DOCSLIB.ORG

The Numi Neutrino Beam

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Numi Neutrino Beam The NuMI neutrino beam The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Adamson, P., K. Anderson, M. Andrews, R. Andrews, I. Anghel, D. Augustine, A. Aurisano, et al. 2016. “The NuMI Neutrino Beam.” Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 806 (January): 279–306. doi:10.1016/j.nima.2015.08.063. Published Version doi:10.1016/j.nima.2015.08.063 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:30781092 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Open Access Policy Articles, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#OAP The NuMI Neutrino Beam P. Adamsond, K. Andersond, M. Andrewsd, R. Andrewsd, I. Anghelv,i, D. Augustined, A. Aurisanoc, S. Avvakumovau, D. S. Ayresi, B. Ballerd, B. Barishg, G. Barrak, W. L. Barrettbf, R. H. Bernsteind, J. Biggsd, M. Bishaim, A. Blakeb, V. Boceand, G. J. Bockd, D. J. Boehnleind, D. Bogertd, K. Bourklandd, S. V. Caoay, C. M. Castromontebc, S. Childressd, B. C. Choudharyd, J. A. B. Coelhoba,bb, J. H. Cobbak, L. Corwinas,w, D. Craned, J. P. Cravensay, D. Cronin-Hennessyaf, R. J. Ducard,bi, J. K. de Jongak, A. V. Devanbg, N. E. Devenishaw, M. V. Diwanm, A. R. Erwinbh,bi, C. O. Escobarbb, J. J. Evansad, E. Falkaw, G. J. Feldmanr, T. H. Fieldsi, R. Fordd, M. V. Frohnes,bi, H. R. Gallagherba, V. Garkushaao, R. A. Gomesbc, M. C. Goodmani, P. Gouffonbd, N. Grafu, R. Granah, N. Grossmand, K. Grzelakbe, A. Habigah, S. R. Hahnd, D. Hardingd, D. Harrisd, P. G. Harrisaw, J. Hartnellaw, R. Hatcherd, S. Haysd, K. Helleraf, A. Holinf, J. Huangay, J. Hylend, A. Ibrahimd, D. Indurthyay, G. M. Irwinau, Z. Isvanm,an, D. E. Jaffem, C. Jamesd, D. Jensend, J. Johnstoned, T. Kafkaba, S. M. S. Kasaharaaf, G. Koizumid, S. Koppay, M. Kordoskybg, A. Kreymerd, K. Langay, C. Laughtond, G. Lefeuvreaw, J. Lingm, P. J. Litchfieldaf,e, L. Loiaconoay, P. Lucasd, W. A. Mannba, A. Marchionnid, M. L. Marshakaf, N. Mayerba,w, C. McGivernan, M. M. Medeirosbc, R. Mehdiyevay, J. R. Meieraf, M. D. Messierw,r, D. G. Michaelg,bi, R. H. Milburnba, J. L. Millery,bi, W. H. Milleraf, S. R. Mishraar, S. Moed Sherd, C. D. Moored, J. Morf´ınd, L. Mualemg, S. Mufsonw, S. Murgiaau, M. Murtaghm,bi, J. Musserw, D. Naplesan, J. K. Nelsonbg, H. B. Newmang, R. J. Nicholf, J. A. Nowakaf, J. O'Connorf, W. P. Oliverba, M. Olsend, M. Orchaniang, S. Ospreyak, R. B. Pahlkad, J. Paleyi, A. Parad, R. B. Pattersong, T. Patzakn, Z.ˇ Pavlovi´cay, G. Pawloskiaf,au, A. Perchf, E. A. Petersonaf, D. A. Petytaf, M. M. Pf¨utznerf, S. Phan-Buddi, R. K. Plunkettd, N. Poonthottathild, P. Prietod, D. Pushkad, X. Qiuau, A. Radovicbg, R. A. Rameikad, J. Ratchforday, B. Rebeld, R. Reillyd, C. Rosenfeldar, H. A. Rubinu, K. Ruddickaf, M. C. Sanchezv,i, N. Saoulidoud, L. Sauerd, J. Schnepsba, D. Schood, A. Schreckenbergeray,af, P. Schreineri, P. Shanahand, R. Sharmad, W. Smartd, C. Smithf, A. Sousac,r, A. Stefanikd, N. Taggaj, R. L. Talagai, G. Tassottod, J. Thomasf, J. Thompsonan,bi, M. A. Thomsonb, X. Tianar, A. Timmonsad, D. Tinsleyd, S. C. Togninibc, R. Tonerr, D. Torrettad, I. Trostinx,bi, G. Tzanakosj,bi, J. Urheimw, P. Vahlebg, K. Vazirid, E. Villegasd, B. Virenm, G. Vogeld, R. C. Webberd, A. Weberak,e, R. C. Webbax, A. Wehmannd, C. Whiteu, L. Whiteheadt,m, L. H. Whiteheadf, S. G. Wojcickiau, d d bg ao arXiv:1507.06690v2 [physics.acc-ph] 29 Jul 2015 M. L. Wong-Squires , T. Yang , F. X. Yumiceva , V. Zarucheisky , R. Zwaskad aLawrence Berkeley National Laboratory, Berkeley, California, 94720 USA bCavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 0HE, United Kingdom cDepartment of Physics, University of Cincinnati, Cincinnati, Ohio 45221, USA Preprint