Scintillator phase of the SNO+ experiment
|
|
- Cordelia Henderson
- 6 years ago
- Views:
Transcription
1 Mathematik und Naturwissenschaften Institut für Kern- und Teilchen Physik Scintillator phase of the experiment Valentina Lozza On behalf of Collaboration TAUP2011, Munich
2 Outline = SNO + Liquid Scintillator - New detector design - Liquid scintillator Phases of Operation: - Scintillator phase - Nd loaded phase Solar neutrinos - pep - CNO Geo and reactor neutrinos Summary
3 Detector 780t of liquid scintillator (LAB) Active medium PSUP = PMT Support Structure ~9500 PMT ~ 54% coverage Acrylic Vessel Φ=12 m, thickness = 5 cm Light water (H2O) shielding t internal t external Urylon Liner and Radon Seal
4 Detector 780t of liquid scintillator (LAB) Active medium PSUP = PMT Support Structure ~9500 PMT ~ 54% coverage Acrylic Vessel Φ=12 m, thickness = 5 cm Light water (H2O) shielding t internal t external Urylon Liner and Radon Seal
5 New ropes hold down system Liquid scintillator is lighter than water (ρ=0.86 g/cm3) From SNO To Hold up Hold down
6 New ropes hold down system Liquid scintillator is lighter than water (ρ=0.86 g/cm3) From SNO To Hold up Hold down
7 Liquid scintillator LAB Linear alkylbenzene (LAB) identified as the liquid scintillator solvent Chemical compatibility with acrylic High light yield ( times higher than D2O) Good optical transparency Low scattering Fast decay, different for alphas and betas High purity available Safe Low toxicity High flash point 130 C Boiling point C Environmentally safe Low solubility in water mg/l Inexpensive Petresa Plant Bécancour, QC
8 Liquid scintillator LAB Linear alkylbenzene (LAB) identified as the liquid scintillator solvent Chemical compatibility with acrylic High light yield ( times higher than D2O) Good optical transparency Low scattering Fast decay, different for alphas and betas High purity available Safe Low toxicity High flash point 130 C Boiling point C Environmentally safe Low solubility in water mg/l Inexpensive Safe scintillators Petresa Plant Bécancour, QC
9 Phases of operation Two main phases of operation: Liquid Scintillator Phase Solar Neutrinos Reactor and Geo-Neutrinos Supernovae Neutrinos Nd-Loaded phase Neutrinoless Double-Beta decay Reactor and Geo-Neutrinos Supernovae Neutrinos Other interesting studies: nucleon decay, sterile neutrinos,...
10 Nd loaded phase Neutrinoless double beta decay with liquid scintillator: Large mass, low background Poor energy resolution (3.5% at Nd endpoint) Use 150Nd : High Q-value (3371 kev) low background Successfully loaded in LAB. 0.1% loading Optimized 0.3% under study See Jeffrey Hartnell talk Double Beta Decay, Neutrino Mass W4
11 Scintillator phase: Solar neutrinos Complete our understanding of the solar neutrino fluxes (complementary to SNO) Next target measurement: pep, 7Be and 8B neutrinos Possibility to further extend into pp region (depending on 14C and 85Kr levels) Probe solar metallicity with CNO (spectrum shape very close to the 210Bi one)
12 pep neutrinos, Why? pep solar neutrino component is favorable due to: - single energy (1.442 MeV) - very well predicted flux (1.1 % uncertainty) Accurate measurements of neutrino survival probabilities in the low energy range can: - improve the precision on the oscillation parameters - provide sensitivity to alternative models of neutrino mixing pep solar neutrino as a test for MSW present data suggest MSW testing the vacuum-matter transition is sensitive to new physics Vacuum dominated Matter dominated
13 pep neutrinos, Why? pep solar neutrino component is favorable due to: - single energy (1.442 MeV) - very well predicted flux (1.1 % uncertainty) Accurate measurements of neutrino survival probabilities in the low energy range can: - improve the precision on the oscillation parameters - provide sensitivity to alternative models of neutrino mixing Friedland, Lunardini, Peña-Garay, PLB 594 (2004) Good probe for NSI pep solar neutrino as a test for MSW present data suggest MSW testing the vacuum-matter transition is sensitive to new physics Vacuum dominated oscillation solutions with NSI can fit existing solar and atmospheric neutrino data NSI not currently constrained new pep solar neutrino data would test NSI Matter dominated
14 pep neutrinos, Requirements Requirements for measuring the pep neutrino flux 1. Depth reduce the background induced by cosmogenic muons (11C) 2. Good light output from the scintillator 3. Radiopurity - 14C is not a problem since pep signal is at higher energy - U, Th not a problem if one can repeat KamLAND scintillator purity - 40K, 210Bi (Radon daughter) - 85Kr, 210Po not a problem since pep signal is at higher energy
