DOCSLIB.ORG

A Review of Future Experiments

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

A review of future experiments Albrecht Karle University of Wisconsin-Madison Neutrino 2012 Kyoto Outline: •Neutrinos and Cosmic rays •Energy scales of neutrino telescopes, next challenges •1 to 100 GeV: Low energy extensions: PINGU,... •0.1 to 10000 TeV: Neutrino telescopes for neutrino astronomy •10^16 to 10^20eV: Strategies for cosmogenic neutrino flux discovery Albrecht Karle, UW-Madison Cosmic Rays and Neutrino Sources : neutrinos from accelerators Can neutrinos reveal origins Cosmic rays of cosmic rays? T. Gaisser 2005 pγ → pπ 0 ,nπ + + + π → µ + νµ + + µ → e + νe + νµ Cosmic ray interaction in accelerator region knee Prime Candidates 1 part m-2 yr-1 – SN remnants – Active Galactic Nuclei Ankle – Gamma Ray Bursts 1 part km-2 yr-1 2 Neutrino producUon from cosmic rays on known targets. T. GaisserT. Gaisser 2005 2005 pp → NN + pions; pγ → pπ 0 ,nπ + + + π → µ + νµ + + µ → e + νe + νµ Known targets: • Earth’s atmosphere: Atmospheric neutrinos (from π and K decay) • Interstellar maer in GalacUc plane: Cosmic rays interacUng with Interstellar maer, concentrated in the disk • Cosmic Microwave background: UHE cosmic rays interact with photons in intergalacUc photon fields. 3 Neutrino producUon from cosmic rays on known targets. T. GaisserT. Gaisser 2005 2005 pp → NN + pions; pγ → pπ 0 ,nπ + + + π → µ + νµ + + µ → e + νe + νµ Known targets: • Earth’s atmosphere: Atmospheric neutrinos (from π and K decay) Atmospheric neutrinos: • Interstellar maer in GalacUc AMANDA, IceCube plane: Cosmic rays interacUng with Interstellar maer, concentrated in the Waxman –bahcall upper bound disk IceCube E^-2 upper limit • Cosmic Microwave background: Cosmogenic UHE cosmic rays interact with GalacUc neutrino neutrino flux, flux model: eg ESS (blue line) photons in intergalacUc photon eg. Ingelman & Thunman fields. 4 How to detect UHE high energy neutrinos? The challenge: • Fluxes are small • The cross secUon is small Need to instrument/view very large target mass • backgrounds from cosmic rays, cosmic ray muons are high Need some overburden (or other good discriminaon) • Need to use natural targets, which are free, but – need to deal with environmental challenges – no control of the medium – lack of infrastructure (access, power, communicaons) – possibly unstable backgrounds Challenges for Calibraon full understanding of the medium, noise backgrounds, sensiUvity of sensor in situ (absolute sensiUvity, angular response) 5 Water/ice Cherenkov detectors: IceCube IceCube • Total of 86 strings and 162 IceTop tanks; • Compleon with 86 strings: December 2010 • Full operaon with all strings since May 2011. For results: see talks by G. Sullivan and A. Ishihara and numerous posters at this conference 6 A. Karle, UW-Madison 6 Water/ice Cherenkov detectors: Neutrino effecUve areas Wide energy range due to increase in effec1ve area! Area at 100 TeV (1TeV) 5 2 2 ) 10 IceCube 86: 40m (0.3m ) 2 10 4 Deep Core lowers threshold 3 10 from 100 GeV to 10 GeV. 10 2 10 IC-80 up TL EffecUve area for 1 νµ -1 Strong rise with energy: 10 – (up to 100TeV) -2 Antares 2007-8 10 – Increase of muon range Effective Neutrino Area (m -3 with energy up to PeV 10 – Flaening above PeV -4 energies. 10 IC-79 all sky PS -5 10 -6 10 1 2 3 4 5 6 7 8 9 10 11 log10(Primary Neutrino Energy - GeV) 7 Water/ice Cherenkov detectors: Neutrino effecUve areas Energy scales and future detectors - from low to high energy. PINGU: lower threshold 5 ) 10 from ~10 to few GeV 2 10 4 10 3 10 2 10 IC-80 up TL 1 -1 10 -2 Antares 2007-8 10 Effective Neutrino Area (m -3 10 -4 10 IC-79 all sky PS -5 10 -6 10 1 2 3 4 5 6 7 8 9 10 11 log (Primary Neutrino Energy - GeV) Low energy extensions 10 to IceCube’s DeepCore: PINGU, MICA 8 Water/ice Cherenkov detectors: Neutrino effecUve areas big neutrino telescopes 5 ) 10 TeV-PeV energy froner: 2 like KM3Net would 4 Km3Net, Baikal GVD 10 establish larger 3 detectors with more 10 2 sensiUvity from TeV to 10 PeV: 10 IC-80 up TL Astrophysical point 1 sources of neutrinos. -1 OpUmal view to GalacUc 10 -2 Antares 2007-8 Center (Southern 10 Hemisphere) Effective Neutrino Area (m -3 10 -4 10 IC-79 all sky PS -5 10 -6 10 1 2 3 4 5 6 7 8 9 10 11 log (Primary Neutrino Energy - GeV) Low energy extensions 10 to IceCube, DeepCore: PINGU, MICA 9 Water/ice Cherenkov detectors: Neutrino effecUve areas 5 ) 10 TeV-PeV energy froner: 2 UHE energy detectors 4 Km3Net, Baikal GVD 10 for GZK neutrino flux: 10 3 ARA, ARIANNA 10 2 10 IC-80 up TL Radio detecDon in ice: 1 Detecon volume and -1 thus sensivity 10 -2 Antares 2007-8 increases roughly 10 Effective Neutrino Area (m linearly with energy! -3 10 -4 10 IC-79 all sky PS -5 10 -6 10 1 2 3 4 5 6 7 8 9 10 11 log (Primary Neutrino Energy - GeV) Low energy extensions 10 to IceCube, DeepCore: PINGU, MICA 10 Low energies, 1 – 100 GeV, PINGU ... The Neutrino Detector Spectrum NOνA OPERA Accelerator based K2K, MINOS T2K Atmosphericl 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV Solar/ Astrophysical Reactor Atmospheric IceCube/ANTARES ANITA/RICE/Auger/ KM3Net/baikal GVD ARA/ARIANNA borexino/KamLand/Daya Bay/Double Chooz/SNO/SuperK Non-accelerator based Slide: Courtesy Darren Grant NNN 2011 * boxes select primary detector physics energy regimes and are not absolute limits 11 Low energies, 1 – 100 GeV, PINGU ... The Neutrino Detector Spectrum NOνA OPERA Accelerator based K2K, MINOS T2K Atmosphericl 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV Solar/ Astrophysical Reactor Atmospheric Gap IceCube/ANTARES ANITA/RICE/Auger/ KM3Net/baikal GVD ARA/ARIANNA borexino/KamLand/Daya Bay/Double Chooz/SNO/SuperK Dark Non-accelerator based Maer ντ Appearance νμ Neutrino Disappearance Mass Hierarchy Slide: Courtesy Darren Grant NNN 2011 * boxes select primary detector physics energy regimes and are not absolute limits 12 Low energies, 1 – 100 GeV, PINGU ... The Neutrino Detector Spectrum NOνA OPERA Accelerator based K2K, MINOS T2K Atmosphericl 10 MeV 100 MeV 1 GeV 10 GeV 100 GeV 1 TeV 10 TeV 1 EeV Solar/ DeepCore Astrophysical Reactor Atmospheric IceCube/ANTARES ANITA/RICE/Auger/ borexino/KamLand/Daya Bay/Double KM3Net/baikal GVD ARA/ARIANNA Chooz/SNO/SuperK PINGU Non-accelerator based beyond PINGU ~70 active members in feasibility studies: IceCube, KM3Net, Several neutrino experiments Photon detector developers Slide aer: Darren Grant Theorists NNN 2011 * boxes select primary detector physics energy regimes and are not absolute limits 13 Low energies, 1 – 100 GeV, PINGU ... IceCube-DeepCore • IceCube extended its “low” energy response with a densely instrumented infill array: DeepCore http://arxiv.org/abs/1109.6096" • Significant improvement in capabilities from ~10 GeV to ~300 GeV (νμ) • Scientific Motivations: • Indirect search for dark matter • Neutrino oscillations (e.g., ντ appearance) • Neutrino point sources in the southern hemisphere (e.g., galactic center) 14 Low energies, 1 – 100 GeV, PINGU ... IceCube - DeepCore: DESIGN http://arxiv.org/abs/1109.6096" •! Eight special strings in filled in the bottom center of IceCube •! ~5x higher effective photocathode density than regular IceCube IceCube! •! Result: ~20 MTon detector with % extra% ~10 GeV threshold, will collect % veto cap! O(100k) physics quality atmospheric "/yr! VETO AMANDA! •! IceCube’s top and outer layers of strings m provide an active veto shield for DeepCore! Deep % Core! 350 •! Effective #-free depth much greater! •! Atm. #/" trigger ratio is ~106! 250 m •! Vetoing algorithms expected to reach well beyond 106 level of background rejection (Muon flux after veto comparable to Sudbury depth)! 15 Low energies, 1 – 100 GeV, PINGU ... PINGU •! Phased IceCube Next-Generaon PINGU geometry Upgrade (more compact version also studied) •! Add 20 strings with ~1000 opUcal modules inside the Deep Core region (~500PMT) •! Expected energy threshold near 1 GeV •! R&D opportunity for future developments 100 Numu NHits 20 String PINGU V2 PRELIMINARY IC86 SMT3 Triggered 80 No Noise 4m PINGU DOM DOM Spacing 60 Average Number of Hits 40 20 Courtesy J. Koskinen 0 0 10 20 30 40 50 Neutrino Energy (GeV) 16 Simulated event in DeepCore and PINGU! DeepCore Only! • 8 GeV up-going muon neutrino (physics only hits)! DeepCore + PINGU! • No. of PMTs fired:! ! !Deep Core: 11 ! ! !PINGU: 83 ! 17 Courtesy J. Koskinen Neutrino PINGU Physics hierarchy Mena, Mocioiu & Razzaque, Phys. Rev. D78, 093003 (2008) 2 (sin (2θ13)=0.1) • Probe lower mass WIMPs • Gain sensitivity to second oscillation peak/trough • enhanced sensitivity to neutrino mass hierarchy ντ appearance • Gain increased sensitivity to supernova neutrino bursts νµ disappearance • Extension of current search for coherent increase in singles rate across entire detector volume • Only 2±1 core collapse SN/century in Milky Way • need to reach out to our neighboring galaxies • Gain depends strongly on noise reduction via Deep Core data coincident photon detection (e.g., in neighbor Resconi et al. (Poster) DOMs) Ref. on Supernova detecDon: G. Sullivan’s talk - L. Demiroers, M. Ribordy, M. Salathe arXiv:1106.1937 - Posters by M. Voge, R. Bruin Mass hierarchy Figure and Analysis from: Akhmedov, Razzaque, Smirnov, arXiv: 1205.7071 See poster by E. Resconi et al. (IceCube and PINGU) • Expected significance for observed number of events for IH vs NH are shown in energy vs. zenith plot • If required energy and direcUonal resoluUon is achievable: high stasUcal significance +6 18 +3 14 0 GeV 10 Conclusion (Akhmedov et al.): -1 Significance “Our preliminary esBmates show that aDer 5 years of PINGU 20 6 operaBon the significance of the determinaBon of the hierarchy can -2 range from 3 to 11 (without taking into account parameter [-1,08] [-0.8,-0.5] [-0.5,0.0] degeneracy), depending on the accuracy of reconstrucon of neutrino cos (theta) energy and direcon.” Assumed above: Energy resoluon: 4 GeV, Angular resoluDon: 0.3 in cos(theta) Exposure: 10 Mt yr 19 Low energies, 1 – 100 GeV, PINGU ..
Recommended publications
  • Snowmass 2021 Letter of Interest: Ultra-High-Energy Neutrinos

