Neutrino observatories
|
|
- Darrell Cross
- 5 years ago
- Views:
Transcription
1 Gravitational-wave Physics&Astronomy Workshop, January 28, 2011 Neutrino observatories M.Nakahata Kamioka observatory ICRR/IPMU, Univ. of Tokyo SN1987A
2 Contents Supernova burst neutrinos How they are produced SN1987A Current detectors in the world What information neutrino detectors can provide High energy astrophysical neutrinos How they are produced Detectors in the world
3 Core-collapse supernova Standard scenario of the core-collapse supernova Core-collapse Neutrino trapping Core bounce H He C+O Si Fe n n n n n n n Supernova burst Shock wave propagation Shock wave at core n Neutron star Figure from K.Sato n n n n
4 Neutrino emission from supernova burst Released gravitational energy: ~3x10 53 erg Neutrinos carry almost all (99%) of the energy. Energy for explosion and optical emission is only ~1%(~10 51 erg). Expected time profile Livermore simulation (x=m,t) Mean neutrino energy (x=m,t) T.Totani, K.Sato, H.E.Dalhed and J.R.Wilson, ApJ.496,216(1998)
5 Total Binding Energy SN1987A: supernova at LMC(50kpc) Kamiokande-II IMB-3 BAKSAN Feb.23, 1987 at 7:35UT Kam-II (11 evts.) IMB-3 (8 evts.) Baksan (5 evts.) 24 events total 95 % CL Contours Theory from G.Raffelt _ Spectral n e Temperature
6 Supernova burst detectors in the world (running and near future experiments) Borexino LVD Super-Kamiokande Baksan SNO+ (under construction) HALO KamLAND IceCube
7 The Baksan underground scintillation telescope (Russia) E.N.Alexeyev, L.N.Alexeyeva, astro-ph/ Total number of standard detectors Total target mass tons of oil-based scintillator ~100 n e p e + n events expected for 10 kpc SN. Running since 1980 with ~90% live time. From E.N.Alexeyev
8 LVD detector LVD consists of an array of 840 counters, 1.5 m 3 each. Total target: 1000 t liquid scintillator 4MeV threshold With <1MeV threshold for delayed signal (neutron tagging efficiency of %) E resolution: 13%(1s) at 15MeV ~300 n e p e + n events expected for 10 kpc SN. Twenty From W.Flugione Years after SN1987A At Gran Sasso Fulgione@to.infn.it Lab., Italy
9 Single volume liquid scintillator detectors KamLAND Borexino SNO+ (Kamioka, Japan) (Gran Sasso, Italy) (SNO Lab.,Canada) 300ton liq.sci. Running since ton liq.sci. Running since ton liq.sci. Under construction. From K.Inoue, G.Bellini, M.Chen
10 Liquid scinitillator detectors Expected number of events(for 10kpc SN) Events/1000 tons Inverse beta( n e +p e + +n) : ~300 events Spectrum measurement with good energy resolution, e.g. for spectrum distortion of earth matter effect. CC on 12 C (n e + 12 C e+ 12 N( 12 B)) : Tagged by 12 N( 12 B) beta decay Electron scattering (n+e - n+e - ) : NC g from 12 C (n+ 12 C n+ 12 C+g): Total neutrino flux, 15.11MeV mono-energetic gamma n+p scattering( n+p n+p): Sensitive to all types of neutrinos. (Independent from neutrino oscillation) Spectrum measurement of higher energy component. ~30 events ~20 events ~60 events ~300 events From K.Inoue, G.Bellini, M.Chen
11 HALO - a Helium and Lead Observatory (SNO Lab., Canada) SNO 3 He neutron detectors with lead target CC: NC: HALO-1 is using an available 76 tonnes of Pb In HALO-1 for a 10kpc, Assuming FD distribution with T=8 MeV for n μ s, n τ s. 65 neutrons through n e charged current channels 20 neutrons through ν x neutral current channels ~ 85 neutrons liberated; with ~50% of detection efficiency, ~40 events expected. HALO-2 is a future kt-scale detector From C.Virtue
12 IceCube: The Giga-ton Detector Array IceTop Design Specifications (South pole) InIce AMANDA Fully digital detector concept Number of strings 75 Number of surface tanks 160 Number of Optical modules (DOMs) 4820 Instrumented volume 1 km 3 Supernova neutrinos coherently increase single rates of PMTs. Construction finished on Dec.18, From L.Koepke, S.Yoshida
13 IceCube as MeV n detector 10 kpc to SN Simulation based on Livermore model Advantage: high statistics (0.75% stat. 0.5s and 100ms bins) Good for fine time structures (noise low)! Disadvantage: no pointing no energy intrinsic noise Galactic Center IceCube Amanda LMC SMC Significance: Galactic center: ~200 s LMC : ~5 s SMC : ~4 s From L.Koepke