15 pep neutrinos, 11C 11C decays are the major background in pep energy window Since they are produced by cosmic muons, the deeper the experiment the better the background KamLAND Borexino Eμ [GeV] n12c[x1031] (all C) 4.51 R data [kt 1yr 1] (1.14±0.21) 103 (403.69±64.97) 103 (102.20±1.46) 103 other expected backgrounds not shown - 1 year exposure ktons fiducial volume (50%) - detector resolution of 5%/ (E[MeV]). -11C background signal is obtained from KamLAND data extrapolation
16 pep neutrinos, 11C 11C decays are the major background in pep energy window Since they are produced by cosmic muons, the deeper the experiment the better the background KamLAND Borexino Eμ [GeV] n12c[x1031] (all C) 4.51 R data [kt 1yr 1] (1.14±0.21) 103 (403.69±64.97) 103 (102.20±1.46) 103 other expected backgrounds not shown Borexino - 1 year exposure 100 tons fiducial volume detector resolution of 5%/ (E[MeV]). data from arxiv: v1
17 pep neutrinos, Impact on osc. parameters E range: MeV, 50% FV Determine the survival probability according to the current solar best fit point: tan²θ12 := Δm21² := 6.02 x 10-5 ev² sin²θ13 := 0.01 Adding 1 resp. 2 years of data to the other solar experiments (excl. latest Borexino) Significant improvement on sin²θ13
18 CNO neutrinos Improved models (2005) suggest 30% lower metallicity broken the previous excellent agreement between solar model calculations and helioseismology Astrophysical puzzle: Are elements homogeneously distributed in the Sun? CNO neutrinos can measure the metalicity of the core. BPS08 solar model: Peña-Garay and Serenelli arxiv:
19 Geo neutrinos Anti-neutrinos from U-238, Th-232 and K-40 on Earth o 20% from mantle at o Check models of Earth heat production detection: anti-ve + p e+ + n Measured geo-neutrino flux: KamLAND2008 (25±9) ev/kt yr 1.6 Borexino ( ) ev/0.1kt yr Expected geo-neutrino flux : 29 ev/0.78kt(lab) yr - 21ev/0.78kT(LAB) yr from reactor KamLAND: 32ev/1kT(CH2) yr 218ev/1kT(CH2) yr from reactor Borexino: 3ev/0.1kT(C9H12) yr 1.5 ev/0.1kt(c9h12) yr from reactor S. Enomoto XIII International Workshop on Neutrino Telescopes, Venice, March MULTI SITE MEASUREMENT
20 Reactor neutrinos Bruce Detection rate including oscillation Pickering Darlington
21 Reactor neutrinos Flux is 5 times less than KamLAND BUT reactor spectrum, including oscillations, have sharp peaks and minima, that increase the parameter-fitting sensitivity for Δm212 Bruce Pickering Darlington
22 Current Status By the end of the year (2011) Detector upgrade Cavity work, cleaning, PMT repairs Install hold-down rope system Install new calibration hardware Electronic update Next year(2012) Detector upgrade Install purification systems Commissioning Water fill and run Start scintillator fill 2013 Physics/Commissioning Start liquid scintillator phase
23 Summary is the follow up of the SNO experiment replacing the heavy water by liquid scintillator Liquid scintillator has a higher light yield than heavy water and allows to investigate the low energy region (E < 3.5MeV) Two phases of the experiment with different physical goals are planned: A liquid scintillator phase for the search of low energy solar neutrinos (pep, CNO) A Nd loaded phase for the search of neutrinoless double beta decay Other exciting physical goals are reactor oscillation confirmation, geo-neutrinos in a geologically-interesting location, supernova neutrino watch,... The main upgrades to the detector will be completed by the end of the year will start operation with water fill in the second half of 2012
24 BACKUP SLIDES
25 Location
26 SNOLAB: existing SNO facility Over 53,000 sq.ft. of climate-controlled class-2000 cleanroom laboratory space Scintillator purification Water plant Rail-car unloading terminal Storage tanks control room detector
27 SNOLAB: existing SNO facility Over 53,000 sq.ft. of climate-controlled class-2000 cleanroom laboratory space Scintillator purification Water plant Rail-car unloading terminal Storage tanks control room detector
28 SNOlab Inside SNOlab Outside SNOlab
29 Liquid scintillator LAB Purification strategies: Multi-stage distillation Initial LAB cleanup for high radio-purity and optical clarity Dual-stream PPO distillation for scintillator recirculation Pre-purification of PPO concentrated solution Steam/N2 stripping under vacuum Water extraction (liquid-liquid extraction) Effective for ionic metals (K, Pb, Ra) and limited efficiency for Th and Po Stable for PPO-LAB solutions Functional metal scavengers (R&D) High-flow columns effective for Pb, Bi and Ra
Solar Neutrinos in Large Liquid Scintillator Detectors
Solar Neutrinos in Large Liquid Scintillator Detectors M. Chen Queen s University DOANOW March 24, 2007 Low Energy Solar Neutrinos complete our understanding of neutrinos from the Sun pep, CNO, 7 Be, pp