submitted to Nuclear Instruments and Methods in Physics Research A, July 30, 2015 dFermi National Accelerator Laboratory, Batavia, Illinois 60510, USA eRutherford Appleton Laboratory, Science and TechnologiesFacilities Council, Didcot, OX11 0QX, United Kingdom fDepartment of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, United Kingdom gLauritsen Laboratory, California Institute of Technology, Pasadena, California 91125, USA hDepartment of Physics and Astronomy, University of Alabama, Tuscaloosa, Alabama 35487, USA iArgonne National Laboratory, Argonne, Illinois 60439, USA jDepartment of Physics, University of Athens, GR-15771 Athens, Greece kDepartment of Physics, National Tech. University of Athens, GR-15780 Athens, Greece lPhysics Department, Benedictine University, Lisle, Illinois 60532, USA mBrookhaven National Laboratory, Upton, New York 11973, USA nAPC { Universit´eParis 7 Denis Diderot, 10, rue Alice Domon et L´eonieDuquet, F-75205 Paris Cedex 13, France oCleveland Clinic, Cleveland, Ohio 44195, USA pDepartment of Physics & Astrophysics, University of Delhi, Delhi 110007, India qGE Healthcare, Florence South Carolina 29501, USA rDepartment of Physics, Harvard University, Cambridge, Massachusetts 02138, USA sHoly Cross College, Notre Dame, Indiana 46556, USA tDepartment of Physics, University of Houston, Houston, Texas 77204, USA uDepartment of Physics, Illinois Institute of Technology, Chicago, Illinois 60616, USA vDepartment of Physics and Astronomy, Iowa State University, Ames, Iowa 50011 USA wIndiana University, Bloomington, Indiana 47405, USA xHigh Energy Experimental Physics Department, ITEP, B. Cheremushkinskaya, 25, 117218 Moscow, Russia yPhysics Department, James Madison University, Harrisonburg, Virginia 22807, USA zNuclear Nonproliferation Division, Threat Reduction Directorate, Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA aaNuclear Physics Department, Lebedev Physical Institute, Leninsky Prospect 53, 119991 Moscow, Russia abLawrence Livermore National Laboratory, Livermore, California 94550, USA acLos Alamos National Laboratory, Los Alamos, New Mexico 87545, USA adSchool of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, United Kingdom aeLincoln Laboratory, Massachusetts Institute of Technology, Lexington, Massachusetts 02420, USA afUniversity of Minnesota, Minneapolis, Minnesota 55455, USA agMath, Science and Technology Department, University of Minnesota { Crookston, Crookston, Minnesota 56716, USA ahDepartment of Physics, University of Minnesota Duluth, Duluth, Minnesota 55812, USA aiCenter for Cosmology and Astro Particle Physics, Ohio State University, Columbus, Ohio 43210 USA ajOtterbein College, Westerville, Ohio 43081, USA akSubdepartment of Particle Physics, University of Oxford, Oxford OX1 3RH, United Kingdom alDepartment of Physics, Pennsylvania State University, State College, Pennsylvania 16802, USA amDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, Pennsylvania 19104, USA anDepartment of Physics and Astronomy, University of Pittsburgh, Pittsburgh, Pennsylvania 15260, USA aoInstitute for High Energy Physics, Protvino, Moscow Region RU-140284, Russia apDepartment of Physics and Astronomy, University of Rochester, New York 14627 USA aqPhysics Department, Royal Holloway, University of London, Egham, Surrey, TW20 0EX, United Kingdom 2 arDepartment of Physics and Astronomy, University of South Carolina, Columbia, South Carolina 29208, USA asSouth Dakota School of Mines and Technology, Rapid City, South Dakota 57701, USA atStanford Linear Accelerator Center, Stanford, California 94309, USA auDepartment of Physics, Stanford University, Stanford, California 94305, USA avPhysics Department, St. John Fisher