14 Super-Kamiokande detector (Kamioka, Japan) LINAC 41.4m Electronics hut ID OD 39.3m Water and air purification system Control room Ikeno-yama Kamioka-cho, Gifu Japan Mozumi 3km SK Atotsu entrance 1km (2700mwe) 2km Atotsu 50,000 ton water 32,000 ton photosensitive volume ~2m OD viewed by inch PMTs 32kt ID viewed by 11, inch PMTs 22.5kt fid. vol. (2m from wall) ~4.5MeV energy threshold SK-I: April 1996~ SK-IV is running
15 Super-K: Expected number of events Neutrino flux and energy spectrum from Livermore simulation (T.Totani, K.Sato, H.E.Dalhed and J.R.Wilson, ApJ.496,216(1998)) ~7,300 n e +p events ~300 n+e events ~ O NC g events ~ O CC events (with 5MeV thr.) for 10 kpc supernova
16 Summary of current supernova n detectors # of events expected for 10kpc. Directionality Baksan (1980-) LVD (1992-) Super-K (1996-) KamLAND (2002-) ICECUBE (2005-) BOREXINO (2007-) HALO (2010-) 330 ton liquid scintillator ~100 n e p e + n events ton liquid scintillator. 840 counters 1.5m 3 each. 4 MeV thres., ~50% eff. for tagging decayed signal. ~300 n e p e + n events. 32,000 tons of water target. ~7300 n e p e + n, ~300 ne ne scattering events ton liquid scintillator, single volume. ~300 n e p, several 10 CC on 12 C, ~60 NC g, ~300 np np Gigaton ice target. By coherent increase of PMT single rates. High precision time structure measurement. 300 ton liquid scintillator, single volume. ~100 n e p, ~10 CC on 12 C, ~20 NC g, ~100 np np SNO 3 He neutron detectors with 76 ton lead target. ~40 events expected. No No Yes No No No No
17 Super-Kamiokande: Water Cherenkov detector Cherenkov light Emitted when particle travels faster than speed of light in water(c/1.33). e Emission angle = cos -1 (1/nb)=42 q Using hit PMT timing, vertex position is reconstructed. Then, direction is reconstructed using hit PMT pattern. One of the SN1987A events in Kamiokande
18 Neutrino interaction in water Cross section (H 2 O target) Angular distribution Supernova n ν+e - ν+e - ν e +p e + +n ν e + 16 O e F ν e + 16 O e N Neutrino COSq SN
19 Super-K: simulation of angular distribution n+e n+e SN at 10kpc ne+p ne+p n+e n+e ne+p ne+p Direction of supernova can be determined with an accuracy of ~5 degree. Neutrino flux and spectrum from Livermore simulation
20 Captures on Gd Future possible improvement in Super-K Identify n e p events by neutron tagging with Gadolinium. Gadolinium has large neutron capture cross section and emit 8MeV gamma cascade. n e p e + n Gd γ 100% 80% 0.1% Gd gives >90% efficiency for n capture In Super-K this means ~100 tons of water soluble GdCl 3 or Gd 2 (SO 4 ) 3 8 MeV ΔT~20μs Vertices within 50cm The main purpose of this project is to detect diffuse supernova neutrinos. 60% 40% 20% 0% % 0.001% 0.01% 0.1% 1% Gd in Water
21 Super-K: Angular distribution (with Gd) ne+p n+e ne+p n+e With n e p identification by neutron tagging ne+p n+e ne+p n+e Direction accuracy can be improved to ~3 degree. SN at 10kpc
22 Burst onset time Simulation of initial stage of a burst (10kpc supernova) Super-Kamiokande IceCube Halzen, Raffelt, arxiv: IceCube example 10~40 events in the first 20msec. ±3.5 msec at 95% C.L. Super-K and IceCube have a few msec precision on onset time.
23 Triangulation on supernova direction Beacom, Vogel, Phys.Rev.D60, , 1999 Super-K (36 N) cosq = t / d q IceCube (90 S) If Super-K and IceCube has ~2 msec rise time resolution, cos(q) = ~0.1 (i.e. about 25 deg.). Super-K resolution by electron-scattering is much better.
24 SuperNova Early Warning System snews.bnl.gov Details: arxiv:astro-ph/ Individual supernova-sensitive experiments send burst datagrams to SNEWS coincidence computer at Brookhaven National Lab(backup at U. of Bologna) alert to astronomers if coincidence in 10 seconds Participating experiments: arxiv: Super- Kamiokande (Japan) From K. Scholberg Large Volume Detector (Italy) IceCube (South Pole) SNO (Canada) until end of 2006
25 High Energy Astrophysical Neutrinos There are high energy accelerators in the universe. We know cosmic rays(p, He,..) exist. So, there much be cosmic high energy neutrinos. Possible sources: AGN, supernova remnants,. n e e + m + n m n m + g sync e - p g sync accretion disk Black hole
26 Cosmic Ultra High Energy neutrinos Ultra High Energy Cosmic Ray(UHECR) exists. Horizon of UHECR is ~50Mpc. Neutrinos galactic Extragalactic cosmic rays interact with the microwave background p g m n m } n e { e m e : n m : n t 1:1:1 GZK neutrinos m (due to n osc.)
