LoNu Workshop R. B. Vogelaar October 14, 2006 Extraordinary Neutrino Beam Free of Charge For NEUTRINO PHYSICS: WELL DEFINED HIGHEST FLUX (~10 11 cm -2.

Slides:

Advertisements

Similar presentations

The SNO+ Experiment: Overview and Status

Advertisements

Neutrinos Louvain, February 2005 Alan Martin Arguably the most fascinating of the elementary particles. Certainly they take us beyond the Standard Model.

Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%

DMSAG 14/8/06 Mark Boulay Towards Dark Matter with DEAP at SNOLAB Mark Boulay Canada Research Chair in Particle Astrophysics Queen’s University DEAP-1:

Source Neutrino Experiments

Stockholm, May 2-6, 2006 SNOW Sub-MeV solar neutrinos: experimental techniques and backgrounds Aldo Ianni Gran Sasso Laboratory, INFN.

Zone convective 2e - +4p 4 He+2 e  MeV coeur zone radiative 500'000 km (70% 1 H, 28% 4 He,...) e L= m. Le soleil.

Neutrino Physics - Lecture 5 Steve Elliott LANL Staff Member UNM Adjunct Professor ,

Prospects for 7 Be Solar Neutrino Detection with KamLAND Stanford University Department of Physics Kazumi Ishii.

CP-phase dependence of neutrino oscillation probability in matter 梅 (ume) 田 (da) 義 (yoshi) 章 (aki) with Lin Guey-Lin ( 林貴林 ) National Chiao-Tung University.

The XENON Project A 1 tonne Liquid Xenon experiment for a sensitive Dark Matter Search Elena Aprile Columbia University.

Solar & Atmospheric. June 2005Steve Elliott, NPSS Outline Neutrinos from the Sun The neutrinos Past experiments What we know and what we want to.

8/5/2002Ulrich Heintz - Quarknet neutrino puzzles Ulrich Heintz Boston University

No s is good s Sheffield Physoc 21/04/2005 Jeanne Wilson A historical introduction to neutrinoless double beta decay.

Potassium Geo-neutrino Detection Mark Chen Queen’s University Neutrino Geophysics, Honolulu, Hawaii December 15, 2005.

Neutrino emission =0.27 MeV E=0.39,0.86 MeV =6.74 MeV ppI loss: ~2% ppII loss: 4% note: /Q= 0.27/26.73 = 1% ppIII loss: 28% Total loss: 2.3%

Neutrino Physics - Lecture 4 Steve Elliott LANL Staff Member UNM Adjunct Professor ,

The Importance of Low-Energy Solar Neutrino Experiments Thomas Bowles Los Alamos National Laboratory Markov Symposium Institute for Nuclear Research 5/13/05.

Neutrinos as Probes: Solar-, Geo-, Supernova neutrinos; Laguna

Aldo IanniNNN05 April 8, Status and future prospects of Gran Sasso Aldo Ianni INFN Gran Sasso Laboratory NNN05 Aussois, April 7-9.

Neutrino Working Group Kevin T. Lesko  12 Neutrino Mixing  Next Generation Solar Neutrino Experiments  National Underground Scientific Laboratory.

SNO+ Mark Chen Queen’s University Neutrino Geophysics, Honolulu, Hawaii December 15, 2005.

I. Giomataris NOSTOS Neutrino studies with a tritium source Neutrino Oscillations with triton neutrinos The concept of a spherical TPC Measurement of.

Solar Neutrinos Perspectives and Objectives Mark Chen Queen’s University and Canadian Institute for Advanced Research (CIFAR)

The Elementary Particles. e−e− e−e− γγ u u γ d d The Basic Interactions of Particles g u, d W+W+ u d Z0Z0 ν ν Z0Z0 e−e− e−e− Z0Z0 e−e− νeνe W+W+ Electromagnetic.

