the world to measure the CNO solar neutrino flux, at the same time addressing a wide range of other problems. Moscow, December 13, 2018 Comprehensive overview Development of many areas in modern physics, astrophysics and related fields is closely related to the neutrino studies. Neutrinos may bring the key to the way the Standard Model (SM) should be extended: in fact, it is the neutrino oscillations which violate the SM conservation laws (lepton numbers of individual generations) and give the only laboratory proof of the SM incompleteness. The discovery of the oscillations in the solar neutrinos gave a bright example of the application of astrophysical results to understanding of basic properties of elementary particles.
    [Show full text]
  • 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.
    [Show full text]
  • PASAG Report
    Report of the HEPAP Particle Astrophysics Scientific Assessment Group (PASAG) 23 October 2009 Introduction and Executive Summary 1.1 Introduction The US is presently a leader in the exploration of the Cosmic Frontier. Compelling opportunities exist for dark matter search experiments, and for both ground-based and space-based dark energy investigations. In addition, two other cosmic frontier areas offer important scientific opportunities: the study of high- energy particles from space and the cosmic microwave background.” - P5 Report, 2008 May, page 4 Together with the Energy Frontier and the Intensity Frontier, the Cosmic Frontier is an essential element of the U.S. High Energy Physics (HEP) program. Scientific efforts at the Cosmic Frontier provide unique opportunities to discover physics beyond the Standard Model and directly address fundamental physics: the study of energy, matter, space, and time. Astrophysical observations strongly imply that most of the matter in the Universe is of a type that is very different from what composes us and everything we see in daily life. At the same time, well-motivated extensions to the Standard Model of particle physics, invented to solve very different sets of problems, also tend to predict the existence of relic particles from the early Universe that are excellent candidates for the mysterious dark matter. If true, the dark matter isn’t just “out there” but is also passing through us. The opportunity to detect dark matter interactions is both compelling and challenging. Investments from the previous decades have paid off: the capability is now within reach to detect directly the feeble signals of the passage of cosmic dark matter particles in ultra-low-noise underground laboratories, as well as the possibility to isolate for the first time the high-energy particle signals in the cosmos, particularly in gamma rays, that should occur when dark matter particles collide with each other in astronomical systems.
    [Show full text]
  • «Nucleus-2020»
    NRC «Kurchatov Institute» Saint Petersburg State University Joint Institute for Nuclear Research LXX INTERNATIONAL CONFERENCE «NUCLEUS-2020» NUCLEAR PHYSICS AND ELEMENTARY PARTICLE PHYSICS. NUCLEAR PHYSICS TECHNOLOGIES. BOOK OF ABSTRACTS Online part. 12 – 17 October 2020 Saint Petersburg НИЦ «Курчатовский институт» Санкт-Петербургский государственный университет Объединенный институт ядерных исследований LXX МЕЖДУНАРОДНАЯ КОНФЕРЕНЦИЯ «ЯДРО-2020» ЯДЕРНАЯ ФИЗИКА И ФИЗИКА ЭЛЕМЕНТАРНЫХ ЧАСТИЦ. ЯДЕРНО-ФИЗИЧЕСКИЕ ТЕХНОЛОГИИ. СБОРНИК ТЕЗИСОВ Онлайн часть. 12 – 17 октября 2020 Санкт-Петербург Organisers NRC «Kurchatov Institute» Saint Petersburg State University Joint Institute for Nuclear Research Chairs M. Kovalchuk (Chairman, NRC “Kurchatov Institute”) V. Zherebchevsky (Co-Chairman, SPbU) P. Forsh (Vice-Chairman, NRC “Kurchatov Institute”) Yu. Dyakova (Vice-Chairman, NRC “Kurchatov Institute”) A. Vlasnikov (Vice-Chairman, SPbU) S. Torilov (Scientific Secretary, SPbU) The contributions are reproduced directly from the originals. The responsibility for misprints in the report and paper texts is held by the authors of the reports. International Conference “NUCLEUS – 2020. Nuclear physics and elementary particle physics. Nuclear physics technologies” (LXX; 2020; Online part). LXX International conference “NUCLEUS – 2020. Nuclear physics and elementary particle physics. Nuclear physics technologies” (Saint Petersburg, Russia, 12–17 October 2020): Book of Abstracts /Ed. by V. N. Kovalenko and E. V. Andronov. – Saint Petersburg: VVM, 2020. – 324p. ISBN Международная Конференция «ЯДРО – 2020. Ядерная физика и физика элементарных частиц. Ядерно-физические технологии» (LXX; 2020; Онлайн часть). LXX Международная Конференция «ЯДРО – 2020. Ядерная физика и физика элементарных частиц. Ядерно-физические технологии» (Санкт-Петербург, Россия, 12–17 Октября 2020): Аннот. докл./под ред. В.Н. Коваленко, Е.В. Андронова. – Санкт-Петербург: ВВМ , 2020. – 324 c. ISBN 978-5-9651-0587-8 ISBN 978-5-9651-0587-8 ii Program Committee V.