27 Detectors for High Energy Astrophysical Neutrinos Antares Mediterranean sea 0.2x0.2x0.4km Volume: 0.01 km 3 Running since May 2008 South pole Volume:1 km 3 Construction finished in Dec.2010 NT200+ Lake Bikal 0.2 kmf 0.2 kmh Volume: 0.01 km 3 Running from 2006
28 n m only Diffuse n limit Now below the Waxman-Bahcall limit Atmospheric n IceCube Preliminary This work From S.Yoshida Sean Grullon (UW-Madison)
29 GZK n search All flavor (n e n m n t ) limits Systematic errors included IceCube Preliminary Aya Ishihara (Chiba) From S.Yoshida
30 Conclusions Supernova burst neutrinos Many detectors in the world with various types of signals. ~8,000 events expected at Super-K for 10kpc SN. High precision time profile by Icecube. ~5 deg. accuracy in direction of supernova by Super-K neutron-electron scattering events. Onset time with ~2 msec resolution by Super-K and IceCube. High energy neutrinos Construction of the IceCube was finished. High energy neutrino events are expected in near future.
31 Backups
32 Distance to Galactic supernova Mirizzi, Raffelt and Serpico, JCAP 0605,012(2006), astro-ph/ Based on birth location of neutron stars Type Ia Core collapse type mean: 10.7 kpc r.m.s.: 4.9 kpc 0 10kpc 20kpc 7% probability < 3.16 kpc > x10 statistics 16% probability < 5 kpc > x 4 statistics 3% probability > 20 kpc < 1/4 statistics
33 Super-K: Angular distribution (without Gd) ne+p n+e n+e Without n e p identification by neutron tagging ne+p n+e n+e ne+p ne+p SN at 10kpc
34 Accuracy of supernova direction with neutron tag Thomas, Sekikoz, Raffelt, Kachelriess, Dighe, hep-ph/ v2 Accuracy of SN direction with simulated supernova Tagging efficiency vs. accuracy (95% CL) Accuracy can be improved by a factor of two with neutron tagging. G: Garching model, L: Livermore model a: normal hierarchy sin 2 q 13 >10-3 b: inv. hierarchy sin 2 q 13 >10-3 c: any hierarchy sin 2 q 13 <10-3
35 COSq SN Angular distribution of ν e +p e + +n ν e +p e + + n neutrino energy 5MeV 10MeV 20MeV 30MeV A. Strumia and F. Vissani, Phys.Lett.B564:42-54,2003.
36 Super-K: Neutronization burst (e - +p n+n e ) SN at 10kpc Neutrino flux and spectrum from Livermore simulation Event rate of n e +p events Event rate of neutronization burst (forward peaked n+e scattering events) No oscillation Normal P H =1 or Inverted hierarchy Normal hierarchy P H =0 P H : crossing probability at H resonance (P H =0: adiabatic) Number of events from neutronization burst is 0.9~6 events for SN@10kpc. n e p events during this 10msec is about 8-30 events. N.H. +adiamacitc case: neutronization=0.9ev., n e p = 14 ev.(1.4 for SN direction).
37 n+p elastic signal( n+p n+p) at liq. Scintillator detectors Beacom, Farr, and Vogel, PRD66, (2002) Expected spectrum Sensitivity of temperature measurement n e n e ~300 events/kt above 200keV ~150 events/kt above 500keV Determine original n m, n m, n t, n t temperature with ~10% accuracy. (free from neutrino oscillation.) Current Borexino threshold: 200keV Current KamLAND threshold: 600~700keV(will be lowered after 2008 distillation.)