    Snowmass 2021 Letter of Interest: Ultra-High-Energy Neutrinos

    Snowmass 2021 Letter of Interest: Ultra-High-Energy Neutrinos Markus Ahlers,1 Jaime Alvarez-Mu~niz,´ 2 Rafael Alves Batista,3 Luis Anchordoqui,4 Carlos A. Arg¨uelles,5 Jos´e Bazo,6 James Beatty,7 Douglas R. Bergman,8 Dave Besson,9, 10 Stijn Buitink,11 Mauricio Bustamante,1, 12, ∗ Olga Botner,13 Anthony M. Brown,14 Washington Carvalho Jr.,15 Pisin Chen,16 Brian A. Clark,17 Amy Connolly,7 Linda Cremonesi,18 Cosmin Deaconu,19 Valentin Decoene,20 Paul de Jong,21, 22 Sijbrand de Jong,23, 22 Peter B. Denton,24, y Krijn De Vries,25 Michele Doro,26 Michael A. DuVernois,27 Ke Fang,28 Christian Glaser,13 Peter Gorham,29 Claire Gu´epin,30 Allan Hallgren,13 Jordan C. Hanson,31 Tim Huege,32, 11 Martin H. Israel,33 Albrecht Karle,27 Spencer R. Klein,34, 35 Kumiko Kotera,20 Ilya Kravchenko,36 John Krizmanic,30, 37 John G. Learned,29 Olivier Martineau-Huynh,38 Peter M´esz´aros,39 Thomas Meures,27 Miguel A. Mostaf´a,39, 40 Katharine Mulrey,11 Kohta Murase,39, 40, 41 Jiwoo Nam,16 Anna Nelles,42, 43 Eric Oberla,44 Foteini Oikonomou,45 Angela V. Olinto,44 Yasar Onel,46 A. Nepomuk Otte,47 Sergio Palomares-Ruiz,48 Alex Pizzuto,27 Steven Prohira,7 Brian Rauch,49 Mary Hall Reno,46 Juan Rojo,50, 51 Andr´esRomero-Wolf,52 Ibrahim Safa,5, 27 Olaf Scholten,53, 25 Frank G. Schr¨oder,54, 32 Wayne Springer,55 Irene Tamborra,1, 12 Charles Timmermans,51, 23 Diego F. Torres,56 Jo~aoR.
  • Neutrino Astrophysics