College, Rochester, New York 14618 USA awDepartment of Physics and Astronomy, University of Sussex, Falmer, Brighton BN1 9QH, United Kingdom axPhysics Department, Texas A&M University, College Station, Texas 77843, USA ayDepartment of Physics, University of Texas at Austin, 1 University Station C1600, Austin, Texas 78712, USA azTech-X Corporation, Boulder, Colorado 80303, USA baPhysics Department, Tufts University, Medford, Massachusetts 02155, USA bbUniversidade Estadual de Campinas, IFGW-UNICAMP, CP 6165, 13083-970, Campinas, SP, Brazil bcInstituto de F´ısica, Universidade Federal de Goi´as,CP 131, 74001-970, Goi^ania,GO, Brazil bdInstituto de F´ısica, Universidade de S~aoPaulo, CP 66318, 05315-970, S~aoPaulo, SP, Brazil beDepartment of Physics, University of Warsaw, Pasteura 5, PL-02-093 Warsaw, Poland bfPhysics Department, Western Washington University, Bellingham, Washington 98225, USA bgDepartment of Physics, College of William & Mary, Williamsburg, Virginia 23187, USA bhPhysics Department, University of Wisconsin, Madison, Wisconsin 53706, USA biDeceased. Abstract This paper describes the hardware and operations of the Neutrinos at the Main Injector (NuMI) beam at Fermilab. It elaborates on the design considerations for the beam as a whole and for individual elements. The most important design details of individual components are described. Beam monitoring systems and procedures, including the tuning and alignment of the beam and NuMI long- term performance, are also discussed. Keywords: Neutrinos, Long baseline, Beam, Target, Main Injector. 1. Introduction to The NuMI Beam The Neutrinos at the Main Injector (NuMI) neutrino beam [1, 2] was built at Fermilab to provide neutrinos for the MINOS [3] experiment, a long-baseline neutrino oscillation search, as well as for the COSMOS experiment [4], which was initially approved but subsequently
Load more

Recommended publications
  • New Projects in Underground Physics
    NEW PROJECTS IN UNDERGROUND PHYSICS MAURY GOODMAN High Energy Physics Division Argonne National Laboratory Argonne IL 60439 E-mail: [email protected] ABSTRACT A large fraction of neutrino research is taking place in facilities underground. In this paper, I review the underground facilities for neutrino research. Then I discuss ideas for future reactor experiments being considered to measure θ13 and the UNO proton decay project. 1. Introduction Large numbers of particle physicists first went underground in the early 1980’s to search for nucleon decay. Atmospheric neutrinos were a background to those experiments, but the study of atmospheric neutrinos has spearheaded tremendous progress in our understanding of the neutrino. Since neutrino cross sections, and hence event rates are fairly small, and backgrounds from cosmic rays often need to be minimized to measure a signal, many more other neutrino experiments are found underground. This includes experiments to measure solar ν’s, atmospheric ν’s, reactor ν’s, accelerator ν’s and neutrinoless double beta decay. In the last few years we have seen remarkable progress in understanding the neu- trino. Compelling evidence for the existence of neutrino mixing and oscillations has been presented by Super-Kamiokande1) in 1998, based on the flavor ratio and zenith angle distribution of atmospheric neutrinos. That interpretation is supported by anal- 2) arXiv:hep-ex/0307017v1 8 Jul 2003 yses of similar data from IMB, Kamiokande, Soudan 2 and MACRO. And 2002 was a miracle year for neutrinos, with the results from SNO3) and KamLAND4) solving the long standing solar neutrino puzzle and providing evidence for neutrino oscilla- tions using both neutrinos from the sun and neutrinos from nuclear reactors.