Detection of supernova Neutrinos
Supernovae Conference, Kyoto, October 3, 3 Detection of supernova Neutrinos M.Nakahata Kamioka observatory ICRR/IPMU, Univ. of Tokyo SN87A Contents Supernova burst neutrinos SN87A Current detectors in
More informationSupernova Neutrino Detectors: Current and Future. Kate Scholberg, Duke University June 24, 2005
Supernova Neutrino Detectors: Current and Future Kate Scholberg, Duke University June 24, 2005 OUTLINE Supernovae and the Neutrino Signal What We Will Learn Supernova Neutrino Detection Current SN ν Detectors
More informationNeutrino June 29 th Neutrino Probes of Extragalactic Supernovae. Shin ichiro Ando University of Tokyo
Neutrino Workshop@ICRR June 29 th 2005 Neutrino Probes of Extragalactic Supernovae Shin ichiro Ando University of Tokyo 1. Introduction Core-Collapse Supernova and Neutrino Burst Gravitational binding
More informationAstroparticle physics
Timo Enqvist University of Oulu Oulu Southern institute lecture cource on Astroparticle physics 15.09.2009 15.12.2009 Supernovae and supernova neutrinos 4.1 4 Supernovae and supernova neutrinos 4.1 Supernova
More informationIntroduction Core-collapse SN1987A Prospects Conclusions. Supernova neutrinos. Ane Anema. November 12, 2010
Supernova neutrinos Ane Anema November 12, 2010 Outline 1 Introduction 2 Core-collapse 3 SN1987A 4 Prospects 5 Conclusions Types of supernovae Figure: Classification (figure 15.1, Giunti) Supernova rates
More informationGADZOOKS! project at Super-Kamiokande
GADZOOKS! project at Super-Kamiokande M.Ikeda (Kamioka ICRR, U.of Tokyo) for Super-K collaboration 2015,6,9@WIN2015 Contents GADZOOKS! project Supernova Relic Neutrino search R&D status and Plan Summary
More informationSupernova Neutrinos in Future Liquid-Scintillator Detectors
Supernova Neutrinos in Future Liquid-Scintillator Detectors Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 9, China E-mail: liyufeng@ihep.ac.cn A high-statistics measurement of
More informationSupernova Neutrinos Supernova Neutrino Detection!
Supernova Neutrinos Supernova Neutrino Detection! Kate Scholberg, Duke University JINA-CEE International Symposium on Neutron Stars in the Multi-Messenger Era Athens, Ohio, May 2016 e e µ µ l Three flavors
More informationRecent results from Super-Kamiokande
Quarks to Universe in Computational Science, Nara, Japan, November 4th, 2015 Recent results from Super-Kamiokande M.Nakahata Kamioka Observatory, ICRR, Kavli IPMU, Univ. of Tokyo for Super-K collaboration
More informationFossil Records of Star Formation: John Beacom, The Ohio State University
Fossil Records of Star Formation: Supernova Neutrinos and Gamma Rays Basic Pitch Supernovae are of broad and fundamental interest Neutrinos and gamma rays are direct messengers Recent results show that
More informationSearching for Supernova Relic Neutrinos. Dr. Matthew Malek University of Birmingham HEP Seminar 11 May 2011
Searching for Supernova Relic Neutrinos Dr. Matthew Malek University of Birmingham HEP Seminar 11 May 2011 Outline Introduction: A Brief History of Neutrinos Theory Supernova Neutrino Emission Supernova
More informationC02: Investigation of Supernova Mechanism via Neutrinos. Mark Vagins Kavli IPMU, UTokyo
C02: Investigation of Supernova Mechanism via Neutrinos Mark Vagins Kavli IPMU, UTokyo GW Genesis 1 st Annual Symposium University of Tokyo, Kashiwa March 7, 2018 Supernova explosions play an absolutely
More informationIceCube. francis halzen. why would you want to build a a kilometer scale neutrino detector? IceCube: a cubic kilometer detector
IceCube francis halzen why would you want to build a a kilometer scale neutrino detector? IceCube: a cubic kilometer detector the discovery (and confirmation) of cosmic neutrinos from discovery to astronomy
More informationNeutrinos and Supernovae
Neutrinos and Supernovae Introduction, basic characteristics of a SN. Detection of SN neutrinos: How to determine, for all three flavors, the flux and temperatures. Other issues: Oscillations, neutronization
More informationGalactic Supernova for neutrino mixing and SN astrophysics
Galactic Supernova for neutrino mixing and SN astrophysics Amol Dighe Tata Institute of Fundamental Research Mumbai NNN05, Aussois, France, April 7-9, 2005 Galactic Supernova forneutrino mixing and SN
More informationMeasuring the neutrino mass hierarchy with atmospheric neutrinos in IceCube(-Gen2)
Measuring the neutrino mass hierarchy with atmospheric neutrinos in IceCube(-Gen2) Beyond the Standard Model with Neutrinos and Nuclear Physics Solvay Workshop November 30, 2017 Darren R Grant The atmospheric