    Neutrino Astrophysics

    Neutrino Astrophysics Ryan Nichol UK Input to European Strategy Neutrino Astrophysics Ryan Nichol UK Input to European Strategy Highly cited papers • Higgs Discovery (2012) • Z discovery (1983) –1500+ – 8000+ citations –2000+ • SN1987a neutrinos (1987) • Atmospheric neutrino • Positron excess –1500+ oscillations (1998) [PAMELA] (2008) • Weak neutral current –5000+ citations –1900+ (1973) • Top quark discovery • Reactor neutrino theta_13 –1500+ (1995) (2012) • Charmomium (2003) –3000+ citations –1900+ –1400+ • Solar neutrino oscillations • b-quark discovery (1977) • B-Bbar oscillation (1987) (2002) –1900+ –1300+ –3000+ citations • W-discovery (1983) • nu_mu -> nu_e (2011) • Kaon CP violations (1964) –1800+ –1300+ –3000+ citations • Z width (2005) • Accelerator neutrino • Reactor antineutrino –1700+ oscillation (2002) [KamLAND] (2003) • Proton spin crisis (1989) –1100+ –2000+ citations –1700+ • Muon neutrino discovery • Gravitational Waves • LSND anomaly (2001) (1962) (2016) –1700+ –1100+ –2000+ citations • Parity non conservation • DAMA/Libra (2008-) • c-quark discovery (1974) (1957) –1000+ –2000+ citations –1600+ • Pentaquark [LEPS] (2003) • Solar neutrino • LUX Dark Matter (2013) –1000+ [Homestake] (1968-1998) –1500+ • Neutron EDM (2006) !3 –2000+ • g-2 (2006) –1000+ Highly cited papers • Higgs Discovery (2012) • Z discovery (1983) –1500+ – 8000+ citations –2000+ • SN1987a neutrinos (1987) • Atmospheric neutrino • Positron excess –1500+ oscillations (1998) [PAMELA] (2008) • Weak neutral current –5000+ citations –1900+ (1973) • Top quark
  • In the Light of LSND, Miniboone and Other Data

    In the Light of LSND, Miniboone and Other Data

    DAPNIA-SPhT Joint Seminar, 21 May 2007 Exotic Neutrino Physics in the light of LSND, MiniBooNE and other data Marco Cirelli + Stéphane Lavignac SPhT - CEA/Saclay Introduction CDHSW Neutrino Physics (pre-MiniBooNE): CHORUS NOMAD NOMAD NOMAD 0 KARMEN2 CHORUS Everything fits in terms of: 10 LSND 3 neutrino oscillations (mass-driven) Bugey BNL E776 K2K SuperK CHOOZ erde 10–3 PaloV Super-K+SNO Cl +KamLAND ] 2 KamLAND [eV 2 –6 SNO m 10 Super-K ∆ Ga –9 10 νe↔νX νµ↔ντ νe↔ντ νe↔νµ 10–12 10–4 10–2 100 102 tan2θ http://hitoshi.berkeley.edu/neutrino Particle Data Group 2006 Introduction CDHSW Neutrino Physics (pre-MiniBooNE): CHORUS NOMAD NOMAD NOMAD 0 KARMEN2 CHORUS Everything fits in terms of: 10 LSND 3 neutrino oscillations (mass-driven) Bugey BNL E776 K2K SuperK Simple ingredients: CHOOZ erde 10–3 PaloV νe, νµ, ντ m1, m2, m3 Super-K+SNO Cl +KamLAND ] θ12, θ23, θ13 δCP 2 KamLAND [eV 2 –6 SNO m 10 Super-K ∆ Ga –9 10 νe↔νX νµ↔ντ νe↔ντ νe↔νµ 10–12 10–4 10–2 100 102 tan2θ http://hitoshi.berkeley.edu/neutrino Particle Data Group 2006 Introduction CDHSW Neutrino Physics (pre-MiniBooNE): CHORUS NOMAD NOMAD NOMAD 0 KARMEN2 CHORUS Everything fits in terms of: 10 LSND 3 neutrino oscillations (mass-driven) Bugey BNL E776 K2K SuperK Simple ingredients: CHOOZ erde 10–3 PaloV νe, νµ, ντ m1, m2, m3 Super-K+SNO Cl +KamLAND ] θ12, θ23, θ13 δCP 2 KamLAND Simple theory: [eV 2 –6 SNO m 10 |ν! = cos θ|ν1! + sin θ|ν2! Super-K ∆ −E1t −E2t |ν(t)! = e cos θ|ν1! + e sin θ|ν2! Ga 2 Ei = p + mi /2p 2 –9 ν ↔ν m L 10 e X 2 2 ∆ ν ↔ν P ν → ν θ µ τ ( α β) = sin 2 αβ sin ν ↔ν E e
  • The Compact Program Booklet

