DOCSLIB.ORG

Neutrino Signals at Dark Matter Direct Detection Experiments

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Neutrino Signals at Dark Matter Direct Detection Experiments Neutrino Signals at Dark Matter Direct Detection Experiments Jocelyn Monroe, Royal Holloway, University of London XXIX International Conference on Neutrino Physics and Astrophysics June 30, 2020 Dark Matter Direct Detection Signal: N ➙ N or e- ➙ e- Backgrounds: γ e- ➙γe- N ➙ N N ➙N’ + α, e- νN ➙νN experimental requirements: particle ID for recoil N, e-, alpha, n (multiple)γ final states γ Jocelyn Monroe June 30, 2020 / p. 2 Dark Matter Direct Neutrino Detection Signal: ν N ➙ ν N or ν e- ➙ ν e- ν ν Backgrounds: γ e- ➙γe- N ➙ N N ➙N’ + α, e- N ➙N? very similar requirements! ν (and ideally also measure direction) ν Jocelyn Monroe June 30, 2020 / p. 3 2008: Neutrino Backgrounds to Dark Matter Searches and Directionality Jocelyn Monroe May 30, 2008 2008 2020: Neutrino Backgrounds Signals in Dark Matter Searches (and Directionality) Jocelyn Monroe May 30, 2008 ν Cross Sections 2 2 -44 2 ν-N coherent scattering: ~ A x (Eν/MeV) x 10 cm recoils are O(10 keV) … neutrino floor in DM searches ν ν Z Φ(solar B8 ν) = 5.86 x 106 cm-2 s-1 N N Aprile et al., PhysRevLett 123 (2019) LZ Projected Nuclear Recoil Backgrounds J. Dobson, UCLA DM 2018 circa O(tens) of events/ton-year = 2008 ~ 10-46 cm2 limit JM, P. Fisher, Phys. Rev. D76 (2007) Rev. Phys. Fisher, JM, P. circa An irreducible background,2019 without direction measurement! JM, P. Fisher, Phys. Rev. D 76:033007 (2007) Jocelyn Monroe June 30, 2020 / p. 3 ν Cross Sections 2 2 -44 2 ν-N coherent scattering: ~ A x (Eν/MeV) x 10 cm recoils are O(10 keV) … neutrino floor in DM searches ν ν-e elastic scattering: smaller by ~ (me / Eν) ν but recoils are “high” energy ~ Eν Z and directional! e e LZ Projected Electronic Recoil Backgrounds LZ Projected Nuclear Recoil Backgrounds J. Dobson, UCLA DM 2018 J. Dobson, UCLA DM 2018 J. Dobson, UCLA DM’18 Jocelyn Monroe June 30, 2020 / p. 7 What ν signals can future dark matter detectors see? https://masterclass.icecube.wisc.edu/en/learn/detecting-neutrinos Jocelyn Monroe June 30, 2020 / p. 8 What ν signals can future dark matter detectors see? https://masterclass.icecube.wisc.edu/en/learn/detecting-neutrinos Jocelyn Monroe June 30, 2020 / p. 8 Future Large-Mass Dark Matter Detectors Detector Technology: dual-phase Time Projection Chambers with 4-50 tonne liquid Xe, Ar targets read out primary scintillation: “S1” + proportional gas scintillation from drifted electrons: “S2” • x-y resolution ~cm • z resolution ~mm Goal: zeptobarn -> yoctobarn sensitivity to dark matter! https://lz.slac.stanford.edu/our-research/lz-research Jocelyn Monroe June 30, 2020 / p. 9 2-Phase TPCs: Near(ish) Future XENON-nT: 6 t LXe (active), following XENON-1T (LNGS), from 2020. PandaX-4: 4 t LXe (active), following PandaX (JinPing), from 2020. LZ: 7 t LXe (active), following LUX (SURF), from 2020. DarkSide-20k: 50 t LAr (LNGS), ArDM+DEAP+DS50+MiniCLEAN, from 2023. DARWIN: 40 t LXe (LNGS), following XENON-nT. ARGO: 400 t LAr (SNOLAB?), following