ICRC 2021 Programme
Total Page：16
File Type：pdf, Size：1020Kb
Load more
Recommended publications
-
Presentation File
The Future of High Energy Physics and China’s Role Yifang Wang Institute of High Energy Physics, Beijing HKUST, Sep. 24, 2018 A Very Active Field ILC,FCC, China-based LHC: ATLAS/CMS CEPC/SPPC High China-participated Others Energy Compositeness AMS, PAMELA Extra-dimensions Supersymmetry Antimatter Higgs CP violation Daya Bay, JUNO,T2K,Nova, SuperK,HyperK,LBNF/DUNE, Icecube/PINGU, KM3net/ORKA, Neutrinos SNO+,EXO/nEXO, KamLAND-Zen, Precision Standard COMET, tests Model Gerda,Katrin… mu2e, g-2, K-decays,… Hadron physics Cosmology & QCD Standard Model of Cosmology Rare decays Dark matter LUX, Xenon, LZ, BESIII,LHCb, Axions PandaX, CDEX, High BELLEII, Darkside, … precision PANDA,… ADMX,… Fermi, DAMPE, AMS,… 2 Roadmaps of HEP in the World • Japan (2012) – If new particles(e.g. Higgs) are discovered, build ILC – If θ13 is big enough, build HyperK and T2HK • EU (2013) – Continue LHC, upgrade its luminosity, until 2035 – Study future circular collider (FCC-hh or FCC-ee) • US (2014) – Build long baseline neutrino facility LBNF/DUNE – Study future colliders A new round of roadmap study is starting 3 Where Are We Going ? • ILC is a machine we planned for ~30 years, way before the Higgs boson was discovered. Is it still the only machine for our future ? • Shall we wait for results from LHC/HL-LHC to decide our next step ? • What if ILC could not be approved ? • What is the future of High Energy Physics ? • A new route: – Thanks to the low mass Higgs, there is a possibility to build a circular e+e- collider(Higgs factory) followed by a proton machine in the same tunnel – This idea was reported for the first time at the “Higgs Factory workshop(HF2012)” in Oct. -
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 -
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 -
Effective Neutrino Masses in KATRIN and Future Tritium Beta-Decay Experiments
PHYSICAL REVIEW D 101, 016003 (2020) Effective neutrino masses in KATRIN and future tritium beta-decay experiments † ‡ Guo-yuan Huang,1,2,* Werner Rodejohann ,3, and Shun Zhou1,2, 1Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China 2School of Physical Sciences, University of Chinese Academy of Sciences, Beijing 100049, China 3Max-Planck-Institut für Kernphysik, Postfach 103980, D-69029 Heidelberg, Germany (Received 25 October 2019; published 3 January 2020) Past and current direct neutrino mass experiments set limits on the so-called effective neutrino mass, which is an incoherent sum of neutrino masses and lepton mixing matrix elements. The electron energy spectrum which neglects the relativistic and nuclear recoil effects is often assumed. Alternative definitions of effective masses exist, and an exact relativistic spectrum is calculable. We quantitatively compare the validity of those different approximations as function of energy resolution and exposure in view of tritium beta decays in the KATRIN, Project 8, and PTOLEMY experiments. Furthermore, adopting the Bayesian approach, we present the posterior distributions of the effective neutrino mass by including current experimental information from neutrino oscillations, beta decay, neutrinoless double-beta decay, and cosmological observations. Both linear and logarithmic priors for the smallest neutrino mass are assumed. DOI: 10.1103/PhysRevD.101.016003 I. INTRODUCTION region close to its end point will be distorted in com- parisontothatinthelimitofzeroneutrinomasses.This Neutrino oscillation experiments have measured with kinematic effect is usually described by the effective very good precision the three leptonic flavor mixing neutrino mass [7] angles fθ12; θ13; θ23g and two independent neutrino 2 2 2 2 mass-squared differences Δm21 ≡ m2 − m1 and jΔm31j≡ qffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi 2 − 2 2 2 2 2 2 2 jm3 m1j. -
Neutrino Mass Analysis with KATRIN
Technical University Munich Max Planck Institute for Physics Physics Department Werner Heisenberg Institute Advanced Lab Course Neutrino Mass Analysis with KATRIN Christian Karl, Susanne Mertens, Martin Slezák Last edited: September 2, 2020 Contents 1 Introduction 3 2 The KATRIN Experiment5 2.1 Neutrino Mass Determination from Beta-Decay............................5 2.2 Molecular Tritium as Beta-Decay Source................................6 2.3 Measuring Principle: MAC-E Filter Electron Spectroscopy.....................7 2.4 Experimental Setup.............................................8 2.4.1 Rear Section.............................................8 2.4.2 Windowless Gaseous Tritium Source..............................8 2.4.3 Pumping Sections.........................................9 2.4.4 Pre- and Main-Spectrometer...................................9 2.4.5 Focal Plane Detector........................................ 