More informationM.Nakahata. Kamioka observatory ICRR/IPMU, Univ. of Tokyo. 2016/11/8 M. Nakahata: Neutrino experiments - 30 years at Kamioka 1
Neutrino experiments -- 30 years at Kamioka -- M.Nakahata Kamioka observatory ICRR/IPMU, Univ. of Tokyo 2016/11/8 M. Nakahata: Neutrino experiments - 30 years at Kamioka 1 Contents Current experiments
More informationParticle Physics Beyond Laboratory Energies
Particle Physics Beyond Laboratory Energies Francis Halzen Wisconsin IceCube Particle Astrophysics Center Nature s accelerators have delivered the highest energy protons, photons and neutrinos closing
More informationIdentifying the neutrino mass hierarchy with supernova neutrinos
Identifying the neutrino mass hierarchy with supernova neutrinos Ricard Tomàs AHEP Group - Institut de Física Corpuscular (CSIC - Universitat de València) IPM School & Conference on Lepton & Hadron Physics
More informationNeutrino AstroPhysics
Nuclear Astrophysics 2003 / Neutrino AstroPhysics 1(44) Neutrino AstroPhysics Supernova Neutrino Detection title.tex Nuclear Astrophysics 2003 / Neutrino AstroPhysics 2(44) Content of the Lecture Intro:
More informationPhysics Potential of Future Supernova Neutrino Observations
Physics Potential of Future Supernova Neutrino Observations Amol Dighe Tata Institute of Fundamental Research Mumbai, India Neutrino 2008 May 25-31, 2008, Christchurch, New Zealand Supernova for neutrino
More informationUNO: Underground Nucleon Decay and Neutrino Observatory
UNO: Underground Nucleon Decay and Neutrino Observatory Clark McGrew NESS, Jan 2002 NESS 2002 McGrew p. 1 The UNO Concept Build on well-established techniques Explore broad range of physics Provide a general
More informationPROBING THE MASS HIERARCHY WITH SUPERNOVA NEUTRINOS
Invisible13 Workshop Lumley Castle, 15-19 July 2013 PROBING THE MASS HIERARCHY WITH SUPERNOVA NEUTRINOS Alessandro MIRIZZI (Hamburg University) OUTLINE Supernova neutrino flavor oscillations Observables
More informationXMASS: a large single-phase liquid-xenon detector
XMASS: a large single-phase liquid-xenon detector Katsuki Hiraide, the university of Tokyo for the XMASS Collaboration October 3 rd, 2016 IPRD16@Siena, Italy 1 XMASS project XMASS: a multi purpose experiment
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 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 informationNeutrino Sources in the Universe
Crab Nebula Neutrino Sources in the Universe Georg G. Raffelt Max-Planck-Institut für Physik, München Where do Neutrinos Appear in Nature? Nuclear Reactors Sun Particle Accelerators Supernovae (Stellar
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 informationSupernova Watches and HALO
Supernova Watches and HALO Workshop May 14-16, 2012 Clarence J. Virtue Supernova neutrinos First order expectations Approximate equipartition of neutrino fluxes Several characteristic timescales for the
More informationDetectors for astroparticle physics
Detectors for astroparticle physics Teresa Marrodán Undagoitia marrodan@physik.uzh.ch Universität Zürich Kern und Teilchenphysik II, Zürich 07.05.2010 Teresa Marrodán Undagoitia (UZH) Detectors for astroparticle
More informationSovan Chakraborty. MPI for Physics, Munich
Neutrino Mass Hierarchy from Supernova Neutrinos Sovan Chakraborty MPI for Physics, Munich Outline Supernova (SN) as Neutrino Source Oscillation of SN Neutrinos Signatures of Neutrino Mass Hierarchy Conclusions
More informationOther Physics with Geo-Neutrino Detectors
Other Physics with Geo-Neutrino Detectors M. Lindner Technical University Munich Neutrino Geophysics Workshop Hawaii, Dec. 14-16, 2005 Neutrinos & New Physics neutrinos as probes neutrino properties &
More informationSpontaneous Symmetry Breaking in Supernova Neutrinos
NOW 2014, 7 14 September Crab Nebula 2014, Otranto, Lecce, Italy Spontaneous Symmetry Breaking in Supernova Neutrinos Georg Raffelt, Max-Planck-Institut für Physik, München Some Developments since NOW
More informationSuper-Kamiokande (on the activities from 2000 to 2006 and future prospects)
Super-Kamiokande (on the activities from 2000 to 2006 and future prospects) M. Nakahata for Neutr ino and astr opar ticle Division Super-Kamiokande detector Atmospheric neutrinos Solar Neutrinos Proton
More informationRadio-chemical method
Neutrino Detectors Radio-chemical method Neutrino reactions: n+ν e => p+e - p+ν e => n+e + Radio chemical reaction in nuclei: A N Z+ν e => A-1 N(Z+1)+e - (Electron anti-neutrino, right) (Z+1) will be extracted,
More informationSupernova neutrinos for neutrino mixing and SN astrophysics