More informationNeutrino Physics with SNO+ Freija Descamps for the SNO+ collaboration
Neutrino Physics with SNO+ Freija Descamps for the SNO+ collaboration NOW 2014, Otranto, Lecce, Italy September 7-14, 2014 Intro Neutrino physics with the SNO+ detector 2 Intro What we know:! Neutrinos
More informationNeutrinoless Double Beta Decay Search with SNO+
Neutrinoless Double Beta Decay Search with SNO+ Kalpana Singh for the SNO+ Collaboration University of Alberta 8th Nov. 2016 1 Location 8th Nov. 2016 2 Location, 5890 mwe 8th Nov. 2016 3 63 muons/ day
More informationNeutrinoless double beta decay with SNO+
Neutrinoless double beta decay with SNO+ - 0!"" with SNO+ - Backgrounds - Schedule Freija Descamps for the SNO+ collaboration 1 SNO+ detector 6000 m.w.e Deck with DAQ SNO+ operator ~780T LAB liquid organic
More informationSolar Neutrinos: Status and Prospects. Marianne Göger-Neff
Solar Neutrinos: Status and Prospects Marianne Göger-Neff NIC 2014, Debrecen TU München Solar Neutrinos Objective of the first solar neutrino experiment: to see into the interior of a star and thus verify
More informationSNO+ ARTFEST, MAY 2014, KINGSTON DR. CHRISTINE KRAUS, LAURENTIAN UNIVERSITY
SNO+ ARTFEST, MAY 2014, KINGSTON DR. CHRISTINE KRAUS, LAURENTIAN UNIVERSITY SNO+ IS LOCATED AT SNOLAB 300 km Canada Ontario Sudbury Creighton mine use existing SNO cavity 2 km or 6000 m.w.e. Artfest 2014,
More informationSolar Neutrinos with Borexino Low Background Lessons for the JinPing Laboratory
Solar Neutrinos with Borexino Low Background Lessons for the JinPing Laboratory Frank Calaprice and Jingke Xu Department of Physics Princeton University 4/10/2014 Solar Neutrinos at Jin Ping 1 Solar Neutrinos
More informationBorexino and status of the project Aldo Ianni INFN, Gran Sasso Laboratory on behalf of the Borexino collaboration
Borexino and status of the project Aldo Ianni INFN, Gran Sasso Laboratory on behalf of the Borexino collaboration Moscow, 15/10/2005 Aldo Ianni, INFN LNGS 1 Outline Borexino: Italian-Russian cooperation
More informationRecent Discoveries in Neutrino Physics
Recent Discoveries in Neutrino Physics Experiments with Reactor Antineutrinos Karsten Heeger http://neutrino.physics.wisc.edu/ Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009 Standard Model and
More informationA Large Liquid Scintillator Detector for Neutrino Mass Hierarchy : RENO-50
A Large Liquid Scintillator Detector for Neutrino Mass Hierarchy : RENO-50 International Meeting for Large Neutrino Infrastructures Ecole Architecture Paris Val de Seine, APPEC, 23-24 June, 2014 Soo-Bong
More informationRecent results from Borexino Gemma Testera INFN Genova TAUP 2015 September 7th, 2015
Recent results from Borexino Gemma Testera INFN Genova TAUP 2015 September 7th, 2015 Signals in Borexino Solar n Anti-n from the Earth (see A. Ianni talk) Anti-n (or n) from a radioactive source (SOX,
More information192 days of Borexino. Neutrino 2008 Christchurch, New Zeland May 26, Cristiano Galbiati on behalf of Borexino Collaboration
192 days of Borexino Neutrino 2008 Christchurch, New Zeland May 26, 2008 Cristiano Galbiati on behalf of Borexino Collaboration 2 Solar Neutrinos Spectrum 3 Solar Neutrinos Spectrum SNO, SuperK 3 Solar
More informationRivelazione di neutrini solari - Borexino Lino Miramonti 6 Giugno 2006 Gran Sasso
Rivelazione di neutrini solari - Borexino Lino Miramonti 6 Giugno 2006 Gran Sasso 1 RADIOCHEMICAL Integrated in energy and time CHERENKOV Less than 0.01% of the solar neutrino flux is been measured in
More informationBOREXINO: A MULTI-PURPOSE DETECTOR FOR THE STUDY OF SOLAR AND TERRESTRIAL NEUTRINOS
BOREXINO: A MULTI-PURPOSE DETECTOR FOR THE STUDY OF SOLAR AND TERRESTRIAL NEUTRINOS Alex Wright Princeton University University of Chicago HEP Seminar May 10 th, 2010 Solar Neutrino Production p-p Solar
More informationReview of Solar Neutrinos. Alan Poon Institute for Nuclear and Particle Astrophysics & Nuclear Science Division Lawrence Berkeley National Laboratory
Review of Solar Neutrinos Alan Poon Institute for Nuclear and Particle Astrophysics & Nuclear Science Division Lawrence Berkeley National Laboratory Solar Neutrinos pp chain: 4p + 2e 4 He + 2ν e + 26.7
More informationLeaching Studies for the SNO+ Experiment
Leaching Studies for the SNO+ Experiment Pouya Khaghani Laurentian University SNOLAB Users Meeting Symposium September 2 nd 2016 1 SNO+ Physics SNOLAB, Creighton Mine (2070m 6000 m. w. e) Linear Alkyl
More informationAndrey Formozov The University of Milan INFN Milan
T h e i nv e s t i g a t i o n of l i q u i d s c i n t i l l a t o r p ro p e r t i e s, e n e r g y a n d s p a t i a l re s o l u t i o n fo r JUNO re a c t o r n e u t r i n o e x p e r i m e n t Andrey