10 2.5 Modelling of the Integrated Beta-Decay Spectrum.......................... 10 2.5.1 Final State Distribution...................................... 10 2.5.2 Doppler Effect........................................... 11 2.5.3 Response Function......................................... 12 2.5.4 Model of the Rate Expectation................................. 13 3 Basic Principles of Data Analysis 15 3.1 Maximum Likelihood Analysis...................................... 15 3.2 Interval Estimation............................................. 16 4 Tasks 18 4.1 Understanding the Model........................................ -
Geo-Neutrino Program at Baksan Neutrino Observatory
Geo-neutrino Program at Baksan Neutrino Observatory Yu.M. Malyshkin1,4, A.N. Fazilakhmetov1, A.M. Gangapshev1,3, V.N. Gavrin1, T.V. Ibragimova1, M.M. Kochkarov1, V.V. Kazalov1, D.Yu. Kudrin1, V.V. Kuzminov1,3, B.K. Lubsandorzhiev1, Yu.M. Malyshkin1,4, G.Ya. Novikova1, A.A. Shikhin1, A.Yu. Sidorenkov1, N.A. Ushakov1, E.P. Veretenkin1, D.M. Voronin1,E.A. Yanovich1 1Institute for Nuclear Research of RAS, Moscow, Russia 2Institute of Astronomy of RAS, Moscow, Russia 3Kabardino-Balkarian State University, Nalchik, Russia 4National Institute of Nuclear Physics, Rome, Italy “Neutrino Geoscience”, Prague October 20-23, 2019 Introduction Construction of a large volume scintillator detector has been discussed for a long time. The works aimed to its preparation has been resumed recently. We will discuss: ● Benefits of its location at Baksan Neutrino Observatory ● Its potential for geo-neutrino studies ● Current progress Neutrino Geoscience 2019 Yury Malyshkin et al, INR RAS 2 BNO Location BNO Nalchik Black See Neutrino Geoscience 2019 Yury Malyshkin et al, INR RAS 3 Baksan Valley Mountain Andyrchy Baksan valley Baksan Neutrino Observatory and Neutrino village Neutrino Geoscience 2019 Yury Malyshkin et al, INR RAS 4 BNO Facilities and Neutrino village Andyrchy EAS array Carpet-3 EAS array BUST Tunnel entrance Neutrino village Neutrino Geoscience 2019 Yury Malyshkin et al, INR RAS 5 Underground labs of BNO Entrance BUST’s hall Low Bkg Lab2 + Laser Interferom. 620 m – 1000 m w.e. Low Bkg Lab1 Low Bkg «НИКА» Lab3 GeoPhys «DULB- OGRAN’s hall GeoPhys Lab1 4900» Lab2 4000 m GGNT’s hall BLVST Neutrino Geoscience 2019 Yury Malyshkin et al, INR RAS 6 Muon shielding -9 Entrance (3.0±0.15)·10 μ/cm2/s Neutrino Geoscience 2019 Yury Malyshkin et al, INR RAS 7 Detector Layout The future neutrino detector at Baksan will have a standard layout, similar to KamLAND and Borexino, but with larger mass and deeper underground. -
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) -
Search for Neutrinos from TANAMI Observed AGN Using Fermi
Search for neutrinos from TANAMI observed AGN using Fermi lightcurves with ANTARES Suche nach Neutrinos von TANAMI-AGN unter Verwendung von Fermi-Lichtkurven mit ANTARES Der Naturwissenschaftlichen Fakultät der Friedrich-Alexander-Universität Erlangen-Nürnberg zur Erlangung des Doktorgrads Dr. rer. nat. vorgelegt von Kerstin Fehn Als Dissertation genehmigt von der Naturwissenschaftlichen Fakultät der Friedrich-Alexander Universität Erlangen-Nürnberg Tag der mündlichen Prüfung: 24.03.2015 Vorsitzender des Promotionsorgans: Prof. Dr. Jörn Wilms Gutachter/in: Prof. Dr. Gisela Anton Prof. Dr. Ulrich Katz ν Abstract Active galactic nuclei (AGN) are promising candidates for hadronic acceleration. The combination of radio, gamma ray and neutrino data should give information on their properties, especially concerning the sources of the high-energetic cosmic rays. Assuming a temporal correlation of gamma and neutrino emission in AGN the background of neutrino telescopes can be reduced using gamma ray lightcurves. Thereby the sensitivity for discovering cosmic neutrino sources is enhanced. In the present work a stacked search for a group of AGN with the ANTARES neutrino telescope in the Mediterranean is presented. The selection of AGN is based on the source sample of TANAMI, a multiwavelength observation program (radio to gamma rays) of extragalactic jets southerly of −30◦ declination. In the analysis lightcurves of the gamma satellite Fermi are used. In an unbinned maximum likelihood approach the test statistic in the background only case and in the signal and background case is determined. For the investigated 10% of data of ANTARES within the measurement time between 01.09.2008 and 30.07.2012 no significant excess is observed. -
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. -
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.