    The Compact Program Booklet

    - 1 - MONDAY, 5 SEPTEMBER 2011 WELCOME TO 12th International Conference on Topics in Astroparticle and Underground Physics 5 – 9 September 2011, Munich, Germany - 2 - structure of The ConferenCe SUNDAY, 4 SEP 2011 WEDNesDAY, 7 SEP 2011 Page 11 17:00 - 21:00 Registration/Reception 09:00 - 10:45 Plenary: Neutrinos 11:15 - 13:00 Plenary: Neutrinos MONDAY, 5 SEP 2011 Page 3 14:30 - 16:10 DM AM DBD/NM LE 09:00 - 10:10 Plenary: Cosmology 16:50 - 18:30 DM AM NO C 10:10 - 10:45 Plenary: Dark Matter 20:00 - 23:30 Conference Dinner 11:15 - 11:50 Plenary: Dark Matter 11:50 - 12:25 Plenary: Astrophysical Messengers THURSDAY, 8 SEP 2011 Page 14 12:25 - 13:00 Plenary: Underground Physics 09:00 - 10:45 Plenary: Astrophysical Messengers 14:30 - 16:10 DM AM DBD/NM LE 11:15 - 13:00 Plenary: Astrophysical Messengers 16:50 - 18:30 DM AM NO C 14:30 - 16:10 DM AM DBD/NM GW 16:50 - 18:30 DM LE DBD/NM GW TUesDAY, 6 seP 2011 Page 6 09:00 - 10:50 Plenary: Dark Matter FRIDAY, 9 seP 2011 Page 17 11:15 - 13:00 Plenary: Dark Matter 09:00 - 09:35 Plenary: Underground Physics 14:30 - 16:10 DM AM DBD/NM LE 09:35 - 10:45 Plenary: Astrophysical Messengers 16:50 - 18:30 DM AM NO C 11:15 - 12:25 Plenary: Astrophysical Messengers 18:30 - 20:00 Poster Session 12:25 - 13:00 Concluding Session DM Dark Matter NO Neutrino Oscillations AM Astrophysical Messengers DBD/NM Double Beta Decay, Neutrino Mass C Cosmology LE Low-Energy Neutrinos GW Gravitational Waves - 3 - MONDAY, 5 SEPTEMBER 2011 PLENARY SessION: CosmoloGY I Festsaal 09:00 CMB and Planck Francois Bouchet (IAP Paris)
  • Science Case for the Giant Radio Antenna Neutrino Detector

    Science Case for the Giant Radio Antenna Neutrino Detector

    Science Case for the Giant Radio Antenna Neutrino Detector Kumiko Kotera — Institut d’Astrophysique de Paris, UMR 7095 - CNRS, Université Pierre & Marie Curie, 98 bis boulevard Arago, 75014, Paris, France ; email: [email protected] “The title [of this book] is more of an expression of hope than a de- scription of the book’s contents [...]. As new ideas (theoretical and experimental) are explored, the observational horizon of neutrino as- trophysics may grow and the successor to this book may take on a different character, perhaps in a time as short as one or two decades.” John N. Bahcall, Neutrino Astrophysics, Cambridge University Press, 1989 igh-energy (> 1015 eV) neutrino as- progress in the fields of high-energy astro- tronomy will probe the working of physics and astroparticle physics. Addi- Hthe most violent phenomena in the tionally, they should contribute to unveil Universe. When most of the information fundamental neutrino properties. we have on the Universe stems from the observation of light, one essential strategy to undertake is to diversify our messengers. 1 Why neutrinos? The most energetic, mysterious and hardly understood astrophysical sources or events Neutrinos are unique messengers that let (fast-rotating neutron stars, supernova ex- us see deeper in objects, further in dis- plosions and remnants, gamma-ray bursts, tance, and pinpoint the exact location of outflows and flares from active galactic nu- their sources. clei, ...) are expected to be producers Neutrinos can escape much denser as- of high-energy non-thermal hadronic emis- trophysical environments than light, hence sion. Hence they should produce copious they enable us to explore processes in the amounts of high-energy neutrinos.
  • Km3net/ORCA Telescopes