More informationUSING NEUTRINOS TO STUDY THE EARTH. Nikolai Tolich University of Washington
USING NEUTRINOS TO STUDY THE EARTH Nikolai Tolich University of Washington Outline Introduction Recent results The future Structure of the Earth Seismic data splits Earth into 5 basic regions: inner core,
More informationPresent and future of SNO: SNO, SNO+ and SNOLAB. Aksel Hallin,Queen s University for the SNO Collaboration NDM, Paris, September 2006
Present and future of SNO: SNO, SNO+ and SNOLAB Aksel Hallin,Queen s University for the SNO Collaboration NDM, Paris, September 2006 Sudbury Neutrino Observatory 1000 tonnes D 2 O Support Structure for
More informationResults from Borexino on solar (and geo-neutrinos) Gemma Testera
Results from Borexino on solar (and geo-neutrinos) Gemma Testera Istituto Nazionale di Fisica Nucleare (Genova) On behalf of the Borexino collaboration Scintillator: 270 t PC+PPO (1.5 g/l) in a 150 mm
More informationResults on geoneutrinos at Borexino experiment. Heavy Quarks and Leptons Yamagata Davide Basilico
Results on geoneutrinos at Borexino experiment Heavy Quarks and Leptons 2018 - Yamagata Davide Basilico Outline 1. Geoneutrinos 2. Borexino 3. Analysis and results 2 What are geoneutrinos? Distribution
More informationNeutrino detectors. V. Lozza,
Neutrino detectors, 5.10.2011 Outline - Introduction to neutrinos Sources of neutrinos Detection techniques Why we need to go underground? Background components What to do? Summary A brief of history 1914:
More informationKamLAND. Studying Neutrinos from Reactor
KamLAND : Studying Neutrinos from Reactor Atsuto Suzuki KEK : High Energy Accelerator Research Organization KamLAND Collaboration Outline 1. KamLAND Overview 2. Reactor Neutrinos 3. e Detection in Liquid
More informationNeutrino Experiments: Lecture 2 M. Shaevitz Columbia University
Neutrino Experiments: Lecture 2 M. Shaevitz Columbia University 1 Outline 2 Lecture 1: Experimental Neutrino Physics Neutrino Physics and Interactions Neutrino Mass Experiments Neutrino Sources/Beams and
More informationSolar spectrum. Nuclear burning in the sun produce Heat, Luminosity and Neutrinos. pp neutrinos < 0.4 MeV
SOLAR NEUTRINOS Solar spectrum Nuclear burning in the sun produce Heat, Luminosity and Neutrinos pp neutrinos < 0.4 MeV Beryllium neutrinos 0.86 MeV Monochromatic since 2 body decay 2 kev width due to
More informationNeutrinos from the Sun and other sources: Results from the Borexino experiment
Neutrinos from the Sun and other sources: Results from the Borexino experiment Marianne Göger-Neff 23.05.2014 Neutrinos from the Sun and other sources: Results from the Borexino experiment Motivation:
More informationLOW ENERGY SOLAR NEUTRINOS WITH BOREXINO. Lea Di Noto on behalf of the Borexino collaboration
LOW ENERGY SOLAR NEUTRINOS WITH BOREXINO Lea Di Noto on behalf of the Borexino collaboration Vulcano Workshop 20 th -26 th May 2018 [cm -2 s -1 MeV -1 ] SOLAR NEUTRINOS Electrons neutrinos are produced
More informationSynthesis and Characterization of Organic Tellurium Compounds for SNO+ Liquid Scintillator
Synthesis and Characterization of Organic Tellurium Compounds for SNO+ Liquid Scintillator Lianpeng Tian Queen s University For SNO+ Collaboration LSC2017 Conference Large multi-purpose liquid scintillator
More informationSolar Neutrinos with Borexino at LNGS Current Results/Future Opportunities
Solar Neutrinos with Borexino at LNGS Current Results/Future Opportunities Frank Calaprice Princeton University 10/15/13 U.S. - Italy Celebration, Princeton 1 Borexino Collaboration A 20 + year successful
More informationThe GERmanium Detector Array
The GERmanium Detector Array n n ν=v p e - e - p Outline: Exp. issues of 0νββ-decay of 76 Ge Concept of GERDA Status of the experiment Summary and conclusions Kevin Kröninger (Max-Planck-Institut für Physik,
More informationLi in a WbLS Detector
7 Li in a WbLS Detector Gabriel D. Orebi Gann JinPing Solar Workshop, LBNL June 10th, 2014 U. C. Berkeley & LBNL Probing the Transition Region: why we need 8 B Largest affect on shape of survival probability
More informationWater Purification in Borexino
Water Purification in Borexino Marco G. Giammarchi Istituto Nazionale di Fisica Nucleare - Via Celoria 16 20133 Milano (Italy) marco.giammarchi@mi.infn.it http://pcgiammarchi.mi.infn.it/giammarchi/ On
More informationSearch for Sterile Neutrinos with the Borexino Detector
Search for Sterile Neutrinos with the Borexino Detector PANIC 2014 Hamburg on behalf of the BOREXINO Collaboration Institut für Experimentalphysik (Universität Hamburg) Borexino Detector Site 1400 m of
More informationThe LENA Neutrino Observatory
The LENA Neutrino Observatory for the LENA Collaboration 1 Consortium of European science institutions and industry partners Design studies funded by the European Community (FP7) LAGUNA: detector site,