    [Show full text]
  • Experimental Froniers in Nucleon Decay
    Experimental Fron/ers in Nucleon Decay Ed Kearns, Boston University froner Hyper-K 10 35 LAr20 LAr10 10 34 Super-K 10 33 Lifetime Sensitivity (90% CL) IMB 10 32 1995 2000 2005 2010 2015 2020 2025 2030 2035 2040 Year ∼ 0.5 Mt yr exposure Star/ng /me? Guess 1 decade from now. by Super-K before next Adjust star/ng /me as you wish. generaon experiments 2 What moves us towards the froners? v Connue exposure v Improve analysis Super-K v Search in new channels v Next generaon experiments • Detector R&D NNN • Experiment proposals Hyper-Kamiokande 560 kton water cherenkov 99K PMTs (20% coverage) LBNE 10/20 kton LAr TPC surface/underground? GLACIER/LBNO 20 kton LAr TPC 2-phase LENA 51 kton liquid scin/llator 30,000 PMTs 3 How to improve exis/ng analyses v Sensi/vity is based on: v Achieve: higher efficiency, lower background rate v Also important: improve accuracy of model (signal and/or BG) (which may increase or reduce sensi/vity) v Also: reduce systemac uncertainty v None of this is easy – gains will be small and hard fought v Increased exposure – gains are now minimal 4 Super-Kamiokande I Time(ns) < 952 952- 962 962- 972 972- 982 982- 992 992-1002 1002-1012 Simple signature: back-to-back 1012-1022 1022-1032 1032-1042 reconstruc/on of EM showers. 1042-1052 1052-1062 1062-1072 1072-1082 1082-1092 Efficiency ∼45% dominated by >1092 0 670 nuclear absorp/on of π 536 402 268 Low background ∼0.2 events/100 ktyr in SK 134 0 0 500 1000 1500 2000 Times (ns) Relavely insensi/ve to PMT density.
    [Show full text]
  • Icecube Searches for Neutrinos from Dark Matter Annihilations in the Sun and Cosmic Accelerators
    UNIVERSITE´ DE GENEVE` FACULTE´ DES SCIENCES Section de physique Professeur Teresa Montaruli D´epartement de physique nucl´eaireet corpusculaire IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators. THESE` pr´esent´ee`ala Facult´edes sciences de l'Universit´ede Gen`eve pour obtenir le grade de Docteur `essciences, mention physique par M. Rameez de Kozhikode, Kerala (India) Th`eseN◦ 4923 GENEVE` 2016 i Declaration of Authorship I, Mohamed Rameez, declare that this thesis titled, 'IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators.' and the work presented in it are my own. I confirm that: This work was done wholly or mainly while in candidature for a research degree at this University. Where any part of this thesis has previously been submitted for a degree or any other qualifica- tion at this University or any other institution, this has been clearly stated. Where I have consulted the published work of others, this is always clearly attributed. Where I have quoted from the work of others, the source is always given. With the exception of such quotations, this thesis is entirely my own work. I have acknowledged all main sources of help. Where the thesis is based on work done by myself jointly with others, I have made clear exactly what was done by others and what I have contributed myself. Signed: Date: 27 April 2016 ii UNIVERSITE´ DE GENEVE` Abstract Section de Physique D´epartement de physique nucl´eaireet corpusculaire Doctor of Philosophy IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators.
