Astroparticles at CC-IN2P3 Rachid Lemrani, June 11Th, 2014 Astroparticle Experiments at CC-IN2P3

Total Page:16

File Type:pdf, Size:1020Kb

Astroparticles at CC-IN2P3 Rachid Lemrani, June 11Th, 2014 Astroparticle Experiments at CC-IN2P3 Centre de Calcul de l’Institut National de Physique Nucléaire et de Physique des Particules Astroparticles at CC-IN2P3 Rachid Lemrani, June 11th, 2014 Astroparticle experiments at CC-IN2P3 running soon later Astroparticles Gamma HESS-II CTA Extreme energies FERMI Origin Composition Neutrino ANTARES KM3NET Anti-matter Dark Matter Gravity Cosmic rays AUGER JEM-EUSO AMS02 Gravitational Waves VIRGO Adv VIRGO ET Cosmology Dark Matter Dark Matter EDELWEISS EURECA Dark Energy SuperNovae,WL,... SNLS / SNF LSST / EUCLID Parameters CMB PLANCK Neutrinos : Majorana/Mass ν-less double β Decay NEMO ! SuperNEMO Mixing Neutrino Oscillation OPERA ! ! D-CHOOZ ! ! T2K ! Proton decay LAGUNA Most computing intensive in the future : CTA, LSST, Euclid Astroparticle experiments at CC-IN2P3, June 11th 2014 !2 Planck Planck publication : 21st march 2013 ~ 5 MHS05.hour / month - CC-IN2P3 provided increased amount of computing before the publication Planck Astroparticle experiments at CC-IN2P3, June 11th 2014 !3 Astroparticle experiments at CC-IN2P3 Auger AMS HESS Supernovae ANTARES VIRGO Planck Fermi Opera Double-Chooz Nemo Edelweiss Astroparticle experiments at CC-IN2P3, June 11th 2014 !4 Astroparticle experiments at CC-IN2P3 DOUBLE-CHOOZ SPACE AMS FERMI EDELWEISS PLANCK CC-IN2P3 NEMO EUCLID VIRGO ANTARES OPERA T2K SNLS/SNF CTA ? LSST HESS AUGER Astroparticle experiments at CC-IN2P3, June 11th 2014 !5 Types of data ! Events : gammas, neutrinos, cosmic rays ! 1D signals : gravitational waves, CMB ! 2D Images : Supernovae ! run conditions : calibration, monitoring Astroparticle experiments at CC-IN2P3, June 11th 2014 !6 Types of storage ! Mass storage on tapes (HPSS) : large files ! Data analysis on Semi-Permanent Storage (GPFS) : SuperNovae, Planck ... ! Disks : gravitational waves, ... ! Shared files on AFS : programs, ... ! Databases : run conditions, parameters Astroparticle experiments at CC-IN2P3, June 11th 2014 !7 Data management and access ! Management with IRODS : data transfer, heterogeneous support : cartridges, disks, databases. Unix like commands to copy, list, search for files in a simple arborescence ! ! Access with XROOTD : well adapted to root files (other formats also possible) interfaced at CC-IN2P3 with HPSS Astroparticle experiments at CC-IN2P3, June 11th 2014 !8 Computing types ! Parallel processing MPI : CMB ! Signal processing : GW, CMB (1D → 2D maps) ! Images processing: Supernovae ! Events processing: reconstruction, analyses, ... ! Monte-Carlo simulations : - Atmospheric showers (auger, cta) - Propagation of light in the sea (antares) - Backgrounds for rare events detection (edelweiss, supernemo) - ... ! Interactive : programs tuning before mass computing Astroparticle experiments at CC-IN2P3, June 11th 2014 !9 Future !10 Future storage increased Increase expected by experiments Cumulated Disk TB Cumulated Tape TB 25000 40000 20000 30000 15000 20000 10000 10000 5000 0 0 2014 2015 2016 2017 2018 2013 2014 2015 2016 2017 2018 LCG AMS DCHOOZ AUGER VIRGO ANTARES HESS-II EUCLID LSST others Astroparticle experiments at CC-IN2P3, June 11th 2014 !11 CTA ! - 2016 to 2020 ??? deployment of the array -> Increasing data flow - From 2020 : of order 1 to 10 PB/year Astroparticle experiments at CC-IN2P3, June 11th 2014 !12 LSST : Large Synoptic Survey Telescope - Telescope ready for system Integration and