More informationAldo Ianni, LNGS for the Borexinocollaboration Sept. 29th, 2011
Aldo Ianni, LNGS for the Borexinocollaboration Sept. 29th, 2011 First Borexino proposal: 1991 Main goal: real time measurement of sub-mev solar neutrinos Why? To solve the Solar Neutrino Puzzle (missingsolarneutrinos)
More informationThe SOX experiment. Stefano Davini (on behalf of the Borexino-SOX collaboration) Brussels, December 1 st 2017
The SOX experiment Stefano Davini (on behalf of the Borexino-SOX collaboration) Brussels, December 1 st 2017 Beyond the Standard model with Neutrinos Neutrino masses call for physics beyond Standard model
More informationDaya Bay and joint reactor neutrino analysis
Daya Bay and joint reactor neutrino analysis Logan Lebanowski (Tsinghua University) on behalf of the Daya Bay collaboration 2016/11/4 - NNN16, Beijing 1 Contents Daya Bay Reactor Neutrino Experiment Introduction
More informationScintillator Detectors for Neutrino Physics
Scintillator Detectors for Neutrino Physics Minfang Yeh Neutrino and Nuclear Chemistry, BNL Jinping Workshop, Tsinghua, June 5, 2015 BNL-Liquid Scintillator Development Facility A unique facility (since
More information0νββ Physics in WbLS. Andy Mastbaum University of Pennsylvania. WbLS Workshop LBNL 17 May 2014
0νββ Physics in WbLS Andy Mastbaum University of Pennsylvania WbLS Workshop LBNL 17 May 2014 Requirements Future detectors must: Reach a sensitivity of 15 mev at the 3σ CL after years of running, according
More informationOutline. (1) Physics motivations. (2) Project status
Yu-Feng Li Institute of High Energy Physics, Beijing On behalf of the JUNO collaboration 2014-10-10, Hsinchu/Fo-Guang-Shan 2nd International Workshop on Particle Physics and Cosmology after Higgs and Planck
More informationResults from Borexino 26th Rencontres de Blois
Results from Borexino 26th Rencontres de Blois - 2014 Marco G. Giammarchi Istituto Nazionale di Fisica Nucleare Via Celoria 16 20133 Milano (Italy) marco.giammarchi@mi.infn.it http://pcgiammarchi.mi.infn.it/giammarchi/
More informationMetallicities in stars - what solar neutrinos can do
- what solar neutrinos can do Institute for Nuclear and Particle Physics, Technical University Dresden, 01069 Dresden, Germany E-mail: zuber@physik.tu-dresden.de New elemental abundance determinations
More informationProton decay and neutrino astrophysics with the future LENA detector
Proton decay and neutrino astrophysics with the future LENA detector Teresa Marrodán Undagoitia tmarroda@ph.tum.de Institut E15 Physik-Department Technische Universität München Paris, 11.09.08 Outline
More informationStatus of Solar Neutrino Oscillations
Status of Solar Neutrino Oscillations With many thanks to Dave Wark - RAL/ University of Sussex and Stephen Brice - Fermilab The Solar Neutrino Problem Next three plots adapted from http://www.sns.ias.edu/~jnb/
More informationSolar and atmospheric ν s
Solar and atmospheric ν s Masato SHIOZAWA Kamioka Observatory, Institute for Cosmic Ray Research, U of Tokyo, and Kamioka Satellite, Kavli Institute for the Physics and Mathematics of the Universe (WPI),
More informationStatus and Neutrino Oscillation Physics Potential of the Hyper-Kamiokande Project in Japan
Status and Neutrino Oscillation Physics Potential of the Hyper-Kamiokande Project in Japan Gianfranca De Rosa Univ. Federico II and INFN Naples On behalf of Hyper-Kamiokande Collaboration Hyper-Kamiokande:
More informationSolar Neutrino Oscillations
Solar Neutrino Oscillations ( m 2, θ 12 ) Background (aka where we were): Radiochemical experiments Kamiokande and Super-K Where we are: Recent results SNO and KamLAND Global picture Where we are going:
More informationSNO+ and Geoneutrino Physics
SNO+ and Geoneutrino Physics by Chunlin Lan A thesis submitted to the Department of Physics, Engineering Physics and Astronomy in conformity with the requirements for the degree of Master of Science Queen
More informationKamLAND. Introduction Data Analysis First Results Implications Future
KamLAND Introduction Data Analysis First Results Implications Future Bruce Berger 1 Tohoku University, Sendai, Japan University of Alabama University of California at Berkeley/LBNL California Institute
More informationNeutrino oscillation experiments: Recent results and implications
Title transparency Neutrino oscillation experiments: Recent results and implications W. Hampel MPI Kernphysik Heidelberg Motivation for talk On the way from the Standard Model to String Theory: appropriate
More informationChart of Elementary Particles
Chart of Elementary Particles Chart of Elementary Particles Better Chart! Better Chart! As of today: Oscillation of 3 massive active neutrinos is clearly the dominant effect: If neutrinos have mass: For