    [Show full text]
  • Measurement of the + ̅ Charged Current Inclusive Cross Section
    Measurement of the �! + �!̅ Charged Current Inclusive Cross Section on Argon in MicroBooNE Krishan Mistry on behalf of the MicroBooNE Collaboration 15 March 2021 New Directions in Neutrino-Nucleus Scattering (NDNN) NuSTEC Workshop ICARUS T600 MicroBooNE SBND Importance of the �!-Ar cross section • MicroBooNE + SBN Program + DUNE ⇥ Employ Liquid Argon Time Projection Chambers (LArTPCs) arXiv:1503.01520 [physics.ins-det] • Primary signal channel for these experiments is �!– Ar CC interactions arXiv:2002.03005 [hep-ex] 15 March 2021 K Mistry 2 Building a Picture of �! Interactions ArgoNeuT is the first A handful of measurements measurement made on on other nuclei in the argon hundred MeV to GeV range ⇥ Sample of 13 selected events Nuclear Physics B 133, 205 – 219 (1978) Phys. Rev. D 102, 011101(R) (2020) ⇥ Gargamelle Phys. Rev. Lett. 113, 241803 (2014) ⇥ Phys. Rev. D 91, 112010 (2015) T2K J. High Energ. Phys. 2020, 114 (2020) ⇥ MINER�A Phys. Rev. Lett. 116, 081802 (2016) !! " !! " Argon Other 15 March 2021 K Mistry 3 What are we measuring? ! /!̅ " # • Total �!+ �!̅ Charged Current (CC) ! ! $ /$ inclusive cross section • Signature: the neutrino event ? contains at least one electron-liKe shower Ar ⇥ No requirements on the presence (or absence) of any additional particle ⇥ Do not differentiate between �! and �!̅ Inclusive channel is the most straightforward channel to compare to predictions 15 March 2021 K Mistry 4 MicroBooNE • Measurement is performed • Features of a LArTPC using the MicroBooNE detector: LArTPC ⇥ Precise calorimetry ⇥ 4�
    [Show full text]
  • U·M·I University Microfilms International a Bell & Howell Lntormanon Company 300 North Zeeb Road
    INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copysubmitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adverselyaffect reproduction. In the unlikely.event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. Also, if unauthorized copyrightmaterial had to be removed, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, charts) are reproduced by sectioning the original, beginning at the upper left-hand corner and continuing from left to right in equal sections with small overlaps. Each original is also photographed in one exposure and is included in reduced form at the back of the book. Photographs included in the original manuscript have been reproduced xerographically in this copy. Higher quality 6" x 9" black and white photographic prints are available for any photographs or illustrations appearing in this copy for an additional charge. Contact UMI directly to order. U·M·I University Microfilms International A Bell & Howell lntormanon Company 300 North Zeeb Road. Ann Arbor. M148106-1346 USA 313/761-4700 800/521-0600 Order Number 9416065 A treatise on high energy muons in the 1MB detector McGrath, Gary G., Ph.D. University of Hawaii, 1993 V·M·I 300N.
    [Show full text]
  • First MINOS Results from the Numi Beam Nathaniel Tagg, for the MINOS Collaboration Tufts University, 4 Colby Street, Medford, MA, USA 02155 FERMILAB-CONF-06-130-E
    First MINOS Results from the NuMI Beam Nathaniel Tagg, for the MINOS Collaboration Tufts University, 4 Colby Street, Medford, MA, USA 02155 FERMILAB-CONF-06-130-E As of December 2005, the MINOS long-baseline neutrino oscillation experiment collected data with an exposure of 0.93 × 1020 protons on target. Preliminary analysis of these data reveals a result inconsistent with a no- oscillation hypothesis at level of 5.8 sigma. The data are consistent with neutrino oscillations reported by m2 . +0.60 × − 2 θ . +0.12 Super-Kamiokande and K2K, with best fit parameters of ∆ 23 = 3 05−0.55 10 3 and sin 2 23 = 0 88−0.15. 1. Introduction end of the run period in March 2006, the maximum in- tensity delivered to the target was in excess of 25 1012 × The MINOS long-baseline neutrino oscillation ex- protons per pulse, with a maximum target power of periment [1] was designed to accurately measure neu- 250 kW. trino oscillation parameters by looking for νµ disap- pearance. MINOS will improve the measurements of ∆m223 first performed by the Super-Kamiokande 3. The MINOS Detectors [2, 3] and K2K experiments [4]. In addition, MINOS is capable of searching for sub-dominant νµ νe os- The MINOS Near and Far detectors are constructed cillations, can look for CPT-violating modes→ by com- to have nearly identical composition and cross-section. paring νµ toν ¯µ oscillations, and is used to observe The detectors consist of sandwiches of 2.54 cm thick atmospheric neutrinos [5]. steel and 1 cm thick plastic scintillator, hung verti- The MINOS experiment uses a beam of νµ created cally.