testing : July 4 2019 - Camera ready : May 15, 2020 - Commissioning phase will be 24-36 months - 6 months minimum with the Commissioning camera - 18 months with camera for I&T and science verification ! CC-IN2P3 : • half of Data Release Production (other half by NCSA / Urbana Illinois) • will host all the processed data ! Challenges : • data volume 100s PB in 2030 ? • analysis type : images • scale gap wrt SNLS / SN Factory • Huge database : 10s PB of objects, sources, ... Astroparticle experiments at CC-IN2P3, June 11th 2014 !13 LSST - DATA CHALLENGE - Summer 2013 DC-2013 : First major DC involving both CC-IN2P3 and NCSA ! Using DATA from SDSS : SDSS DR7 survey in Stripe 82 : ~5 TB for CC-IN2P3: 298 runs and nearly 4 million images in 5 passbands ! CC-IN2P3 : - 1 millions CPU hours (HS06) - 40 000 jobs - Up to 700 batch slots - One dedicated interactive VM for debug, file transfer, ... - Tests of job submission using DIRAC (on z filter) - Up to 100 TB on sps (GPFS) / 20 million files - Data transfers using IRODS : 100 TB - MySQL server for produced catalog of objects ! Very challenging with only 5 TB of Raw data Astroparticle experiments at CC-IN2P3, June 11th 2014 !14 LSST - QSERV : Distributed LSST database Developped by SLAC & Caltech, contributions by LPC/IN2P3 Clermont Will host 34 PB with 9000 billons entries Overlapping partitions of the sky request results CC-IN2P3 : Test of QSERV platform with 310 nodes (in 2013) Very usefull uncovering unexpected issues : QSERV didn’t scale with more than 250 nodes Astroparticle experiments at CC-IN2P3, June 11th 2014 !15 EUCLID ■ Space mission 7 years, launch in 2020 - Dark Energy / Dark Matter, Gravity, Large Scale Structures ■ 2026 : ~ total 150 PB ? ■ 8 Science Data Centers ! ! ! ! ! ! ■ CC-IN2P3 : 30 % of total Processing and Storage ! Astroparticle experiments at CC-IN2P3, June 11th 2014 !16 Advanced Virgo Virgo shutdown Advanced Virgo : starting end 2015 ? 800 TB / year at CC-IN2P3 from 2019 ? ! - Computing : mainly at CC-IN2P3 and CNAF ! - Preparation for computing model for adv. virgo : ! challenges : type/amount of computing (GPU), heterogeneous clusters ! Virgo Astroparticle experiments at CC-IN2P3, June 11th 2014 !17 Prospects KM3NET high energy neutrinos CTA : gamma rays AUGER upgrade/extension JEM-EUSO : extreme energies EURECA : Dark Matter SUPERNEMO LAGUNA proton decay, neutrino v-less double beta decay advVIRGO /ET Gravitational waves LISA gravitational waves Euclid, LSST, Chile dark energy dark energy Astroparticle experiments at CC-IN2P3, June 11th 2014 !18 Backup Slides !19 CPU Consumption in 2012 2012 [HS06 Hrs] antares 22 637 176 pauger 17 549 325 hess 17 074 751 HESS dchooz 14 902 802 AUGER planck 9 255 537 ams 6 246 575 glast 6 051 319 16 % 15 % nemo 4 179 202 km3net 4 037 867 virgo 3 079 917 DOUBLE- t2k 1 175 106 CHOOZ nusol 965 334 14 % snovae 831 608 21 % trend 642 864 ANTARES lsst 536 866 cta 536 303 8 % xmm 247 230 integral 163 779 6 % sdss 117 093 5 % PLANCK 4 % opera 105 090 nucifer 89 243 jemeuso 62 015 AMS baoradio 7 686 NEMO edelweis 5 588 FERMI Total 110 253 047 Astroparticle experiments at CC-IN2P3, June 11th 2014 !20 Storage in 2012 - Tapes (HPSS) Mass Storage (TB) ams 885 VIRGO ANTARES virgo 819 819 TB antares 591 591 TB dchooz 587 hess 462 pauger 332 210 nemo DOUBLE- 153 snovae AMS baoradio 88 CHOOZ 885 TB cta 81 587 TB km3net 40 edelweis 31 t2k 29 sdss 27 planck 21 HESS 20 trend 462 TB NEMO AUGER 210 TB 332 TB - High performance disks (GPFS) : PLANCK : ~ 150TB SNLS : ~ 140 TB SNF : ~ 65TB Astroparticle experiments at CC-IN2P3, June 11th 2014 !21.