DarkSide-20k. 5 cm x 5 cm tiled SiPM Jocelyn Monroe 10 Jan. 23, 2019 Backgrounds N Gamma ray interactions: electron recoil final states rate ~ Ne x (gamma flux), O(1E7) events/(kg day) mis-identified electrons mimic nuclear recoils … part-per-billion level particle ID! Ajaj et al, Phys.Rev..D100 (2019) Contamination: modified from Malling, UCLA DM’16 238U and 232Th decays, recoiling progeny and 2009 mis-identified alphas, betas mimic nuclear recoils Neutrons: 2019 Nuclear recoil final state. (alpha,n), U, Th fission, DEAP, +PSD cosmogenic spallation pp solar neutrinos μ μ γ N* N D. Malling, UCLA DM’16 n D. Malling, UCLA DM’16 Jocelyn Monroe June 30, 2020 / p. 11 Backgrounds N Gamma ray interactions: electron recoil final states rate ~ Ne x (gamma flux), O(1E7) events/(kg day) mis-identified electrons mimic nuclear recoils … part-per-billion level particle ID! Ajaj et al, Phys.Rev..D100 (2019) Contamination: modified from Malling, UCLA DM’16 238U and 232Th decays, recoiling progeny and 2009 mis-identified alphas, betas mimic nuclear recoils Neutrons: 2019 Nuclear recoil final state. (alpha,n), U, Th fission, DEAP, +PSD cosmogenic spallation pp solar neutrinos μ μ γ N* N D. Malling, UCLA DM’16 n D. Malling, UCLA DM’16 Amaudruz et al, Phys.Rev.Lett. 121 (2018) no.7, 071801 Jocelyn Monroe June 30, 2020 / p. 11 Backgrounds N Gamma ray interactions: electron recoil final states rate ~ Ne x (gamma flux), O(1E7) events/(kg day) mis-identified electrons mimic nuclear recoils … part-per-billion level particle ID! Ajaj et al, Phys.Rev..D100 (2019) Contamination: modified from Malling, UCLA DM’16 238U and 232Th decays, recoiling progeny and 2009 mis-identified alphas, betas mimic nuclear recoils Neutrons: 2019 Nuclear recoil final state. (alpha,n), U, Th fission, DEAP, +PSD cosmogenic spallation pp solar neutrinos μ μ γ N* N D. Malling, UCLA DM’16 n D. Malling, UCLA DM’16 Jocelyn Monroe June 30, 2020 / p. 11 Backgrounds N Gamma ray interactions: electron recoil final states rate ~ Ne x (gamma flux), O(1E7) events/(kg day) mis-identified electrons mimic nuclear recoils … part-per-billion level particle ID! Ajaj et al, Phys.Rev..D100 (2019) Contamination: modified from Malling, UCLA DM’16 238U and 232Th decays, recoiling progeny and 2009 mis-identified alphas, betas mimic nuclear recoils Neutrons: 2019 Nuclear recoil final state. (alpha,n), U, Th fission, DEAP, +PSD cosmogenic spallation pp solar neutrinos μ μ γ N* N D. Malling, UCLA DM’16 n D. Malling, UCLA DM’16 + large, active veto detectors Jocelyn Monroe June 30, 2020 / p. 11 12 ) 10 -1 11 pp 10 7 What ν signals can bin Be -1 10 13 s 10 N -2 future dark matter detectors see? 109 15O 17 108 F 8B 107 Flux (cm hep ν 106 105 Solar 104 103 102 10-1 1 10 Neutrino Energy (MeV) https://masterclass.icecube.wisc.edu/en/learn/detecting-neutrinos Jocelyn Monroe June 30, 2020 / p. 12 Prospects for Solar ν-N Coherent Scattering European Strategy for Particle Physics, Physics Briefing Book (2019) DarkSide-20k ESPP 2019 Jocelyn Monroe June 30, 2020 / p. 13 12 ) 10 -1 Solar ν-e Event Rates 11 pp 10 7 ν bin Be ν -1 10 13 s 10 N example event