    [Show full text]
  • Alpha Backgrounds and Their Implications for Neutrinoless Double-Beta Decay Experiments Using Hpge Detectors
    Alpha Backgrounds and Their Implications for Neutrinoless Double-Beta Decay Experiments Using HPGe Detectors Robert A. Johnson A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy University of Washington 2010 Program Authorized to Offer Degree: Physics University of Washington Graduate School This is to certify that I have examined this copy of a doctoral dissertation by Robert A. Johnson and have found that it is complete and satisfactory in all respects, and that any and all revisions required by the final examining committee have been made. Chair of the Supervisory Committee: John F. Wilkerson Reading Committee: Steven R. Elliott Nikolai R. Tolich John F. Wilkerson Date: In presenting this dissertation in partial fulfillment of the requirements for the doctoral degree at the University of Washington, I agree that the Library shall make its copies freely available for inspection. I further agree that extensive copying of this dissertation is allowable only for scholarly purposes, consistent with “fair use” as prescribed in the U.S. Copyright Law. Requests for copying or reproduction of this dissertation may be referred to Proquest Information and Learning, 300 North Zeeb Road, Ann Arbor, MI 48106-1346, 1-800-521-0600, to whom the author has granted “the right to reproduce and sell (a) copies of the manuscript in microform and/or (b) printed copies of the manuscript made from microform.” Signature Date University of Washington Abstract Alpha Backgrounds and Their Implications for Neutrinoless Double-Beta Decay Experiments Using HPGe Detectors Robert A. Johnson Chair of the Supervisory Committee: Professor John F.
    [Show full text]
  • INO/ICAL/PHY/NOTE/2015-01 Arxiv:1505.07380 [Physics.Ins-Det]
    INO/ICAL/PHY/NOTE/2015-01 ArXiv:1505.07380 [physics.ins-det] Pramana - J Phys (2017) 88 : 79 doi:10.1007/s12043-017-1373-4 Physics Potential of the ICAL detector at the India-based Neutrino Observatory (INO) The ICAL Collaboration arXiv:1505.07380v2 [physics.ins-det] 9 May 2017 Physics Potential of ICAL at INO [The ICAL Collaboration] Shakeel Ahmed, M. Sajjad Athar, Rashid Hasan, Mohammad Salim, S. K. Singh Aligarh Muslim University, Aligarh 202001, India S. S. R. Inbanathan The American College, Madurai 625002, India Venktesh Singh, V. S. Subrahmanyam Banaras Hindu University, Varanasi 221005, India Shiba Prasad BeheraHB, Vinay B. Chandratre, Nitali DashHB, Vivek M. DatarVD, V. K. S. KashyapHB, Ajit K. Mohanty, Lalit M. Pant Bhabha Atomic Research Centre, Trombay, Mumbai 400085, India Animesh ChatterjeeAC;HB, Sandhya Choubey, Raj Gandhi, Anushree GhoshAG;HB, Deepak TiwariHB Harish Chandra Research Institute, Jhunsi, Allahabad 211019, India Ali AjmiHB, S. Uma Sankar Indian Institute of Technology Bombay, Powai, Mumbai 400076, India Prafulla Behera, Aleena Chacko, Sadiq Jafer, James Libby, K. RaveendrababuHB, K. R. Rebin Indian Institute of Technology Madras, Chennai 600036, India D. Indumathi, K. MeghnaHB, S. M. LakshmiHB, M. V. N. Murthy, Sumanta PalSP;HB, G. RajasekaranGR, Nita Sinha Institute of Mathematical Sciences, Taramani, Chennai 600113, India Sanjib Kumar Agarwalla, Amina KhatunHB Institute of Physics, Sachivalaya Marg, Bhubaneswar 751005, India Poonam Mehta Jawaharlal Nehru University, New Delhi 110067, India Vipin Bhatnagar, R. Kanishka, A. Kumar, J. S. Shahi, J. B. Singh Panjab University, Chandigarh 160014, India Monojit GhoshMG, Pomita GhoshalPG, Srubabati Goswami, Chandan GuptaHB, Sushant RautSR Physical Research Laboratory, Navrangpura, Ahmedabad 380009, India Sudeb Bhattacharya, Suvendu Bose, Ambar Ghosal, Abhik JashHB, Kamalesh Kar, Debasish Majumdar, Nayana Majumdar, Supratik Mukhopadhyay, Satyajit Saha Saha Institute of Nuclear Physics, Bidhannagar, Kolkata 700064, India B.