Recommended publications
  • 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
    [Show full text]
  • 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.
    [Show full text]
  • 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) .
    [Show full text]
  • Results in Neutrino Oscillations from Super-Kamiokande I
    Status of the RENO Reactor Neutrino Experiment RENO = Reactor Experiment for Neutrino Oscillation (For RENO Collaboration) K.K. Joo Chonnam National University February 15, 2011 Research Techniques Seminar @FNAL Outline Experiment Goals of the RENO Exp. - Short introduction - Expected q13 sensitivity - Systematic uncertainty Overview of the RENO Experiment - Experimental Setup of RENO - Schedule - Tunnel excavation - Status of detector construction - DAQ, data analysis tools Summary Brief History of Neutrinos 1930: Pauli postulated neutrino to explain b decay problem 1933: Fermi baptized the neutrino in his weak-interaction theory 1956: First discovery of neutrino by Reines & Cowan from reactor 1957: Neutrinos are left-handed by Glodhaber et al. 1962: Discovery of nm by Lederman et al. (Brookhaven Lab) 1974: Discovery of neutral currents due to neutrinos 1977: Tau lepton discovery by Perl et al. (SLAC) 1998: Atmospheric neutrino oscillation observed by Super-K 2000: nt discovery by DONUT (Fermilab) 2002: Solar neutrino oscillation observed by SNO and confirmed by Kamland What NEXT? Standard Model Neutrinos in SM Neutrino Oscillation . Three types of neutrinos exist & mixing among them Oscillation parameters (q12 , q23 , q13) Not measured yet . Elementary particles with almost no interactions . Almost massless: impossible to measure its mass Neutrino Mixing Parameters Matrix Components: νe Ue1 Ue2 Ue3 ν1 3 Angles (θ ; θ ; θ ) 12 13 23 ν U U U ν 1 CP phase (δ) μ μ1 μ2 μ3 2 2 Mass differences ντ Uτ1 Uτ2 Uτ3 ν3 1 0 0 c 0 s ei c s 0 13 13 12 12 U 0 c23 s23 0 1 0 s12 c12 0 i 0 s23 c23 s13e 0 c13 0 0 1 atmospheric SK, K2K The Next Big Thing? SNO, solar SK, KamLAND ≈ ≈ ° q23 qatm 45 q12 ≈qsol ≈ 32° Large and maximal mixing! Reduction of reactor neutrinos due to oscillations Disappearance Reactor neutrino disappearance Prob.
    [Show full text]
  • Letter of Interest Forthcoming Science from The
    Snowmass2021 - Letter of Interest Forthcoming Science from the PROSPECT-I Data Set Neutrino Frontier Topical Groups: (NF02) Sterile neutrinos (NF03) Beyond the Standard Model (NF07) Applications (NF09) Artificial neutrino sources Contact Information: Nathaniel Bowden (LLNL) [[email protected]] Karsten Heeger (Yale University) [[email protected]] Pieter Mumm (NIST) [[email protected]] M. Andriamirado,6 A. B. Balantekin,16 H. R. Band,17 C. D. Bass,8 D. E. Bergeron,10 D. Berish,13 N. S. Bowden,7 J. P.Brodsky,7 C. D. Bryan,11 R. Carr,9 T. Classen,7 A. J. Conant,4 G. Deichert,11 M. V.Diwan,2 M. J. Dolinski,3 A. Erickson,4 B. T. Foust,17 J. K. Gaison,17 A. Galindo-Uribarri,12, 14 C. E. Gilbert,12, 14 C. Grant,1 B. T. Hackett,12, 14 S. Hans,2 A. B. Hansell,13 K. M. Heeger,17 D. E. Jaffe,2 X. Ji,2 D. C. Jones,13 O. Kyzylova,3 C. E. Lane,3 T. J. Langford,17 J. LaRosa,10 B. R. Littlejohn,6 X. Lu,12, 14 J. Maricic,5 M. P.Mendenhall,7 A. M. Meyer,5 R. Milincic,5 I. Mitchell,5 P.E. Mueller,12 H. P.Mumm,10 J. Napolitano,13 C. Nave,3 R. Neilson,3 J. A. Nikkel,17 D. Norcini,17 S. Nour,10 J. L. Palomino,6 D. A. Pushin,15 X. Qian,2 E. Romero-Romero,12, 14 R. Rosero,2 P.T. Surukuchi,17 M. A. Tyra,10 R. L. Varner,12 D. Venegas-Vargas,12, 14 P.B.