Supernova neutrinos for neutrino mixing and SN astrophysics Amol Dighe Tata Institute of Fundamental Research TPSC Seminar, IMSc, Chennai, 23 February 2005 Supernova neutrinos forneutrino mixing and SN
More informationPoS(NOW2016)041. IceCube and High Energy Neutrinos. J. Kiryluk (for the IceCube Collaboration)
IceCube and High Energy Neutrinos Stony Brook University, Stony Brook, NY 11794-3800, USA E-mail: Joanna.Kiryluk@stonybrook.edu IceCube is a 1km 3 neutrino telescope that was designed to discover astrophysical
More informationarxiv: v1 [astro-ph.im] 27 May 2012
Supernova Neutrino Detection Kate Scholberg Department of Physics, Duke University, Durham NC 27708, USA; email: schol@phy.duke.edu arxiv:1205.6003v1 [astro-ph.im] 27 May 2012 A core-collapse supernova
More informationHigh Energy Neutrino Astronomy
High Energy Neutrino Astronomy VII International Pontecorvo School Prague, August 2017 Christian Spiering, DESY Zeuthen Content Lecture 1 Scientific context Operation principles The detectors Atmospheric
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 informationCherenkov Detector. Cosmic Rays Cherenkov Detector. Lodovico Lappetito. CherenkovDetector_ENG - 28/04/2016 Pag. 1
Cherenkov Detector Cosmic Rays Cherenkov Detector Lodovico Lappetito CherenkovDetector_ENG - 28/04/2016 Pag. 1 Table of Contents Introduction on Cherenkov Effect... 4 Super - Kamiokande... 6 Construction
More informationOklahoma State University. Solar Neutrinos and their Detection Techniques. S.A.Saad. Department of Physics
Oklahoma State University Solar Neutrinos and their Detection Techniques S.A.Saad Department of Physics Topics to be covered Solar Neutrinos Solar Neutrino Detection Techniques Solar Neutrino Puzzle and
More informationSupernova Neutrino Physics with XENON1T and Beyond
Supernova Neutrino Physics with XENON1T and Beyond Shayne Reichard* University of Zurich nueclipse 2017 August 22 R. F. Lang*, C. McCabe, M. Selvi*, and I. Tamborra Phys. Rev. D94, arxiv:1606.09243 *Members
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 informationLow-Energy Neutrino-Argon Interactions: A Window into Stellar Collapse. Christopher Grant
Low-Energy Neutrino-Argon Interactions: A Window into Stellar Collapse Christopher Grant Neutrino bombs in outer space Critical Fe core mass ~1.4 M ν ν ν ν For core-collapse supernovae (SN) Gravitational
More informationNeutrino Physics: an Introduction
Neutrino Physics: an Introduction Lecture 3: Neutrinos in astrophysics and cosmology Amol Dighe Department of Theoretical Physics Tata Institute of Fundamental Research, Mumbai SERC EHEP School 2017 NISER
More informationLawrence Berkeley National Laboratory Lawrence Berkeley National Laboratory
Lawrence Berkeley National Laboratory Lawrence Berkeley National Laboratory Title Neutrino Physics with the IceCube Detector Permalink https://escholarship.org/uc/item/6rq7897p Authors Kiryluk, Joanna
More informationZakopane, Tatra Mountains, Poland, May Supernova Neutrinos. Georg G. Raffelt Max-Planck-Institut für Physik, München, Germany
52 nd Cracow School Crab Nebula on Theoretical Physics Zakopane, Tatra Mountains, Poland, 19 27 May 2012 Supernova Neutrinos Georg G. Raffelt Max-Planck-Institut für Physik, München, Germany Sanduleak
More informationMiami Conference December 15-20, 2011 Fort Lauderdale, FL. A.R. Fazely Southern University, Baton Rouge, LA
Miami Conference December 15-20, 2011 Fort Lauderdale, FL A.R. Fazely Southern University, Baton Rouge, LA What is IceCube? A gigaton neutrino detector funded through the National Science Foundation and
More informationLessons from Neutrinos in the IceCube Deep Core Array
Lessons from Neutrinos in the IceCube Deep Core Array Irina Mocioiu Penn State TeV 2009, July 15 2009 Point sources Diffuse fluxes from astrophysical objects from cosmic ray interactions from dark matter
More informationNeutrino Probes of Galactic and Extragalactic Supernovae
Neutrino Probes of Galactic and Extragalactic Supernovae Shin'ichiro Ando California Institute of Technology, Mail Code 130-33, Pasadena, CA 91125 Abstract. Neutrinos are a messenger of extreme condition
More informationSupernova Neutrinos Georg Raffelt, MPI Physics, Munich 2nd Schrödinger Lecture, University Vienna, 10 May 2011
Supernova Neutrinos Supernova Neutrinos Physics Opportunities with Supernova Neutrinos Georg Raffelt, Max-Planck-Institut für Physik, München Sanduleak -69 202 Sanduleak -69 202 Tarantula Nebula Large
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 informationHigh Energy Neutrino Astrophysics Latest results and future prospects