    Km3net/ORCA Telescopes

    Search for light sterile neutrinos with ANTARES and KM3NeT/ORCA telescopes A. Domi1,2, J. A. B. Coelho3, T. Thakore4, for the ANTARES and KM3NeT Collaborations 1 Università degli Studi di Genova, Genoa (Italy) - [email protected] 2 INFN-Genova, Genoa (Italy) 3 LAL, Univ. Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, Orsay (France) - [email protected] 4 University of Cincinnati, Ohio (United States) - [email protected] VLVnT Workshop - 19/05/2021 1 Where are we with light sterile neutrinos? • Majority of experiments have confirmed the 3 flavour neutrino oscillations. • In parallel, anomalies observed in some oscillation experiments: Anomalies in Short baseline (SBL) Ref: Prog.Part.Nucl.Phys. 111 (2020) 103736 experiments •LSND: �� -> �e •MINIBooNE: �� -> �e / �� -> �e Gallium Anomalies: �e disappearance Reactor anomalies: e disappearance � Disagreement between appearance and disappearance NO ANOMALIES observed in / disappearance. Further observations needed! �� �� 2 Where are we with light sterile neutrinos? Cosmology • Constrains the effective number of relativistic species (Neff) in our universe. • A SBL neutrino would require Neff=4. • Measured Neff compatible with 3. -> Tension with SBL anomalies. • Tension relaxes when cosmological data are combined with astrophysical data. • Cosmological data alone can be compatible with • an eV-mass sterile neutrino only if its contribution to Neff is very small, • a larger Neff only if it comes from a nearly massless sterile particle. We need further observations: neutrino telescopes make it possible! 3 Sterile Neutrinos • Oscillations in the presence of sterile neutrinos are solutions of: 2 • Adding one sterile neutrino introduces 6 more free parameters: �m41 , 3 mixing angles (�14,�24,�34) and 2 more CP phases (�14, �24).
  • A Survey of the Physics Related to Underground Labs

    A Survey of the Physics Related to Underground Labs

    ANDES: A survey of the physics related to underground labs. Osvaldo Civitarese Dept.of Physics, University of La Plata and IFLP-CONICET ANDES/CLES working group ANDES: A survey of the physics related to underground labs. – p. 1 Plan of the talk The field in perspective The neutrino mass problem The two-neutrino and neutrino-less double beta decay Neutrino-nucleus scattering Constraints on the neutrino mass and WR mass from LHC-CMS and 0νββ Dark matter Supernovae neutrinos, matter formation Sterile neutrinos High energy neutrinos, GRB Decoherence Summary The field in perspective How the matter in the Universe was (is) formed ? What is the composition of Dark matter? Neutrino physics: violation of fundamental symmetries? The atomic nucleus as a laboratory: exploring physics at large scale. Neutrino oscillations Building neutrino flavor states from mass eigenstates νl = Uliνi i X Energy of the state m2c4 E ≈ pc + i i 2E Probability of survival/disappearance 2 ′ −i(Ei−Ep)t/h¯ ∗ P (νl → νl′ )= | δ(l, l )+ Ul′i(e − 1)Uli | 6 Xi=p 2 2 4 (mi −mp )c L provided 2Ehc¯ ≥ 1 Neutrino oscillations The existence of neutrino oscillations was demonstrated by experiments conducted at SNO and Kamioka. The Swedish Academy rewarded the findings with two Nobel Prices : Koshiba, Davis and Giacconi (2002) and Kajita and Mc Donald (2015) Some of the experiments which contributed (and still contribute) to the measurements of neutrino oscillation parameters are K2K, Double CHOOZ, Borexino, MINOS, T2K, Daya Bay. Like other underground labs ANDES will certainly be a good option for these large scale experiments.
  • The ANTARES and Km3net Neutrino Telescopes: Status and Outlook for Acoustic Studies