Latest SNO Results from Salt-Phase Data and Current NCD-Phase Status Melin Huang ● Introduction ● Results of Salt Phase (Phase II) ● Status of NCD Phase.

Solar neutrino measurement at Super Kamiokande ICHEP'04 ICRR K.Ishihara for SK collaboration Super Kamiokande detector Result from SK-I Status of SK-II.

J.T. White Texas A&M University SIGN (Scintillation and Ionization in Gaseous Neon) A High-Pressure, Room-Temperature, Gaseous-Neon- Based Underground.

Status of the BOREXINO experiment Hardy Simgen Max-Planck-Institut für Kernphysik / Heidelberg for the BOREXINO collaboration.

Methods and problems in low energy neutrino experiments (solar, reactors, geo-) I G. Ranucci ISAPP 2011 International School on Astroparticle physics THE.

A large water shield for dark matter, double beta decay and low background screening. T. Shutt - Case R. Gaitskell - Brown.

Moscow, 15/10/2005 Aldo Ianni, INFN LNGS 1 Borexino and status of the project Aldo Ianni INFN, Gran Sasso Laboratory on behalf of the Borexino collaboration.

Context: astroparticle physics, non-accelerator physics, low energy physics, natural sources physics, let’s-understand-the-Universe physics mainly looking.

DEAP Part I: Andrew Hime (Los Alamos National Laboratory) DEAP Concept DEAP-0 Test-Results & Requirements of a DEAP Program Synergy with CLEAN Program.

Present and future detectors for Geo-neutrinos: Borexino and LENA Applied Antineutrino Physics Workshop APC, Paris, Dec L. Oberauer, TU München.

Wednesday, Feb. 14, 2007PHYS 5326, Spring 2007 Jae Yu 1 PHYS 5326 – Lecture #6 Wednesday, Feb. 14, 2007 Dr. Jae Yu 1.Neutrino Oscillation Formalism 2.Neutrino.

J.T. White Texas A&M University SIGN (Scintillation and Ionization in Gaseous Neon) A High-Pressure, Room- Temperature, Gaseous-Neon-Based Underground.

XMASS experiment Current status 10 th ICEPP Symposium in Hakuba 16 Feb 2004 Yohei Ashie ICRR Univ.of Tokyo.

SNO Liquid Scintillator Project NOW September 2004 Mark Chen Queen’s University & The Canadian Institute for Advanced Research.

Kr2Det: TWO - DETECTOR REACTOR NEUTRINO OSCILLATION EXPERIMENT AT KRASNOYARSK UNDERGROUND SITE L. Mikaelyan for KURCHATOV INSTITUTE NEUTRINO GROUP.

SNO and the new SNOLAB SNO: Heavy Water Phase Complete Status of SNOLAB Future experiments at SNOLAB: (Dark Matter, Double beta, Solar, geo-, supernova.

A. IanniIFAE, Catania Mar. 30, Solar neutrinos: present and future Aldo Ianni INFN, Gran Sasso Laboratory.

in Beijing August 18, 2004 Recent status of the XMASS project Physics goals at XMASS Overview of XMASS Current status of R&D Summary.

New Results from the Salt Phase of SNO Kathryn Miknaitis Center for Experimental Nuclear Physics and Astrophysics, Univ. of Washington For the Sudbury.

TUNL R. B. Vogelaar March 1, 2007 Measuring the complete Solar neutrino spectrum E th =114 keV (95% of pp spectrum) Measure pp- 3% Determine CNO-fraction.

Data Processing for the Sudbury Neutrino Observatory Aksel Hallin Queen’s, October 2006.

Neutrinos from the sun, earth and SN’s: a brief excursion Aldo IFAE 2006 Pavia April 19 th.

Masatoshi Koshiba Raymond Davis Jr. The Nobel Prize in Physics 2002 "for pioneering contributions to astrophysics, in particular for the detection of cosmic.