High Energy Neutrino Astrophysics Latest results and future prospects C. Spiering, Moscow, August 22, 2013 DETECTION PRINCIPLE Detection Modes Muon track from CC muon neutrino interactions Angular resolution
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 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 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 informationThe current status of the neutrino telescope experiments
The current status of the neutrino telescope experiments K. Mase, Chiba Univ. The neutrino astronomy Want to open the neutrino astronomy QuickTimeý Dz TIFFÅià èkç»çµåj êlí ÉvÉçÉOÉâÉÄ Ç Ç±ÇÃÉsÉNÉ`ÉÉǾå
More informationneutrino astronomy francis halzen university of wisconsin
neutrino astronomy francis halzen university of wisconsin http://icecube.wisc.edu 50,000 year old sterile ice instead of water we built a km 3 neutrino detector 3 challenges: drilling optics of ice atmospheric
More informationThe Hyper-Kamiokande project
22-July-2017 @Quy Nhon The Hyper-Kamiokande project Yasuo Takeuchi Kobe University Hyper-Kamiokande detector & current R&Ds Current status of the project Physics/Observation targets in HK Summary 1 Hyper-Kamiokande
More informationSupernova Neutrino Directionality
Supernova Neutrino Directionality Fan Zhang April 25, 2016 Subject: Senior Thesis Date Performed: Jan 2015 to Apr 2016 Instructor: Prof. Kate Scholberg Defense Committee: Prof. Kate Scholberg Prof. Roxanne
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 informationν?? Solar & Atmospheric Oscillation Experiments Greg Sullivan University of Maryland Aspen Winter Conference January 21, 1999 )Past )Present )Future
Solar & Atmospheric Oscillation Experiments Greg Sullivan of Maryland Aspen Winter Conference January 21, 1999 ν?? e )Past z Neutrino Mass Mass & Oscillations )Present z Atmospheric neutrinos z Solar Solar
More informationNeutrino Astronomy. Ph 135 Scott Wilbur
Neutrino Astronomy Ph 135 Scott Wilbur Why do Astronomy with Neutrinos? Stars, active galactic nuclei, etc. are opaque to photons High energy photons are absorbed by the CMB beyond ~100 Mpc 10 20 ev protons,
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 informationRecent advances in neutrino astrophysics. Cristina VOLPE (AstroParticule et Cosmologie APC, Paris)
Recent advances in neutrino astrophysics Cristina VOLPE (AstroParticule et Cosmologie APC, Paris) Flux (cm -2 s -1 MeV -1 ) 10 24 10 20 10 16 10 12 10 8 10 4 10 0 10-4 10-8 Neutrinos in Nature Cosmological
More informationIceCube: Ultra-high Energy Neutrinos
IceCube: Ultra-high Energy Neutrinos Aya Ishihara JSPS Research Fellow at Chiba University for the IceCube collaboration Neutrino2012 at Kyoto June 8 th 2012 1 Ultra-high Energy Neutrinos: PeV and above
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 informationMass Composition Study at the Pierre Auger Observatory
OBSERVATORY Mass Composition Study at the Pierre Auger Observatory Laura Collica for the Auger Milano Group 4.04.2013, Astrosiesta INAF Milano 1 Outline The physics: The UHECR spectrum Extensive Air Showers
More informationPossible Interpretations of IceCube High Energy Neutrinos
Possible Interpretations of IceCube High Energy Neutrinos ~1 km² Geographic South Pole Program on Particle Physics at the Dawn of the LHC13. ICTP-SP. Boris Panes, USP. Nov 12-2015 Based on 1411.5318 and
More informationParticle Physics with Neutrino Telescope Aart Heijboer, Nikhef
Particle Physics with Neutrino Telescope Aart Heijboer, Nikhef 1 high energy Quanta from the Universe (why look for neutrinos) Universe contains very high Energy particle accelerators (E = up to 10 6
More informationHigh-energy neutrinos
High-energy neutrinos Stefan Roth December 5, 2005 Abstract In the last decades, the interest in neutrinos raised strongly, not only because of the solution of the solar neutrino problem. This report is
More informationNeutrino Astronomy at the South Pole AMANDA and IceCube
1 Neutrino Astronomy at the South Pole AMANDA and IceCube Ignacio Taboada University of California - Berkeley Topics in Astroparticle and Underground Physics Zaragoza. Sept 10-14, 2005 2 The IceCube Collaboration
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 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 informationDetection of Gravitational Waves and Neutrinos from Astronomical Events
Detection of Gravitational Waves and Neutrinos from Astronomical Events Jia-Shu Lu IHEP,CAS April 18, 216 JUNO Neutrino Astronomy and Astrophysics Seminar 1 / 24 Outline Sources of both GW and neutrinos.