    [Show full text]
  • APC Scientific Board 2017 Tech
    2012-2016 APC Laboratory Technical Activities T. Zerguerras on behalf of the Technical Departments 20/11/2017 APC Scientific Board 2017 1 Technical Departments Organisation Equipment, facilities and platform Instrumentation Department (Techniques Expérimentales) Electronics and Microelectronics Department Mechanics Department IT Department Quality Unit R&D: CMB µelectronic, Compton, GAMMACUBE, Liquido Analysis & Prospects 20/11/2017 APC Scientific Board 2017 2 General organisation • 5 technical departments + Quality Unit + the FACe platform • Building an instrument => combining skills 22/09/2017 APC Scientific Board 2017 3 Technical departments organisation Matrix organisation structure: Project/Department (Assignment to a department, participation to projects) One specific skill (Mechanics, Electronics/µelectronics, Instrumentation, IT, QA/PA) Transverse activities of the Quality Unit Supervision : Head of department Project coordination: Project manager Indicator Boards for activities and assignments monitoring Project Monitoring Committee (Comité de Suivi de Projets CSP) This organisation aims to create a bond of trust with funding and tutelage agencies 20/11/2017 APC Scientific Board 2017 4 Organisation: Technical staff evolution On 31/12 Technical departments staff evolution 60 Technical departments staff - Gender 45 50 40 40 35 34 30 30 33 35 38 38 Permanent 25 MEN Fixed-term 20 38 40 39 40 39 20 WOMEN 15 10 10 15 17 13 12 12 5 10 11 9 10 11 0 0 2012 2013 2014 2015 2016 2012 2013 2014 2015 2016 Technical departments
    [Show full text]
  • Muon Spallation in Double Chooz
    Muon Spallation in Double Chooz Claire Thomas∗ REU, Columbia University and MIT (Dated: August 10, 2009) This report presents my work for Double Chooz at MIT during the 2009 Summer REU program, funded by Columbia University. Double Chooz is a reactor neutrino experiment that aims to measure the mixing parameter θ13. The experiment detects electron antineutrinos via inverse beta decay. Neutrons and light nuclei made in muon spallation are a major background to the experiment. The delayed neutron emitter 9Li is especially problematic because it mimics the inverse beta decay signal. For this reason I studied muon spallation in Double Chooz, focusing on the production and subsequent decay of 9Li. There are two key differences between 9Li decay and inverse beta decay. The first is that 9Li is a β− decay, so it emits an electron, whereas inverse beta decay emits a positron. The second difference is the energy of the neutrons emitted. In 9Li decay the neutron energy is on the order of MeV, whereas the inverse beta decay neutron has a negligible kinetic energy. Since Double Chooz does not distinguish charge, the positrons and electrons are not easy to distinguish. First, I ran simulations of electrons and positrons in the Double Chooz detector and constructed a late light variable to distinguish them from electrons. This proved insufficient, so I wrote general software to simulate radioactive decays in the Double Chooz detector. In this report I present the deposited energy spectra of a few important decays. 1. INTRODUCTION The consequence of neutrino oscillation is that an ex- periment that is sensitive to only one of the three neu- 1.1.
    [Show full text]
  • A Deep Sea Telescope for High Energy Neutrinos
    A Deep Sea Telescope for High Energy Neutrinos The ANTARES Collaboration 31 May, 1999 arXiv:astro-ph/9907432v1 29 Jul 1999 CPPM-P-1999-02 DAPNIA 99-01 IFIC/99-42 SHEF-HEP/99-06 This document may be retrieved from the Antares web site: http://antares.in2p3.fr/antares/ Abstract The ANTARES Collaboration proposes to construct a large area water Cherenkov detector in the deep Mediterranean Sea, optimised for the detection of muons from high-energy astrophysical neutrinos. This paper presents the scientific motivation for building such a device, along with a review of the technical issues involved in its design and construction. The observation of high energy neutrinos will open a new window on the universe. The primary aim of the experiment is to use neutrinos as a tool to study particle acceleration mechanisms in energetic astrophysical objects such as active galactic nuclei and gamma-ray bursts, which may also shed light on the origin of ultra-high-energy cosmic rays. At somewhat lower energies, non-baryonic dark matter (WIMPs) may be detected through the neutrinos produced when gravitationally captured WIMPs annihilate in the cores of the Earth and the Sun, and neutrino oscillations can be measured by studying distortions in the energy spectrum of upward-going atmospheric neutrinos. The characteristics of the proposed site are an important consideration in detector design. The paper presents measurements of water transparency, counting rates from bioluminescence and potassium 40, bio-fouling of the optical modules housing the detectors photomultipliers, current speeds and site topography. These tests have shown that the proposed site provides a good-quality environment for the detector, and have also demonstrated the feasibility of the deployment technique.