CTF at Gran Sasso (overview of the hardware) Richard Ford (SNOLAB) (who has not been in the collaboration since 2004) March 19 th 2010.

Search for Sterile Neutrino Oscillations with MiniBooNE

Davide Franco – NOW C measurement and the CNO and pep fluxes in Borexino Davide Franco NOW2004 Conca Specchiulla September 2004.

Current status of XMASS experiment 11 th International Workshop on Low Temperature Detectors (LTD-11) Takeda Hall, University of Tokyo, JAPAN 8/1, 2005.

Solar Neutrino Results from SNO

1 Status and background considerations of XMASS experiment Yeongduk Kim Sejong University for the XMASS collaboration LRT2006 Oct. 3, 2006.

Results from Borexino Davide Franco CNRS-APC NOW 2012 September 9-16, 2012.

Second Workshop on large TPC for low energy rare event detection, Paris, December 21 st, 2004.

5th June 2003, NuFact03 Kengo Nakamura1 Solar neutrino results, KamLAND & prospects Solar Neutrino History Solar.

Center for Neutrino Physics Source Neutrino Experiments Jonathan Link Center for Neutrino Physics Virginia Tech NuFact 2016.

News from the Sudbury Neutrino Observatory Simon JM Peeters July 2007 o SNO overview o Results phases I & II o hep neutrinos and DSNB o Update on the III.

DPF-JPS 2006 Oct 31, Hawaii 1 CANDLES system for the study of 48-Ca double beta decay T. Kishimoto Osaka Univ.

Aldo Ianni for the Borexino collaboration 12th International Workshop on Next Generation Nucleon Decay and Neutrino Detectors Zurich, 7 th Nov 2011.

Solar neutrino physics The core of the Sun reaches temperatures of  15.5 million K. At these temperatures, nuclear fusion can occur which transforms 4.

Low energy underground experimentation with a TPC G

XAX Can DM and DBD detectors combined?

Solar Neutrino Problem

“Solar” Neutrino Oscillations (Dm2, q12)

Signal and Background in LENS

Solar neutrinos: form their production to their detection

Davide Franco for the Borexino Collaboration Milano University & INFN

DUNE as the Next-Generation Solar Neutrino Experiment

Presentation transcript:

LoNu Workshop R. B. Vogelaar October 14, 2006 Extraordinary Neutrino Beam Free of Charge For NEUTRINO PHYSICS: WELL DEFINED HIGHEST FLUX (~10 11 cm -2 s -1 ) PURE FLAVOR SOURCE - ν e only LONGEST BASELINE (10 8 km) HIGH DENSITY UP TO 160 g/cm 3 ; ~ g/cm 2 path LOWEST ENERGIES (keV to MeV) PRESENCE OF HIGH MAGNETIC FIELDS FULL SPECTRUM: ENERGY DEPENDENT EFFECTS Best tools for investigating neutrino flavor phenomena in Vacuum and in Matter For ASTROPHYSICS Best tool for unprecedented look at how a real Star works - in the past, present and future SOLAR NEUTRINOS

LoNu Workshop R. B. Vogelaar October 14, 2006 Solar Neutrinos

LoNu Workshop R. B. Vogelaar October 14, 2006

Solar Neutrinos CC NC Elastic

LoNu Workshop R. B. Vogelaar October 14, 2006 Solar Neutrinos nucl-ex/

LoNu Workshop R. B. Vogelaar October 14, 2006 Summary Experimentmono-energetic response Solar Sensitivity %pp 5 yr % 7 Be 5 yr Status Borexino 7 Be, pep?5results in a few years KamLAND 7 Be, CNO?5results in a few years LENS pp  CNO 35ready to prototype MOON pp  CNO r&d only (for now) CLEAN pp  7 Be 1 < 3ready to prototype HERON pp  7 Be 1.55r&d only (for now) TPC ? pp  7 Be r&d XMasspp, 7 Be100 kg prototype SNO+ 7 Be, pep1.5(pep)TDR Fall 06, construct 07

