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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 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 -
Book of Abstracts
12th International Neutrino Summer School 2019 Monday 05 August 2019 - Friday 16 August 2019 Fermi National Accelerator Laboratory Book of Abstracts Contents Intro to Group Exercises .................................... 1 Neutrinos and nuclear non-proliferation ........................... 1 INSS2019 welcome and introduction .............................. 1 Solar and Reactor Neutrino Experiments ........................... 1 Precise Measurement of Reactor Antineutrino Oscillation Parameters and Fuel-dependent Variation of Antineutrino Yield and Spectrum at RENO ................. 1 Using Convolutional Neural Networks to Reconstruct Dead Channels in MicroBooNE . 1 Origin and Nature of Neutrino Mass I ............................. 2 Introduction to Leptogenesis .................................. 2 Origin and Nature of Neutrino Mass II ............................ 2 Direct Neutrino Mass Measurements ............................. 2 Neutrinoless Double-beta Decay Experiments ........................ 2 Neutrino Beams and Fluxes .................................. 3 Lepton-Nucleus Cross Section Theory ............................. 3 Neutrino Cross Section Experiments ............................. 3 Origin and Nature of Neutrino Mass III ............................ 3 Particle Astrophysics with High-Energy Neutrinos ..................... 3 Neutrino Detection II ...................................... 3 Phenomenology of Atmospheric and Accelerator Neutrinos ................ 3 Tau neutrinos and upward-going air showers: stochastic versus continuous -
The Gran Sasso Underground Laboratory Program
The Gran Sasso Underground Laboratory Program Eugenio Coccia INFN Gran Sasso and University of Rome “Tor Vergata” [email protected] XXXIII International Meeting on Fundamental Physics Benasque - March 7, 2005 Underground Laboratories Boulby UK Modane France Canfranc Spain INFN Gran Sasso National Laboratory LNGSLNGS ROME QuickTime™ and a Photo - JPEG decompressor are needed to see this picture. L’AQUILA Tunnel of 10.4 km TERAMO In 1979 A. Zichichi proposed to the Parliament the project of a large underground laboratory close to the Gran Sasso highway tunnel, then under construction In 1982 the Parliament approved the construction, finished in 1987 In 1989 the first experiment, MACRO, started taking data LABORATORI NAZIONALI DEL GRAN SASSO - INFN Largest underground laboratory for astroparticle physics 1400 m rock coverage cosmic µ reduction= 10–6 (1 /m2 h) underground area: 18 000 m2 external facilities Research lines easy access • Neutrino physics 756 scientists from 25 countries Permanent staff = 66 positions (mass, oscillations, stellar physics) • Dark matter • Nuclear reactions of astrophysics interest • Gravitational waves • Geophysics • Biology LNGS Users Foreigners: 356 from 24 countries Italians: 364 Permanent Staff: 64 people Administration Public relationships support Secretariats (visa, work permissions) Outreach Environmental issues Prevention, safety, security External facilities General, safety, electrical plants Civil works Chemistry Cryogenics Mechanical shop Electronics Computing and networks Offices Assembly halls Lab -
Required Sensitivity to Search the Neutrinoless Double Beta Decay in 124Sn
Required sensitivity to search the neutrinoless double beta decay in 124Sn Manoj Kumar Singh,1;2∗ Lakhwinder Singh,1;2 Vivek Sharma,1;2 Manoj Kumar Singh,1 Abhishek Kumar,1 Akash Pandey,1 Venktesh Singh,1∗ Henry Tsz-King Wong2 1 Department of Physics, Institute of Science, Banaras Hindu University, Varanasi 221005, India. 2 Institute of Physics, Academia Sinica, Taipei 11529, Taiwan. E-mail: ∗ [email protected] E-mail: ∗ [email protected] Abstract. The INdias TIN (TIN.TIN) detector is under development in the search for neutrinoless double-β decay (0νββ) using 90% enriched 124Sn isotope as the target mass. This detector will be housed in the upcoming underground facility of the India based Neutrino Observatory. We present the most important experimental parameters that would be used in the study of required sensitivity for the TIN.TIN experiment to probe the neutrino mass hierarchy. The sensitivity of the TIN.TIN detector in the presence of sole two neutrino double-β decay (2νββ) decay background is studied at various energy resolutions. The most optimistic and pessimistic scenario to probe the neutrino mass hierarchy at 3σ sensitivity level and 90% C.L. is also discussed. Keywords: Double Beta Decay, Nuclear Matrix Element, Neutrino Mass Hierarchy. arXiv:1802.04484v2 [hep-ph] 25 Oct 2018 PACS numbers: 12.60.Fr, 11.15.Ex, 23.40-s, 14.60.Pq Required sensitivity to search the neutrinoless double beta decay in 124Sn 2 1. Introduction Neutrinoless double-β decay (0νββ) is an interesting venue to look for the most important question whether neutrinos have Majorana or Dirac nature. -
Design and Construction of the Microboone Detector
BNL-113631-2017-JA Design and Construction of the MicroBooBE Detector The MicroBooNE Collaboration Submitted to Journal of Instrumentation January 17, 2017 Physics Department Brookhaven National Laboratory U.S. Department of Energy USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25) Notice: This manuscript has been co-authored by employees of Brookhaven Science Associates, LLC under Contract No. DE-SC0012704 with the U.S. Department of Energy. The publisher by accepting the manuscript for publication acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or any third party’s use or the results of such use of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof or its contractors or subcontractors. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof. -