More informationStudies of the XENON100 Electromagnetic Background
Studies of the XENON100 Electromagnetic Background Daniel Mayani Physik-Institut University of Zurich PhD Seminar PSI, August 26-27, 2015 Searching for elusive particles The main challenge for experiments
More informationSearch for Dark Matter with Liquid Argon and Pulse Shape Discrimination
Search for Dark Matter with Liquid Argon and Pulse Shape Discrimination Results from DEAP-1 and Status of DEAP-3600 Pierre Gorel for the DEAP collaboration University of Alberta Dark matter Experiment
More information14-th Lomonosov conference on elementary particle physics Moscow, August 19-25,2009 BNO INR V.N. Gavrin. The Solar Neutrinos
14-th Lomonosov conference on elementary particle physics Moscow, August 19-25,2009 BNO INR V.N. Gavrin The Solar Neutrinos 14-th Lomonosov conference on elementary particle physics Moscow, August 19-25,2009
More informationThe Double Chooz reactor neutrino experiment
The Double Chooz reactor neutrino experiment Christian Buck, MPIK Heidelberg MPIK July, 30th 2009 Overview Motivation Double Chooz concept and design Status of experiment MPIK activities Summary Neutrino
More informationRecent results from Super-Kamiokande
Recent results from Super-Kamiokande ~ atmospheric neutrino ~ Yoshinari Hayato ( Kamioka, ICRR, U-Tokyo ) for the Super-Kamiokande collaboration 1 41.4m Super-Kamiokande detector 50000 tons Ring imaging
More information1. Neutrino Oscillations
Neutrino oscillations and masses 1. Neutrino oscillations 2. Atmospheric neutrinos 3. Solar neutrinos, MSW effect 4. Reactor neutrinos 5. Accelerator neutrinos 6. Neutrino masses, double beta decay 1.
More informationPast, Present, and Future of Solar Neutrino Physics
Past, Present, and Future of Solar Neutrino Physics A.B. Balantekin University of Wisconsin SMU ebubble Workshop January 22, 2008 ...to see into the interior of a star and thus verify directly the hypothesis
More informationMINOS. Luke A. Corwin, for MINOS Collaboration Indiana University XIV International Workshop On Neutrino Telescopes 2011 March 15
MINOS Luke A. Corwin, for MINOS Collaboration Indiana University XIV International Workshop On Neutrino Telescopes 2011 March 15 2 Overview and Current Status Beam Detectors Analyses Neutrino Charged Current
More informationNeutrino Oscillations
Neutrino Oscillations Elisa Bernardini Deutsches Elektronen-Synchrotron DESY (Zeuthen) Suggested reading: C. Giunti and C.W. Kim, Fundamentals of Neutrino Physics and Astrophysics, Oxford University Press
More informationMuons in Borexino. SFB Block Meeting. Daniel Bick Universität Hamburg. D. Bick (Uni HH) Muons in Borexino
Muons in Borexino SFB Block Meeting Daniel Bick Universität Hamburg 24.03.2010 D. Bick (Uni HH) Muons in Borexino 24.03.2010 1 / 30 Overview 1 Motivation Physics at Borexino Neutrino Detection in Liquid
More informationNeutrino Oscillation: Non-Accelerator Experiments
Neutrino Oscillation: Non-Accelerator Experiments Yifang Wang 1 Institute of High Energy Physics Yu-Quan Road 19B, Beijing, 100049, P.R. China E-mail: yfwang@ihep.ac.cn In recent years, major advances
More informationSolar Neutrinos & MSW Effect. Pouya Bakhti General Seminar Course Nov IPM
Solar Neutrinos & MSW Effect Pouya Bakhti General Seminar Course Nov. 2012 - IPM Outline Introduction Neutrino Oscillation Solar Neutrinos Solar Neutrino Experiments Conclusions Summary Introduction Introduction
More informationSuper-Kamiokande ~The Status of n Oscillation ~
May 26, 2006 Vulcano Workshop 2006 Super-Kamiokande ~The Status of n Oscillation ~ Yoshihisa OBAYASHI (ICRR, Univ. of Tokyo) for Super-Kamiokande Collaboration May 26, 2006 Y.Obayashi @ Vulcano 2006 1
More informationNeutrino Physics: Lecture 1
Neutrino Physics: Lecture 1 Overview: discoveries, current status, future Amol Dighe Department of Theoretical Physics Tata Institute of Fundamental Research Feb 1, 2010 Plan of the course Omnipresent
More informationreνolution Three Neutrino Oscillation Lecture Two Lindley Winslow Massachusetts Institute of Technology
reνolution Three Neutrino Oscillation Lecture Two Lindley Winslow Massachusetts Institute of Technology 1 The neutrino is neutral. The neutrino only interacts weakly. The neutrino has a small non-zero
More informationLow Energy 8 B Solar Neutrinos in SNO+: Controlling and Constraining Radon Backgrounds
Low Energy 8 B Solar Neutrinos in SNO+: Controlling and Constraining Radon Backgrounds by Maryam Seddighin A thesis submitted to the Department of Physics, Engineering Physics and Astronomy in conformity
More informationarxiv: v1 [physics.ins-det] 3 Feb 2011