    [Show full text]
  • MINOS+: Running the MINOS Detectors in the Numi-Nova Beam
    MINOS+: Running the MINOS Detectors in the Numi-NOvA Beam (FNAL P-1016) Presented by Alexander Radovic of University College London on behalf of the MINOS Collaboration. The Proposal: The Physics Reach: By continuing to the run the MINOS detectors during the NOvA Era Not only could MINOS+ augment the sin22ϴ and Δm2 we would hope to not only help NOvA improve on its measurement measurements of NOvA, it could also represent an opportunity of the oscillation parameters but also to probe new and interesting to probe some interesting areas of new physics. Such as: areas of physics, as well as improve our understanding of the neutrino beam flux. The Study of High Energy Neutrinos. Until now most neutrino oscillation experiments have focused on the lower The diagram on the right energies where the PMNS scenario tells us oscillations will shows the approximate occur. The MINOS detectors however would see the high energy regime that the MINOS energy tail of the NOvA beam, allowing for investigation MINOS detectors will be beyond the PMNS model of oscillations. sensitive to. Clearly very different to the spectrum The Search for seen at the NOvA Sterile Neutrinos. detectors it would give a NOvA The MINOS detectors window into a completely will see a large νμ flux different physical domain. from the NOvA beam which is perfect for With the MINOS detectors searching for a sterile we have a unique neutrino with opportunity to secure 2 2 2 m 4-m 3=O(1eV ) as Fermilab's position as a it would cause the world leader in Neutrino disappearance of research.
    [Show full text]
  • Upgrade of the Minos+ Experiment Data Acquisition for the High Energy Numi Beam Run
    FERMILAB-CONF-14-503-ND (accepted) Upgrade of the Minos+ Experiment Data Acquisition for the High Energy NuMI Beam Run William Badgett, Steve R. Hahn, Donatella Torretta, Jerry Meier, Jeffrey Gunderson, Denise Osterholm, David Saranen Abstract–The Minos+ experiment is an extension of the Minos Minos was designed a number of years before data taking experiment at a higher energy and more intense neutrino beam, commenced; by dint of technical progress, some of the with the data collection having begun in the fall of 2013. The electronics technology involved has become obsolete. The neutrino beam is provided by the Neutrinos from the Main Minos+ experiment was approved to extend the Minos data set Injector (NuMI) beam-line at Fermi National Accelerator Laboratory (Fermilab). The detector apparatus consists of two in the Noνa [2] NuMI beam era [3] with a higher energy and main detectors, one underground at Fermilab and the other in more intense neutrino beam. Both improved beam features Soudan, Minnesota with the purpose of studying neutrino result in higher signal occupancies in the Minos detector, and oscillations at a base line of 735 km. The original data especially so at the near detector located at Fermilab. The acquisition system has been running for several years collecting near detector is situated at 371 meters from the decay pipe, data from NuMI, but with the extended run from 2013, parts of while the far detector is 735 km away. At the peak beam the system needed to be replaced due to obsolescence, reliability problems, and data throughput limitations. Specifically, we have intensities of the high-energy run, we expect twenty neutrino replaced the front-end readout controllers, event builder, and interactions at the near detector per spill of ten micro-seconds data acquisition computing and trigger processing farms with duration at the near detector, compared to a maximum of three modern, modular and reliable devices with few single points of in the run ending in 2011.