rates -2 109 15O of solar neutrino-electron Z, W 17 108 F elastic scattering at LNGS, 8B 107 per tonne-year of CF4 Flux (cm hep e e ν 106 105 Solar 104 103 102 10-1 1 10 Neutrino Energy (MeV) e.g. for Ar target: DarkSide-20k estimates 10k solar neutrino- electron elastic scatters above threshold per 100 tonne-yrs Aalseth, et al. Eur.Phys.J.Plus 133 (2018) Jocelyn Monroe June 30, 2020 / p. 14 Statistics even allow solar oscillation physics! Solar ν-e Event Rates ν ν example event rates of solar neutrino-electron Z, W elastic scattering at LNGS, per tonne-year of CF4 e e Aalbers, et al. arXiv:2006.03114 e.g. for Ar target: DarkSide-20k estimates 10k solar neutrino- electron elastic scatters above threshold per 100 tonne-yrs Aalseth, et al. Eur.Phys.J.Plus 133 (2018) Jocelyn Monroe June 30, 2020 / p. 15 Statistics even allow solar oscillation physics! Solar ν-e Event Rates ν ν example event rates of solar neutrino-electron Z, W elastic scattering at LNGS, per tonne-year of CF4 e e Aalbers, et al. arXiv:2006.03114 e.g. for Ar target: DarkSide-20k estimates 10k solar neutrino- electron elastic scatters above threshold per 100 tonne-yrs Aalseth, et al. Eur.Phys.J.Plus 133 (2018) Jocelyn Monroe June 30, 2020 / p. 15 Solar ν-Electron Scattering Via neutrino-electron elastic scattering, LAr dark matter experiments can measure CNO (via spectral deformation), and CNO vs. Be-7 +with O(500 t-y), study the “solar metallicity problem”. Franco et al., JCAP 1608 (2016) 08 Cerdeno, Davis, Fairbairn, Vincent, JCAP 1804 (2018) 37 big opportunities: 1) distinguish exclusion betweendetection high vs. low metallicity. *Xe-136 background makes LXe CNO more challenging Baudis et al., JCAP 1401 (2014) 044, Baudis et al., 2006.03114 Jocelyn Monroe June 30, 2020 / p. 16 C. Boehm et al., 2006.11250 Solar ν-Electron Scattering Via neutrino-electron elastic scattering, LAr dark matter experiments can measure CNO (via spectral deformation), and CNO vs. Be-7 Xenon1T data +with O(500 t-y), study the “solar metallicity problem”. Franco et al., JCAP 1608 (2016) 08 Cerdeno, Davis, Fairbairn, Vincent, JCAP 1804 (2018) 37 big opportunities: 1) distinguish exclusion betweendetection high vs. low metallicity. 2) study non- standard solar neutrino interactions? *Xe-136 background makes LXe CNO more challenging Aprile et al., 2006.09721 Baudis et al., JCAP 1401 (2014) 044, Baudis et al., 2006.03114 Boehm et al., 2006.11250 Jocelyn Monroe June 30, 2020 / p. 17 Lang et al., Phys. Rev. D 94 (2016) What neutrino signals can Arnaud et al., Phys.Rev.D.65.033010 future dark matter detectors see? (if lucky!) for a supernova at 10 kPc, expect 300-500 ν-N events in near-future experiments. • measure all flavors via NC 40 - 40 • measure νe Ar e K* • multi-messenger observation: sub-eV mass ordering? https://masterclass.icecube.wisc.edu/en/learn/detecting-neutrinos Jocelyn Monroe May 3, 2018 / p. 7 Lang et al., Phys. Rev. D 94 (2016) What neutrino signals can Arnaud et al., Phys.Rev.D.65.033010 future dark matter detectors see? (if lucky!) for a supernova at 10 kPc, expect 300-500 ν-N events in near-future experiments.