Nuclear Instruments and Methods in Physics Research A 00 (2018) 1 5 Alogo.pdf Nuclear Instruments and Methods in Physics Research A Scintillation decay time and pulse shape discrimination in oxygenated
More informationBackground Characterization and Rejection in the LZ Detector. David Malling Brown University IDM 2012 July 25, 2012
Background Characterization and Rejection in the LZ Detector David Malling Brown University IDM 2012 July 25, 2012 LZ Construction 2 Background Sources Ti cryostats 1500 kg
More informationNeutrino Masses and Mixing
Neutrino Masses and Mixing < Why so different??? (Harrison, Perkins, Scott 1999) The Mass Puzzle Seesaw mechanism L R m m D m 2 D M m D M m D L R M Heavy Majorana Neutrino Connection with high mass scales
More informationDaya Bay Neutrino Experiment
Daya Bay Neutrino Experiment Jun Cao Institute of High Energy Physics, Beijing 3rd International Conference on Flavor Physics, Oct. 3-8, 2005 National Central University Chung-li, Taiwan Neutrino Oscillation
More informationTHE BEGINNING OF THE END OF AN ERA: Analysis After the Shutdown of the Sudbury Neutrino Observatory
THE BEGINNING OF THE END OF AN ERA: Analysis After the Shutdown of the Sudbury Neutrino Observatory Introduction Highlights of SNO Results NCD Phase Update Future Analysis Plan Keith Rielage on behalf
More informationNeutrinos: Yesterday, Today and Tomorrow. Stanley Wojcicki SLAC Summer Institute 2010 August 13, 2010
Neutrinos: Yesterday, Today and Tomorrow August 13, 2010 1 My Marching Orders 2 My Marching Orders...the summary talk should be visionary, rather than a dedicated summary of the SSI program. 2 My Marching
More information( Some of the ) Lateset results from Super-Kamiokande
1 ( Some of the ) Lateset results from Super-Kamiokande Yoshinari Hayato ( Kamioka, ICRR ) for the SK collaboration 1. About Super-Kamiokande 2. Solar neutrino studies in SK 3. Atmospheric neutrino studies
More informationLow Background Experiments and Material Assay. Tessa Johnson NSSC Summer School July 2016
Low Background Experiments and Material Assay Tessa Johnson NSSC Summer School July 2016 Outline How do we detect particles? Some interesting questions relating to particle physics How can particle detection
More informationSterile Neutrinos with WbLS! detector. Jelena Maricic! University of Hawaii at Manoa! May 17, 2014
Sterile Neutrinos with WbLS detector Jelena Maricic University of Hawaii at Manoa May 17, 2014 Outline Physics motivation for the very short baseline neutrino oscillations search Concept of the antineutrino
More informationThe Daya Bay Reactor Neutrino Experiment
The Daya Bay Reactor Neutrino Experiment Ming-chung Chu The Chinese University of Hong Kong, Hong Kong On behalf of the Daya Bay Collaboration Partial support: CUHK VC Discretionary Fund, RGC CUHK3/CRF/10R
More informationPurification of Liquid Scintillator and Monte Carlo Simulations of Relevant Internal Backgrounds in SNO+
Purification of Liquid Scintillator and Monte Carlo Simulations of Relevant Internal Backgrounds in SNO+ by Sarah Elizabeth Quirk A thesis submitted to the Department of Physics, Engineering Physics and
More informationLow Energy Neutrino Astronomy and Results from BOREXINO
Low Energy Neutrino Astronomy and Results from BOREXINO DESY Hamburg / DESY Zeuthen March 25 th and 26th Lothar Oberauer, Physikdepartment E15, TU München Charge 0-1 +2/3-1/3 Neutrinos as probes? Neutrinos
More informationDetection of MeV scale neutrinos and the solar energy paradigm
Journal of Physics: Conference Series PAPER OPEN ACCESS Detection of MeV scale neutrinos and the solar energy paradigm To cite this article: Aldo Ianni 2018 J. Phys.: Conf. Ser. 940 012023 View the article
More informationRecent results from Borexino. Sandra Zavatarelli, INFN Genoa (Italy) on behalf of the Borexino Collaboration
Recent results from Borexino Sandra Zavatarelli, INFN Genoa (Italy) on behalf of the Borexino Collaboration Borexino physics! Data-taking since May 2007 : many relevant results on solar/geo ν physics and
More informationDaya Bay Neutrino Experiment NUFACT05. Jun Cao. Institute of High Energy Physics, Beijing
Daya Bay Neutrino Experiment Jun Cao Institute of High Energy Physics, Beijing NUFACT05 7th International Workshop on Neutrino Factories and Superbeams Laboratori Nazionali di Frascati, Frascati (Rome)
More informationFIRST RESULT FROM KamLAND-Zen Double Beta Decay with 136 Xe
FIRST RESULT FROM KamLAND-Zen Double Beta Decay with Xe A. GANDO for the KamLAND-Zen Collaboration Research Center for Neutrino Science, Tohoku University, Sendai 980-8578, Japan We present the first result
More informationAstroparticle physics
Timo Enqvist University of Oulu Oulu Southern institute lecture cource on Astroparticle physics 15.09.2009 15.12.2009 B. Lecture Contents Astroparticle physics: topics and tentative schedule high-energy