    The ANTARES and Km3net Neutrino Telescopes: Status and Outlook for Acoustic Studies

    EPJ Web of Conferences 216, 01004 (2019) https://doi.org/10.1051/epjconf/201921601004 ARENA 2018 The ANTARES and KM3NeT neutrino telescopes: Status and outlook for acoustic studies Véronique Van Elewyck1,2, for the ANTARES and KM3NeT Collaborations 1APC, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, France 2Institut Universitaire de France, 75005 Paris, France Abstract. The ANTARES detector has been operating continuously since 2007 in the Mediterranean Sea, demonstrating the feasibility of an undersea neutrino telescope. Its superior angular resolution in the reconstruction of neutrino events of all flavors results in unprecedented sensitivity for neutrino source searches in the southern sky at TeV en- ergies, so that valuable constraints can be set on the origin of the cosmic neutrino flux discovered by the IceCube detector. The next generation KM3NeT neutrino telescope is now under construction, featuring two detectors with the same technology but different granularity: ARCA designed to search for high energy (TeV-PeV) cosmic neutrinos and ORCA designed to study atmospheric neutrino oscillations at the GeV scale, focusing on the determination of the neutrino mass hierarchy. Both detectors use acoustic devices for positioning calibration, and provide testbeds for acoustic neutrino detection. 1 Introduction Neutrinos have long been proposed as a complementary probe to cosmic rays and photons to explore the high-energy (HE) sky, as they can emerge from dense media and travel across cosmological dis- tances without being deflected by magnetic fields nor absorbed by inter- and intra-galactic matter and radiation. HE (>TeV) neutrinos are expected to be emitted in a wide range of astrophysical objects.
  • Pos(ICHEP2020)886

    Pos(ICHEP2020)886

    The Outer Detector (OD) system for the Hyper-Kamiokande experiment PoS(ICHEP2020)886 Stephane Zsoldos0,1,2,∗ 0Department of Physics, King’s College London, Strand, London WC2R 2LS, United Kingdom 1Department of Physics, University of California, Berkeley, CA 94720, Berkeley, USA 2Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720-8153, USA E-mail: [email protected], [email protected] Hyper-Kamiokande, scheduled to begin construction as soon as 2020, is a next generation under- ground water Cherenkov detector, based on the highly successful Super-Kamiokande experiment. It will serve as a far detector, 295 km away, of a long baseline neutrino experiment for the upgraded J-PARC beam in Japan. It will also be a detector capable of observing — far beyond the sensitivity of the Super-Kamiokande detector — proton decay, atmospheric neutrinos, and neutrinos from astronomical sources. An Outer Detector (OD) consisting of PMTs mounted behind the inner detector PMTs and facing outwards to view the outer shell of the cylindrical tank, would provide topological information to identify interactions originating from particles outside the inner detector. Any optimization would lead to a significant improvement for the physics goals of the experiment, which are the measurement of the CP leptonic phase and the determination of the neutrino mass hierarchy. An innovative new setup using small 3" PMTs is being proposed for the Hyper-Kamiokande OD. They would give better redundancy, spatial, and angular resolution, as there would be twice or three times more photosensors that the original 8" design proposal of the experiment, and for a reduced cost.
  • Realization of the Low Background Neutrino Detector Double Chooz: from the Development of a High-Purity Liquid & Gas Handling Concept to first Neutrino Data

    Realization of the Low Background Neutrino Detector Double Chooz: from the Development of a High-Purity Liquid & Gas Handling Concept to first Neutrino Data