Load more

Recommended publications
  • 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.
    [Show full text]
  • Curriculum Vitæ Jocelyn Monroe
    CURRICULUM VITÆ JOCELYN MONROE ! ADDRESS: CONTACT: Royal Holloway University of London Phone: +44 1784 443513 Department of Physics, W255 Email: [email protected] Egham, Surrey Web: http://www.pp.rhul.ac.uk/~jmonroe EDUCATION: 2006: Ph.D. (Physics) Columbia University Dissertation Title: “A Combined "µ and "e Oscillation Search at MiniBooNE,” Advisor: Prof. Michael Shaevitz 2002: M.A. (Physics) Columbia University 2002: M.Phil. (Physics) Columbia University 1999: B.A. (Astrophysics) Columbia University EMPLOYMENT: May 2013-: Professor of Physics, Royal Holloway University of London 2011-2013: Senior Lecturer, Royal Holloway University of London 2009-2014: Assistant Professor, Massachusetts Institute of Technology 2006-2009: Pappalardo Fellow, Massachusetts Institute of Technology 2000-2006: Research Assistant, Columbia University 1999-2000: Engineering Physicist, Beams Division, Fermi National Accelerator Laboratory 1997: DOE REU Summer Program, Particle Physics Division, Fermi National Accelerator Laboratory COLLABORATION MEMBERSHIPS: 2017-: DarkSide-20k Collaboration, UK P.I. (LNGS, IT), Deputy Spokesperson (2021-) 2019-: The PlomBox Project, P.I. (https://plombox.org/) 2008-: DEAP-3600 (SNOLab, Canada), Executive Board Chair (2014-15) 2006-2016: DMTPC (WIPP, USA), Spokesperson (2011-2016) 2006-2009: SNO (SNOLab, Canada) 1999-2008: MiniBooNE (FNAL, USA) 1999-2000: Neutrino Factory (FNAL, USA) AWARDS AND HONORS: 2016 Breakthrough Prize in Fundamental Physics Laureate 2012 Kavli Frontiers of Science Fellow, U.S. National Academy
    [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]
  • 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).
    [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]
  • Monday 22 June
    Monday 22 June 7:00 AM US CDT Opening 7:00 AM 10 Welcome Steve Brice Fermilab 7:10 AM 5 Update on IUPAP neutrino panel Nigel Smith SNOLab 7:15 AM 5 The Snowmass process for neutrinos Kate Scholberg Duke University 7:20 AM 35+5 Neutrinos in the era of multi-messenger astronomy Francis Halzen University of Wisconsin, Madison 8:00 AM US CDT 10 Break 8:10 AM 25+5 A review of progress in R&D for neutrino detectors David Nygren University of Texas, Arlington 8:40 AM 17+3 Neutrino oscillation measurements with IceCube Summer Blot DESY/Zeuthen 9:00 AM US CDT 10 Break 9:10 AM US CDT Direct Neutrino Mass Measurements 9:10 AM 17+3 Mass meaurements with Ho-163 Maurits Haverkort University of Heidelberg 9:30 AM 20+5 Project 8 Noah Oblath Pacific Northwest National Laboratory 9:55 AM 20+5 KATRIN: first results and future perspectives Susanne Mertens Technical University Munich and Max Planck Institute for Physics 10:20 AM US CDT 10 Break 10:30 AM 60 Poster Session 11:30 AM US CDT End of Day Tuesday 23 June 7:00 AM US CDT Neutrino Interactions 7:00 AM 25+5 Historical Review and Future program of neutrino cross section measurements and calculations Noemi Rocco Argonne National Laboratory and Fermilab 7:30 AM 17+3 Connections between neutrino and electron scattering Adi Ashkenazi MIT 7:50 AM US CDT 10 Break 8:00 AM 20+5 The Neutrino's View of the Nucleus: New Results from MINERvA Deepika Jena Fermilab 8:25 AM 20+5 Neutrino Interaction Measurements on Argon Kirsty Duffy Fermilab 8:50 AM 20+5 Cross-section measurements with NOvA Linda Cremonesi University
    [Show full text]
  • Understanding the Universe from Deep Underground