More informationBackground rejection techniques in Germanium 0νββ-decay experiments. ν=v
Background rejection techniques in Germanium 0νββ-decay experiments n p ν=v n eep II. Physikalisches Institut Universität Göttingen Institutsseminar des Inst. für Kern- und Teilchenphysik, Outline Neutrinos
More informationObservation of Reactor Electron Antineutrino Disappearance & Future Prospect
Observation of Reactor Electron Antineutrino Disappearance & Future Prospect Soo-Bong Kim (KNRC, Seoul National University) at Kyungpook National Univ., November 1, 01 Birth of Neutrino Physics in trouble
More informationSearch for double electron capture on 124 Xe with the XMASS-I detector
Search for double electron capture on 124 Xe with the XMASS-I detector KATSUKI HIRAIDE (ICRR, THE UNIVERSITY OF TOKYO) SEPTEMBER 7 TH, 2015 TAUP2015 1 124 Xe 2n double electron capture Natural xenon contains
More informationThe Double Chooz Project
The Double Chooz Project Progress and Expected Sensitivity David McKee, KSU 13 17 July 2009 TeVPA @ SLAC Outline I. Neutrino mixing and θ 13 II. Existing θ 13 measurements III. This is hard with a single
More informationNeutrino Oscillations
Neutrino Oscillations Supervisor: Kai Schweda 5/18/2009 Johannes Stiller 1 Outline The Standard (Solar) Model Detecting Neutrinos The Solar Neutrino Problem Neutrino Oscillations Neutrino Interactions
More informationAn Underground Laboratory for a Multi-Detector Experiment. Karsten Heeger Lawrence Berkeley National Laboratory
Measuring sin 2 2θ 13 with Reactor Antineutrinos at Daya Bay An Underground Laboratory for a Multi-Detector Experiment Karsten Heeger Lawrence Berkeley National Laboratory On behalf of the Daya Bay collaboration
More informationUNIT1: Experimental Evidences of Neutrino Oscillation Atmospheric and Solar Neutrinos
UNIT1: Experimental Evidences of Neutrino Oscillation Atmospheric and Solar Neutrinos Stefania Ricciardi HEP PostGraduate Lectures 2016 University of London 1 Neutrino Sources Artificial: nuclear reactors
More informationNeutrino oscillation physics potential of Hyper-Kamiokande
Neutrino oscillation physics potential of Hyper-Kamiokande on behalf of the Hyper-Kamiokande Collaboration Queen Mary University of London E-mail: l.cremonesi@qmul.ac.uk Hyper-Kamiokande (Hyper-K) is a
More informationPrecision Measurement of the Low Energy Solar Neutrino Spectrum with the LENS Experiment Mark Pitt * Virginia Tech for the LENS Collaboration
Precision Measurement of the Low Energy Solar Neutrino Spectrum with the LENS Experiment Mark Pitt * Virginia Tech for the LENS Collaboration 2009 Meeting of the Division of Particles and Fields of the
More informationA multipurpose detector for low energy
A multipurpose detector for low energy neutrino physics: Teresa Marrodán Undagoitia tmarroda@ph.tum.de Institut E15 Physik-Department Technische Universität München DPG Teilchenphysik Heidelberg, 09.03.07
More information章飞虹 ZHANG FeiHong INTERNATIONAL SCHOOL OF SUBNUCLEAR PHYSICS Ph.D. student from Institute of High Energy Physics, Beijing
章飞虹 ZHANG FeiHong zhangfh@ihep.ac.cn Ph.D. student from Institute of High Energy Physics, Beijing INTERNATIONAL SCHOOL OF SUBNUCLEAR PHYSICS 2012 Erice, 23 June 2 July 2012 1 Before Hunting Introduction
More informationGadolinium Doped Water Cherenkov Detectors
Gadolinium Doped Water Cherenkov Detectors David Hadley University of Warwick NuInt-UK Workshop 20th July 2015 Water Cherenkov Detector Super-Kamiokande 22.5 kt fiducial mass 2 Physics with Large Scale
More informationarxiv: v1 [hep-ex] 22 Nov 2012
PRAMANA journal of physics Indian Academy of Sciences Low Energy Neutrino Measurements arxiv:1211.5359v1 [hep-ex] 22 Nov 2012 DAVIDE D ANGELO a, a Università degli Studi di Milano e I.N.F.N. sez. di Milano
More informationarxiv:hep-ex/ v1 15 Aug 2006
The Double Chooz Experiment 1 Daniel M. Kaplan (for the Double Chooz Collaboration) Illinois Institute of Technology, 3101 South Dearborn Street, Chicago, Illinois, USA arxiv:hep-ex/0608040v1 15 Aug 2006
More informationJelena Maricic Drexel University. For Double Chooz Collaboration. Spain. France. Germany U.S.A. Japan Russia. Brazil U.K. Courtesy of T.
Jelena Maricic Drexel University For Double Chooz Collaboration France Spain Germany U.S.A Japan Russia Brazil U.K. http://doublechooz.in2p3.fr/ J. Maricic, Drexel U 1 Courtesy of T. Lasserre ν e ν μ ν
More informationNeutrinoless Double Beta Decay for Particle Physicists
Neutrinoless Double Beta Decay for Particle Physicists GK PhD Presentation Björn Lehnert Institut für Kern- und Teilchenphysik Berlin, 04/10/2011 About this talk Double beta decay: Particle physics implications
More information