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) -
Nuclear Physics
Nuclear Physics Overview One of the enduring mysteries of the universe is the nature of matter—what are its basic constituents and how do they interact to form the properties we observe? The largest contribution by far to the mass of the visible matter we are familiar with comes from protons and heavier nuclei. The mission of the Nuclear Physics (NP) program is to discover, explore, and understand all forms of nuclear matter. Although the fundamental particles that compose nuclear matter—quarks and gluons—are themselves relatively well understood, exactly how they interact and combine to form the different types of matter observed in the universe today and during its evolution remains largely unknown. Nuclear physicists seek to understand not just the familiar forms of matter we see around us, but also exotic forms such as those that existed in the first moments after the Big Bang and that exist today inside neutron stars, and to understand why matter takes on the specific forms now observed in nature. Nuclear physics addresses three broad, yet tightly interrelated, scientific thrusts: Quantum Chromodynamics (QCD); Nuclei and Nuclear Astrophysics; and Fundamental Symmetries: . QCD seeks to develop a complete understanding of how the fundamental particles that compose nuclear matter, the quarks and gluons, assemble themselves into composite nuclear particles such as protons and neutrons, how nuclear forces arise between these composite particles that lead to nuclei, and how novel forms of bulk, strongly interacting matter behave, such as the quark-gluon plasma that formed in the early universe. Nuclei and Nuclear Astrophysics seeks to understand how protons and neutrons combine to form atomic nuclei, including some now being observed for the first time, and how these nuclei have arisen during the 13.8 billion years since the birth of the cosmos. -
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. -
Arxiv:1906.07209V1 [Astro-Ph.HE] 17 Jun 2019 Hole-Black Hole and Neutron Star-Neutron Star Mergers)
POEMMA's target of opportunity sensitivity to cosmic neutrino transient sources Tonia M. Venters Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Mary Hall Reno Department of Physics and Astronomy, University of Iowa, Iowa City, IA 52242, USA John F. Krizmanic CRESST/NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA University of Maryland, Baltimore County, Baltimore, MD 21250, USA Luis A. Anchordoqui Department of Physics, Graduate Center, City University of New York (CUNY), NY 10016, USA Department of Physics and Astronomy, Lehman College (CUNY), NY 10468, USA Department of Astrophysics, American Museum of Natural History, NY 10024, USA Claire Gu´epin Sorbonne Universit´e,CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98 bis bd Arago, 75014 Paris, France Angela V. Olinto Department of Astronomy & Astrophysics, KICP, EFI, The University of Chicago, Chicago, IL 60637, USA (Dated: June 19, 2019) We calculate the sensitivity of space-based cosmic neutrino detection from transient sources in the context of the Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) mission using Target- of-Opportunity (ToO) observations. POEMMA uses two spacecraft each with a large Schmidt telescope to simultaneously view the optical signals generated by extensive air showers (EASs). POEMMA is designed for both ultrahigh-energy cosmic ray and very-high-energy neutrino mea- surements. POEMMA has significant neutrino sensitivity starting in the 10 PeV decade via mea- surements of Cherenkov signals from upward-moving EASs initiated by tau neutrinos interacting in the Earth. For ToO observations, POEMMA uses the ability to quickly repoint (90◦ in 500 seconds) each of the two spacecraft to the direction of the transient source. -
The Hunt for Sub-Gev Dark Matter at Neutrino Facilities: a Survey of Past and Present Experiments
Prepared for submission to JHEP The hunt for sub-GeV dark matter at neutrino facilities: a survey of past and present experiments Luca Buonocore,a;b Claudia Frugiuele,c;d Patrick deNivervillee;f aDipartimento di Fisica, Università di Napoli Federico II and INFN, Sezione di Napoli, I-80126 Napoli, Italy bPhysik Institut, Universität Zürich, CH-8057 Zürich, Switzerland cCERN, Theoretical Physics Departments, Geneva, Switzerland dINFN, Sezione di Milano, Via Celoria 16, I-20133 Milano, Italy. eCenter for Theoretical Physics of the Universe, IBS, Daejeon 34126, Korea f T2, Los Alamos National Laboratory (LANL), Los Alamos, NM, USA E-mail: [email protected], [email protected], [email protected] Abstract: We survey the sensitivity of past and present neutrino experiments to MeV-GeV scale vector portal dark matter and find that these experiments possess novel sensitivity that has not yet fully explored. Taking αD = 0:1 and a dark photon to dark matter mass ratio of three, the combined recast of previous analyses of BEBC and a projection of NOνA’s sensitivity are found to rule out the scalar thermal target for dark matter masses between 10 MeV to 100 MeV with existing data, while CHARM-II and MINERνA place somewhat weaker limits. These limits can be dramatically improved by off-axis searches using the NuMI beamline and the MicroBooNE, MiniBooNE or ICARUS detectors, and can even begin to probe the Majorana thermal target. We conclude that past and present neutrino facilities can search for light dark matter concurrently with their neutrino program and reach a competitive sensitivity to proposed future experiments. -
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).