    Understanding the Universe from Deep Underground Sudbury Neutrino Observatory Art McDonald, Professor Emeritus Queen’s University, Kingston, Ontario, Canada With our laboratory deep underground we have created a very low radioactivity location where we study some of the most basic scientific questions: • How do stars like our Sun burn and create the elements from which we are made? • What are the basic Laws of Physics for the smallest fundamental particles? • What is the composition of our Universe and how has it evolved to the present ? How do you make measurements that can provide answers to enormous questions like these? Answers: 1: Measure elusive particles called NEUTRINOS that come from the deepest reaches of the Sun where the energy is generated and from cosmic rays interacting in the atmosphere. 2: Measure fundamental particles (DARK MATTER) that are left over from the original formation of the Universe. 3. Measure rare forms of radioactivity (DOUBLE BETA DECAY) that can tell us more about fundamental laws of physics. Neutrinos from the Sun The middle of the sun is so hot that the centers of the atoms (nuclei) fuse together, giving off lots of energy and neutrinos. The neutrinos penetrate easily through the dense material in the Sun and reach the earth. Neutrino facts: • Neutrinos, along with electrons and quarks, are basic particles of nature that we do not know how to sub-divide further. • Neutrinos come in three “flavours” (electron, mu, tau) as described in The Standard Model of Elementary Particles, a fundamental theory of microscopic particle physics. •They only stop if they hit the nucleus of an atom or an electron head-on and can pass through a million billion kilometers of lead without stopping.
    [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]
  • Jocelyn Monroe
    CURRICULUM VITÆ JOCELYN MONROE ADDRESS: CONTACT: Massachusetts Institute of Technology Phone: (617) 253 2332 77 Massachusetts Avenue, 26-561 Email: [email protected] Cambridge, MA 02139 Web: http://molasses.lns.mit.edu/jocelyn EDUCATION: 2006: Ph.D. (Physics) Columbia University Dissertation Title: “A Combined νµ and νe Oscillation Search at MiniBooNE,” Advisor: Prof. Michael Shaevitz 2002: M.A. (Physics) Columbia University 2002: M.Phil. (Physics) Columbia University 1999: B.A. (Astrophysics) Columbia University EMPLOYMENT: July 2009-: Assistant Professor, Massachusetts Institute of Technology 2006-2009: Pappalardo Fellow, Massachusetts Institute of Technology 2000-2006: Research Assistant, Columbia University 1999-2000: Engineering Physicist, Beams Division, Fermi National Accelerator Laboratory 1997: DOE REU Summer Program, Particle Physics Division, Fermi National Accelerator Laboratory COLLABORATION MEMBERSHIPS: 2008-: CLEAN/DEAP Collaboration (SNOLab, Canada) 2006-: DMTPC Collaboration (MIT, USA) 2006-: SNO Collaboration (SNOLab, Canada) 1999-: MiniBooNE Collaboration (FNAL, USA) 1999-2000: Neutrino Factory Collaboration (FNAL, USA) COMMITTEES: SNO Physics Interpretation Review Committee Chair (2006-present) SNO Low Energy Threshold Analysis Review Committee Member (2006-2009) Conference Organizer, 2nd CYGNUS Directional Dark Matter Workshop (2009) SNO Collaboration Executive Board Junior Member (2007-2008) Conference Organizer, 5th International Workshop on Neutrino Factories (2003) Jocelyn Monroe 1 of 11 OUTREACH: 2009 MIT Physics
    [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]
  • 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 .
    [Show full text]