LoNu Workshop R. B. Vogelaar October 14, 2006 Measuring the 7 Be flux (elastic scattering) Borexino KamLAND 100 ton FV scintillator measure 7 Be flux to 5% g/g U,Th eq 95% psd 90% ce perhaps see pep? above, plus: g/g 11 C tagged to be filled in 2006 ~ 4x g/g; 210 Pb challenge NSF support for US groups

LoNu Workshop R. B. Vogelaar October 14, 2006 Borexino KamLAND Measuring the 7 Be flux (elastic scattering) 300 ton FV scintillator 210 Pb bkgd challenge purification to start Sept 06 need ~ 10 5 reduction

LoNu Workshop R. B. Vogelaar October 14, 2006 pp 7 Be In(   ) 7 Be * pep 15 N 15 O LENS Solar Neutrino Spectrum Measuring the pp- flux – charged current E th =114 keV (95% of pp spectrum) Measure pp- 3% Determine CNO-fraction Measure T sun by change in mean energy of 7 Be line – maybe (hep-ph/ ) needs separate calibration experiment LENS Moon

LoNu Workshop R. B. Vogelaar October 14, 2006 Measuring the pp- flux – charged current LENS Moon 100 Mo( e,e  ) 100 Tc(   )t 1/2 =15.8s E th =168 keV (85% of pp spectrum) 30 tons natural Mo 360 ’s yr  1 one of three design options shown

LoNu Workshop R. B. Vogelaar October 14, 2006 elastic scattering experiments (NC & CC) complementary use: look for Dark Matter Measuring the pp- flux – elastic scattering CLEAN Heron TPC XMass SNO+ 10 ton FV of liquid Ne 20 keV threshold 4 pe / keV absence of long-lived isotopes; density of 1.2 g/cm3; $60k/ton Ne 1% measurement of pp and 7 Be solar neutrinos “mini-CLEAN”

LoNu Workshop R. B. Vogelaar October 14, 2006 Measuring the pp- flux – elastic scattering CLEAN Heron TPC XMass SNO+ PP flux should be determined to <1.5% (one sigma) 7 Be flux should be determined to <5% (one sigma) Some sensitivity to annual total flux variation due to solar orbit  Total Helium mass 22 tonnes at 50mK.  No internal backgnd (superfluid self-cleaning).  Scintillation/rotons or Scintillation/e-bubbles.  Scintillation: 35% of E e into 16 eV UV ( Rayl. > 200 meter; self-transparent;  =1.04).  Detection:2400 wafer calorimeters above liquid.  Event location: coded aperture array; few cm.).  2.5 evts/(day-tonne) LMA (pp+Be) E e > 45 keV.  Helium immune to muon spallation/capture.

LoNu Workshop R. B. Vogelaar October 14, 2006 CLEAN Heron TPC XMass SNO+ Measuring the pp- flux – elastic scattering 10 atm  target mass 7 tons 14m diam x 20 m length Use e  recoil direction to determine incident energy

LoNu Workshop R. B. Vogelaar October 14, 2006 CLEAN Heron TPC XMass SNO+ Measuring the pp- flux – elastic scattering

LoNu Workshop R. B. Vogelaar October 14, 2006 CLEAN Heron TPC XMass SNO+ Measuring the pep- flux – elastic scattering 12 m diameter Acrylic Vessel 18 m diameter support structure; 9500 PMTs (~60% photocathode coverage) 1700 tonnes inner shielding H 2 O 5300 tonnes outer shielding H 2 O Urylon liner radon seal depth: 2092 m (~6010 m.w.e.) ~70 muons/day Scintillator: Linear Alkylbenzene compatible with acrylic high flash point 130 °C low toxicity cheap, (common feedstock for LAS detergent) plant in Quebec makes 120 kton/year 1.5% pep – depth means 11 C bkgd low