    [Show full text]
  • Neutrino Oscillation Studies with Reactors
    REVIEW Received 3 Nov 2014 | Accepted 17 Mar 2015 | Published 27 Apr 2015 DOI: 10.1038/ncomms7935 OPEN Neutrino oscillation studies with reactors P. Vogel1, L.J. Wen2 & C. Zhang3 Nuclear reactors are one of the most intense, pure, controllable, cost-effective and well- understood sources of neutrinos. Reactors have played a major role in the study of neutrino oscillations, a phenomenon that indicates that neutrinos have mass and that neutrino flavours are quantum mechanical mixtures. Over the past several decades, reactors were used in the discovery of neutrinos, were crucial in solving the solar neutrino puzzle, and allowed the determination of the smallest mixing angle y13. In the near future, reactors will help to determine the neutrino mass hierarchy and to solve the puzzling issue of sterile neutrinos. eutrinos, the products of radioactive decay among other things, are somewhat enigmatic, since they can travel enormous distances through matter without interacting even once. NUnderstanding their properties in detail is fundamentally important. Notwithstanding that they are so very difficult to observe, great progress in this field has been achieved in recent decades. The study of neutrinos is opening a path for the generalization of the so-called Standard Model that explains most of what we know about elementary particles and their interactions, but in the view of most physicists is incomplete. The Standard Model of electroweak interactions, developed in late 1960s, incorporates À À neutrinos (ne, nm, nt) as left-handed partners of the three families of charged leptons (e , m , t À ). Since weak interactions are the only way neutrinos interact with anything, the un-needed right-handed components of the neutrino field are absent in the Model by definition and neutrinos are assumed to be massless, with the individual lepton number (that is, the number of leptons of a given flavour or family) being strictly conserved.
    [Show full text]
  • Groupe Neutrino
    Groupe Neutrino HCERES Report 2013-17 Present Composition •[9] permanents –Stavros Katsanevas* (Prof),Antoine Kouchner* (Prof), Thomas Patzak* (Prof), Véronique Van Elewyck (MC), Alessandra Tonazzo* (Prof) –Anatael Cabrera (CR), Jaime Dawson(CR), Davide Franco*(CR) –Thierry Lasserre* (DR CEA) [*HDR] •[4] postdocs –Marco Grassi, LiquidO, Marie Curie, –Anthony Onillon, Double Chooz, IN2P3, 15/09/2015 – 14/09/2018 –Christine Nielson, KM3NeT/ORCA, 09/2017 – –Stefan Wagner, LiquidO, CDD, July. 2017 – June. 2018 •[5] PhD students –Theodoros Avgitas*, CD , Antoine Kouchner, 11/2014 – 11/2017 –Simon Bourret*, AMX, Veronique Van Elewyk (Eduoard Kaminksi), 09/2015 –2018 –Timothée Gregoire*, CDE , Antoine Kouchner, 10/2015- 2018 –Yan Han, CSC, Anatael Cabrera, 09/2017 – 2020 –Andrea Scarpelli, CD , Thomas Patzak & Alessandra Tonazzo, 10/2016 – 2019 [*aussi membres du groupe Haute Energies – KM3NET] Recent Evolution (last 5 years) - I •Permanents Christiano Galbiati, DarkSide, invited professeur UPSC, 03/2016 – 12/2016 Fumihiko Suekane, LiquidO, chair Blaise-Pascal , 04/2017 – 11/2018 Michel Cribier (CEA DR), emeritus 2009 Herve de Kerret (DR), emeritus 2014 Francois Vannucci (PR), emeritus 2012 Daniel Vignaud (DR), emeritus 2007 Didier Kryn (CR), retired 2013 Michel Obolensky (CR), retired 2015 •Postdocs Hector Gomez, DoubleChooz/MuonTomography, labex UnivEarth (E4), 09/2014 - 09/2017 Joao de Abreu Barbosa Coelho, KM3NET ORCA, labex UnivEarth (E4), 12/2015 – 09/2017 Quentin Riffard, DarkSide, UnivEarth (E4), 11/2015 – 09/2017 Romain Roncin, Borexino/SOX,
    [Show full text]
  • Status of Neutrino Oscillations I: the Three-Neutrino Scenario