    [Show full text]
  • Retrospect of GALLEX/GNO
    10th Int. Conf. on Topics in Astroparticle and Underground Physics (TAUP2007) IOP Publishing Journal of Physics: Conference Series 120 (2008) 052013 doi:10.1088/1742-6596/120/5/052013 Retrospect of GALLEX/GNO Till Kirsten Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany E-mail: [email protected] Abstract. After the completion of the gallium solar neutrino experiments at the Laboratori Nazionali del Gran Sasso (GALLEX, GNO), we shortly summarize the major achievements. Among them are the first observation of solar pp-neutrinos and the recognition of a substantial (40%) deficit of sub-MeV solar neutrinos that called for νe transformations enabled by non- vanishing neutrino masses. We also inform about a recent complete re-analysis of the GALLEX data evaluation and reflect on the causes for the termination of GNO. From our gallium data we extract the e-e survival probability Pee for pp-neutrinos after subtraction of the 8B and 7Be contributions based on the experimentally determined 8B- (SNO/SK) and 7Be- (Borexino) neutrino fluxes as Pee(pp only) = 0.52 ± 0.12. 1. Introduction The Gallium solar neutrino experiments at the Laboratori Nazionali del Gran Sasso have been terminated for external non-scientific reasons. This triggers a short retrospect of the achievements of GALLEX and GNO (Section 2). In Section 3 we report on a recent update that is based on data that were impossible to acquire before completion of the low rate measurement phase (solar runs). After some reflections on the causes for the termination of the gallium experiments at Gran Sasso (Section 4), I give a first quantitative estimate of the separate pp solar neutrino production (Section 5).
    [Show full text]
  • Postdoctoral Position in the DEAP and Darkside-20K Experiments
    Postdoctoral position in the DEPARTMENT OF PHYSICS Physics, Engineering Physics, DEAP and DarkSide-20k experiments Astronomy Stirling Hall Queen’s University Kingston, Ontario, Canada K7L 3N6 Tel 613 533-2707 Job Summary Fax 613 533-6463 The experimental particle astrophysics group at Queen's University in Kingston, Canada, which is part of the McDonald Institute (https://mcdonaldinstitute.ca/), expects to hire a postdoc to work on the argon dark matter searches DEAP-3600 and DarkSide-20k with Professors Philippe Di Stefano, Art McDonald and Peter Skensved, and with scientists at the TRIUMF laboratory. The postdoc will be actively involved in the analysis of data from the upgraded DEAP-3600 experiment, and in the development of digital electronics and DAQ for the DarkSide-20k experiment at Gran Sasso with 20 tonnes fiducial of liquid argon extracted from an underground source. Construction of a 1-ton prototype detector will start in 2021. These experiments are a stepping-stone towards a 300-tonne fiducial detector, Argo, for which the preferential location is SNOLAB. Work will be carried out in conjunction with the TRIUMF laboratory in Vancouver, with CERN, and with Gran Sasso. Required Qualifications - Candidates must have obtained a PhD in physics or applied physics, with a specialization in particle physics, nuclear physics, or instrumentation. In exceptional circumstances, PhD candidates with a firm date of defense will be considered. - The ability to perform independent research and to communicate results verbally and in writing. - The ability to work in a team including both graduate and undergraduate students. Preferred Qualifications - Experience with particle detectors, including readout, and scintillators.
    [Show full text]