    Realization of the low background neutrino detector Double Chooz: From the development of a high-purity liquid & gas handling concept to first neutrino data Dissertation of Patrick Pfahler TECHNISCHE UNIVERSITAT¨ MUNCHEN¨ Physik Department Lehrstuhl f¨urexperimentelle Astroteilchenphysik / E15 Univ.-Prof. Dr. Lothar Oberauer Realization of the low background neutrino detector Double Chooz: From the development of high-purity liquid- & gas handling concept to first neutrino data Dipl. Phys. (Univ.) Patrick Pfahler Vollst¨andigerAbdruck der von der Fakult¨atf¨urPhysik der Technischen Universit¨atM¨unchen zur Erlangung des akademischen Grades eines Doktors des Naturwissenschaften (Dr. rer. nat) genehmigten Dissertation. Vorsitzender: Univ.-Prof. Dr. Alejandro Ibarra Pr¨uferder Dissertation: 1. Univ.-Prof. Dr. Lothar Oberauer 2. Priv.-Doz. Dr. Andreas Ulrich Die Dissertation wurde am 3.12.2012 bei der Technischen Universit¨atM¨unchen eingereicht und durch die Fakult¨atf¨urPhysik am 17.12.2012 angenommen. 2 Contents Contents i Introduction 1 I The Neutrino Disappearance Experiment Double Chooz 5 1 Neutrino Oscillation and Flavor Mixing 6 1.1 PMNS Matrix . 6 1.2 Flavor Mixing and Neutrino Oscillations . 7 1.2.1 Survival Probability of Reactor Neutrinos . 9 1.2.2 Neutrino Masses and Mass Hierarchy . 12 2 Reactor Neutrinos 14 2.1 Neutrino Production in Nuclear Power Cores . 14 2.2 Energy Spectrum of Reactor neutrinos . 15 2.3 Neutrino Flux Approximation . 16 3 The Double Chooz Experiment 19 3.1 The Double Chooz Collaboration . 19 3.2 Experimental Site: Commercial Nuclear Power Plant in Chooz . 20 3.3 Physics Program and Experimental Concept . 21 3.4 Signal . 23 3.4.1 The Inverse Beta Decay (IBD) .
  • Ankur Sharma

    Ankur Sharma

    Ankur Sharma Date of Birth 2nd August 1991 Gender Male Nationality Indian Phone +46 76 447 51 45 Address Eklundshovsvägen 4B, Lgh 1104 Email [email protected] 752 37, Uppsala, Sweden [email protected] Research Interests Phenomenological studies of VHE emission from jets of AGNs; multi-messenger and multi-wavelength connection in blazars with neutrino, gamma-ray and X-ray data; gamma-ray astronomy; observability of point sources with Cherenkov neutrino telescopes; detection strategies for ultra-high energy neutrinos Education Jan 2017 - PhD in Physics - University of Pisa (Italy) Present Area of study - Astroparticle Physics, Neutrino Astrophysics - Astroparticles, Experimental Astrophysics & Astroparticle Physics - High Energy Experimental Physics Thesis Title - Analyzing the high energy activity of candidate blazars to constrain their observability by neutrino telescopes Supervisor - Dr. Antonio Marinelli ([email protected]) Aug 2009 - Integrated M.Sc. (M.Sc. + B.Sc.) in Applied Physics - Indian Institute of Technology (ISM), Dhanbad Feb 2015 Area of study - Applied Physics - Nuclear & Particle Physics, Classical Mechanics, Quantum Mechanics, Electrodynamics - Computer Networks, Microprocessors, C++, ForTran Sept 2013 - Erasmus Mundus India4EU II Exchange Mobility - University of Porto (Portugal) July 2014 Area of study - Master Thesis, Astronomy - Stellar Structure & Evolution, Cosmology - Optical Communication, Measurement Techniques & Instrumentation Thesis Title - Constraining the Parameter Space of Dynamical
  • Pos(ICRC2021)048

    Pos(ICRC2021)048

    ICRC 2021 THE ASTROPARTICLE PHYSICS CONFERENCE ONLINE ICRC 2021Berlin | Germany THE ASTROPARTICLE PHYSICS CONFERENCE th Berlin37 International| Germany Cosmic Ray Conference 12–23 July 2021 Rapporteur ICRC 2021: Neutrinos and Muons PoS(ICRC2021)048 0,1, Anna Nelles ∗ 0DESY, Platanenallee 6, 15738 Zeuthen, Germany 1ECAP, Friedrich-Alexander-University Erlangen-Nuremberg, Erwin-Rommel-Str. 1, 91058 Erlangen, Germany E-mail: [email protected] This contribution attempts to summarize the status of the field of neutrinos from the cosmos as presented at the ICRC 2021, the first online-only edition of this conference. This rapporteur report builds on 212 contributions with pre-recorded talks and posters, as well as 11 discussion sessions. Furthermore, many of the session conveners provided valuable input to this summary. 37th International Cosmic Ray Conference (ICRC 2021) July 12th – 23rd, 2021 Online – Berlin, Germany ∗Presenter © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). https://pos.sissa.it/ Rapporteur: Neutrinos and Muons Anna Nelles The field of neutrino astronomy already provides exciting results, however,it is still dominated by very low statistics in astrophysical neutrino detections. The most transformative results have been discussed in the multi-messenger context [1] and clearly neutrinos are becoming a target of opportunity for all experiments with a potential sensitivity to them. The neutrino field itself is booming with new ideas for detectors and has reached a maturity in which detailed data analysis and systematic detector calibration are the order of business. To summarize the sentiment: the community is doing their homework to get ready for many more neutrinos, which the broader community is excited about.