More informationPossible sources of very energetic neutrinos. Active Galactic Nuclei
Possible sources of very energetic neutrinos Active Galactic Nuclei 1 What might we learn from astrophysical neutrinos? Neutrinos not attenuated/absorbed Information about central engines of astrophysical
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 informationDiffuse Supernova Neutrino Background
Diffuse Supernova Neutrino Background John Beacom The Ohio State University Impossible Dream of Neutrino Astronomy If [there are no new forces] -- one can conclude that there is no practically possible
More informationAstrophysical Neutrino at HK
1 2 2 Astrophysical Neutrino at HK Solar neutrino Burning processes, modeling of the Sun Property of neutrino Supernova ν NASA, Chandra & Hubble 2007 5μpc kpc Mpc SN explosion mechanism SN monitor Nucleosynthe
More informationAstroparticle physics
Timo Enqvist University of Oulu Oulu Southern institute lecture cource on Astroparticle physics 15.09.2009 15.12.2009 1 High-energy cosmic rays 1.43 1.5 Cosmic-ray sources Sources, acceleration mechanisms,
More informationThe role of neutrinos in the formation of heavy elements. Gail McLaughlin North Carolina State University
The role of neutrinos in the formation of heavy elements Gail McLaughlin North Carolina State University 1 Neutrino Astrophysics What are the fundamental properties of neutrinos? What do they do in astrophysical
More informationSearch for Astrophysical Neutrino Point Sources at Super-Kamiokande
Search for Astrophysical Neutrino Point Sources at Super-Kamiokande Yusuke Koshio for Super-K collaboration Kamioka, ICRR, Univ. of Tokyo LNGS, INFN Super-Kamiokande detector Recent results of search for
More informationTopics in Nuclear Astrophysics. John Beacom, Theoretical Astrophysics Group, Fermilab
Topics in Nuclear Astrophysics John Beacom Theoretical Astrophysics Group, Fermilab Classical Nuclear Astrophysics How do stars shine? How old is the Universe? How do supernovae work? How do neutron stars
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 informationNeutrinos. Why measure them? Why are they difficult to observe?
Outline What is a neutrino? Why do we want to study them? Building a detector to detect the undetectable What does a neutrino detector see? How do you seperate a neutrino signal from the background? Neutrinos
More informationNeutrinos in Astrophysics and Cosmology
Crab Nebula Neutrinos in Astrophysics and Cosmology Introductory Remarks Georg G. Raffelt Max-Planck-Institut für Physik, München, Germany Periodic System of Elementary Particles Quarks Charge -1/3 Charge
More informationIceCube Results & PINGU Perspectives
1 IceCube Results & PINGU Perspectives D. Jason Koskinen for the IceCube-PINGU Collaboration koskinen@nbi.ku.dk September 2014 Neutrino Oscillation Workshop Otranto, Lecce, Italy 2 IceCube Detector ~1km
More informationSupernovae SN1987A OPERA Constraints on neutrino parameters. Supernova neutrinos. Ly Duong. January 25, 2012
January 25, 2012 Overview Supernovae Supernovae Supernova types Core collapse model Neutrino properties Detection of neutrinos Data and analysis Experiment results Comparison with results Possible neutrino
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 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 information1. Introduction on Astroparticle Physics Research options
Research options Large variety of topics in astro physics and particle physics Cosmic rays (sources, production and acceleration mechanisms) Stability of matter or proton decay (GUTs) Solar neutrinos (the
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 informationIceCube: Dawn of Multi-Messenger Astronomy
IceCube: Dawn of Multi-Messenger Astronomy Introduction Detector Description Multi-Messenger look at the Cosmos Updated Diffuse Astrophysical Neutrino Data Future Plans Conclusions Ali R. Fazely, Southern
More informationDiffuse SN Neutrino Background (DSNB)
Diffuse SN Neutrino Background (DSNB) What can we learn? Ideas under construction Cecilia Lunardini Arizona State University RIKEN BNL Research Center O introduction: motivation and facts O detection potential
More informationSuper-K Gd. M.Ikeda(ICRR) for Super-K collaboration Workshop for Neutrino Programs with facilities in Japan
Super-K Gd M.Ikeda(ICRR) for Super-K collaboration 20150804@JPARC Workshop for Neutrino Programs with facilities in Japan 1 Contents Introduction to SK-Gd Physics motivations Study of Gd effect to SK Plan
More informationSupernova 1987A and the Birth of Neutrino Astronomy
SN 1987A Supernova 1987A and the Birth of Neutrino Astronomy Georg G. Raffelt Max-Planck-Institut für Physik, München Large Magellanic Cloud Distance 50 kpc (160.000 light years) Sanduleak -69 202 Sanduleak
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 informationStudy of the penetrating component of cosmic rays underground using large scintillation detectors
Study of the penetrating component of cosmic rays underground using large scintillation detectors TAUP 2015, Torino, Italia, September, 7 11, 2015 1 Underground physics is the effective method to study
More informationMultiwavelength Search for Transient Neutrino Sources with IceCube's Follow-up Program
Multiwavelength Search for Transient Neutrino Sources with IceCube's Follow-up Program Nora Linn Strotjohann for the DESY Real-Time Group GROWTH Meeting at Caltech, July 26th 2016 The IceCube Neutrino
More information