    [Show full text]
  • The Minerνa Detector Construction Database
    The MINERνA detector construction database Moureen Kemei Mount Holyoke College Physics Department South Hadley, MA, 01075 Supervisor: Dave J Boehnlein Particle Physics Department MINERνA Experiment Fermi National Accelerator Laboratory Batavia, IL, 60510 2009 Summer Internship in Science and Technology(SIST) Program Abstract We describe the construction database for the MINERν-A detector. MINERν- A is a low mass fully active neutrino detector that is designed to study low-energy neutrino interactions. The detector database keeps track of all detector components, illustrates the relationship between different compo- nents, simplifies future data entry and record maintenance. The database is written in Structured Query Language (MySQL). A Python graphical user interface for the detector has been developed. Contents 0.1 Introduction . 2 0.2 Background . 3 0.2.1 The NuMI Beam . 3 0.2.2 The Minerva Detector . 4 0.2.3 Event Reconstruction and Particle Identification . 7 0.3 The Construction Database . 8 0.3.1 Module Table . 9 0.3.2 Outer Detector Table . 10 0.3.3 Plane Table . 11 0.3.4 Outer Detector Channel Table . 12 0.3.5 Outer ECAL Table . 12 0.3.6 Graphical User Interface (GUI) for the database . 12 0.4 Summary and Conclusions . 13 0.5 Acknowledgements . 13 1 0.1 Introduction The Main INjector Experiment for ν-A (MINERνA) is a neutrino scattering experiment that will study low energy ν-nucleus interactions to high preci- sion. The NuMI (neutrino's from the main injector) beamline at Fermilab provides an intense ν(neutrino) beam for the MINERνA detector. Neutrinos outnumber protons, electrons and neutrons yet they are the most difficult particles to observe because they are weakly interacting, have a very small mass and possess no electric charge.
    [Show full text]
  • Component Study of the Numi Neutrino Beam for Noνa Experiment at Fermilab D
    Proceedings of the DAE Symp. on Nucl. Phys. 58 (2013) 822 Component study of the NuMI neutrino beam for NOνA experiment at Fermilab D. Grover1,* B. Mercurio2, K. K. Maan3, S. R. Mishra2 and V. Singh1 1Department of Physics, Banaras Hindu University, Varanasi - 221005, INDIA 2Deptartment of Physics and Astronomy, University of South Carolina, Columbia, SC 229208, USA 3Department of Physics, Panjab University, Chandigarh, INDIA * email:[email protected] 1. Introduction axis beam aids in rejecting backgrounds to the The neutrino beam, NuMI, from Fermilab’s electron neutrino appearance search. Fig. 1 shows Main Injector accelerator is the most intense the effect on neutrino energy spectrum for neutrino beam in the world. The experiment NOνA progressively larger off-axis angles. On-axis, the will use this neutrino beam to study neutrino beam produces a neutrino flux peaked at 7 GeV oscillation where neutrino of a given flavor [2]. oscillates into another flavor. The oscillation is parameterized by the PMNS mixing-matrix and the mass squared differences between the three masses. Thus, there are six variables that affect neutrino oscillation: the three mixing angles θ12, θ23 and θ13, a CP-violating phase δ, and two mass-differences. The angles θ12 and θ23 have been measured to be non zero by several experiments. In 2012, the last angle, θ13, was measured at Daya Bay/Reno to be non zero to a statistical significance of 5.2σ [1]. No measurement of the CP-violating phase, δ has been made. Furthermore, whereas the absolute values of two mass square differences are known, the ordering of the masses has not been determined.
    [Show full text]