    International Workshop on Astroparticle and High Energy Physics PROCEEDINGS Status of neutrino oscillations I: the three-neutrino scenario Michele Maltoni∗ IFIC, CSIC/Universitat de Val`encia, Apt 22085, E{46071 Valencia, Spain YITP, SUNY at Stony Brook, Stony Brook, NY 11794-3840, USA E-mail: [email protected] Abstract: We present a global analysis of neutrino oscillation data within the three- neutrino oscillation scheme, including in our fit all the current solar neutrino data, the reactor neutrino data from KamLAND and CHOOZ, the atmospheric neutrino data from Super-Kamiokande and MACRO, and the first data from the K2K long-baseline accel- erator experiment. We determine the current best fit values and allowed ranges for the three-flavor oscillation parameters, discussing the relevance of each individual data set as well as the complementarity of different data sets. Furthermore, we analyze in detail the 2 2 status of the small parameters θ13 and ∆m21=∆m31, which fix the possible strength of CP violating effects in neutrino oscillations. Keywords: Neutrino mass and mixing; solar, atmospheric, reactor and accelerator neutrinos. 1. Introduction Recently, the Sudbury Neutrino Observatory (SNO) experiment [1] has released an im- proved measurement with enhanced neutral current sensitivity due to neutron capture on salt, which has been added to the heavy water in the SNO detector. This adds precious information to the large amount of data on neutrino oscillations published in the last few years. Thanks to this growing body of data a rather clear picture of the neutrino sector is starting to emerge. In particular, the results of the KamLAND reactor experiment [2] have played an important role in confirming that the disappearance of solar electron neu- trinos [3, 4, 5, 6, 7], the long-standing solar neutrino problem, is mainly due to oscillations and not to other types of neutrino conversions.
    [Show full text]
  • PROSPECT Upgrade
    Precision Reactor Upgrade significantly expands oscillation Oscillation and physics reach in unique parameter space ] prospect.yale.edu ] ] 2 2 90% CL 90% CL 2 90% CL SPECTrum Experiment: PROSPECT, 1 yr Sensitivity PROSPECT, 2 yr Optimized Sensitivity PROSPECT, 2 yr Optimized Sensitivity PROSPECT, 2 yr Sensitivity DANSS Exclusion PROSPECT, 2 yr Optimized Sensitivity, σspectrum = 5% [eV [eV PROSPECT, 2 yr Optimized Sensitivity NEOS Exclusion [eV DYB Exclusion KATRIN Exclusion 2 41 PROSPECT, Current Sensitivity 2 41 STEREO, Current Exclusion 2 41 PROSPECT-I demonstrated PROSPECT, Current Exclusion STEREO, Expected Sensitivity LBN CPV Ambiguity Limit m m 10 m SBL + Gallium Anomaly (RAA + Evolution), 95% CL Δ 10 Δ 10 Upgrade & Science Goals Δ excellent performance H. Pieter Mumm for the PROSPECT collaboration 6 Primary Physics Goals Li capture Search for sterile neutrino oscillation 1 1 1 • Nuclear recoil within unique parameter space important for the reactor anomaly and Long Baseline Electronic recoil experiments. 235 • High-resolution U spectrum and flux 10−1 10−1 10−1 measurement addresses observed shape 10−2 10−1 1 10−2 10−1 1 10−2 10−1 1 sin22θ sin22θ sin22 discrepancies 14 14 θ14 Pulse shape discrimination (PSD) PROSPECT measurement strategy capable scintillator with high light yield • Unique 6Li-doped liquid scintillator as inverse Left: Comparison of sterile oscillation sensitivities for current and projected PROSPECT-II datasets. allows for excellent background beta decay target; distinct IBD topology Center: Projected PROSPECT-II sensitivity compared to selected short-baseline reactor experiments. rejection and > 5%/ E resolution. • Highly segmented array for background Right: Overlap of three year PROSPECT-II sensitivity with relevant regions of parameter space rejection and event localization • ~ 7m baseline to very compact highly- PROSPECT-II uniquely addresses a high Δ m2 region between enriched reactor core provides unique 1 eV2 - 15 eV2, and will reach the 5o sin2(2�14) sensitivity over sensitivity at high Δ m2.
    [Show full text]