Introduction to Underground Physics
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IUPAP Report 41A
IUPAP Report 41a A Report on Deep Underground Research Facilities Worldwide (updated version of August 8, 2018) Table of Contents INTRODUCTION 3 SNOLAB 4 SURF: Sanford Underground Research Facility 10 ANDES: AGUA NEGRA DEEP EXPERIMENT SITE 16 BOULBY UNDERGROUND LABORATORY 18 LSM: LABORATOIRE SOUTERRAIN DE MODANE 21 LSC: LABORATORIO SUBTERRANEO DE CANFRANC 23 LNGS: LABORATORI NAZIONALI DEL GRAN SASSO 26 CALLIO LAB 29 BNO: BAKSAN NEUTRINO OBSERVATORY 34 INO: INDIA BASED NEUTRINO OBSERVATORY 41 CJPL: CHINA JINPING UNDERGROUND LABORATORY 43 Y2L: YANGYANG UNDERGROUND LABORATORY 45 IBS ASTROPHYSICS RESEARCH FACILITY 48 KAMIOKA OBSERVATORY 50 SUPL: STAWELL UNDERGROUND PHYSICS LABORATORY 53 - 2 - __________________________________________________INTRODUCTION LABORATORY ENTRIES BY GEOGRAPHICAL REGION Deep Underground Laboratories and their associated infrastructures are indicated on the following map. These laboratories offer low background radiation for sensitive detection systems with an external users group for research in nuclear physics, astroparticle physics, and dark matter. The individual entries on the Deep Underground Laboratories are primarily the responses obtained through a questionnaire that was circulated. In a few cases, entries were taken from the public information supplied on the lab’s website. The information was provided on a voluntary basis and not all laboratories included in this list have completed construction, as a result, there are some unavoidable gaps. - 3 - ________________________________________________________SNOLAB (CANADA) SNOLAB 1039 Regional Road 24, Creighton Mine #9, Lively ON Canada P3Y 1N2 Telephone: 705-692-7000 Facsimile: 705-692-7001 Email: [email protected] Website: www.snolab.ca Oversight and governance of the SNOLAB facility and the operational management is through the SNOLAB Institute Board of Directors, whose member institutions are Carleton University, Laurentian University, Queen’s University, University of Alberta and the Université de Montréal. -
Arxiv:2009.11757V1 [Physics.Ins-Det] 24 Sep 2020
Prepared for submission to JINST Characterization of Germanium Detectors for the First Underground Laboratory in Mexico. A. Aguilar-Arevaloa S. Alvarado-Mijangosb X. Bertouc C. Canetd M. A. Cruz-Péreze A. Deistingf A. Diasf J. C. D’Olivoa F. Favela-Péreza;c E. A.Garcésb;1 A. González Muñozb;1 J. O. Guerra-Pulidoa J. Mancera-Alejandrezg D. J. Marín-Lámbarrib M. Martinez Monteroa J. Monroef C. Iván Ortega-Hernándeza S. Palingh S. Peetersi D. Ruíz Esparza Rodríguezb P. R. Scovellh C. Türkoğlui;2 E. Vázquez-Jáureguib J. Waldingf aInstituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, CDMX, México bInstituto de Física, Universidad Nacional Autónoma de México, A. P. 20-364, México D. F. 01000, Mexico cCentro Atómico Bariloche, CNEA/CONICET/IB, Bariloche, Argentina dCentro de Ciencias de la Atmósfera, Universidad Nacional Autónoma de México, CDMX, 04110 Mexico ePrograma de Posgrado en Ciencias de la Tierra, Universidad Nacional Autónoma de México, Ciudad Universitaria, Coyoacán 04510, Ciudad de México, Mexico f Royal Holloway, University of London, Egham Hill, United Kingdom gFacultad de Ingeniería, Universidad Nacional Autónoma de México, Mexico hBoulby Underground Laboratory, Boulby Mine, Saltburn-by-the-Sea, United Kingdom iDepartment of Physics and Astronomy, University of Sussex, Brighton, United Kingdom E-mail: [email protected] Abstract: This article reports the characterization of two High Purity Germanium detectors per- formed by extracting and comparing their efficiencies using experimental data and Monte Carlo simulations. The efficiencies were calculated for pointlike γ-ray sources as well as for extended calibration sources. Characteristics of the detectors such as energy linearity, energy resolution and full energy peak efficiencies are reported from measurements performed on surface laboratories. -
Experimental Results on Neutrino Oscillations
Experimental results on neutrino oscillations Ubaldo Dore1 and Domizia Orestano2 1) Dipartimento di Fisica, Universit`adi Roma “La Sapienza” and I.N.F.N., Sezione di Roma, P. A. Moro 2, Roma, Italy 2) Dipartimento di Fisica, Universit`aRoma Tre and I.N.F.N., Sezione di Roma Tre, Via della Vasca Navale 84, Roma, Italy October 23, 2018 E-mail:[email protected] and orestano@fis.uniroma3.it PACS numbers:14.60.Pq, 13.15.+g This is an author-created, un-copyedited version of an article published in Reports on Progress in Physics. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The definitive publisher authenticated version is available online at http://www.iop.org/EJ/journal/RoPP. Abstract The phenomenon of neutrino oscillation has been firmly estab- lished: neutrinos change their flavour in their path from their source arXiv:0811.1194v1 [hep-ex] 7 Nov 2008 to observers. This paper is dedicated to the description of experimen- tal results in the oscillation field, of their present understanding and of possible future developments in the experimental neutrino oscillation physics. Contents 1 Introduction 3 2 Neutrino properties 5 1 3 Neutrino oscillations 8 3.1 Vacuum oscillations . 8 3.1.1 Threeflavormixing.................... 8 3.1.2 Thetwoflavormixing .................. 9 3.2 Matter oscillations . 10 3.3 Approximations for the oscillation probabilities . 12 3.4 Experimental determination of neutrino oscillation parameters 15 3.4.1 Disappearanceexperiments . 16 3.4.2 Appearanceexperiments . 17 4 Neutrino sources 17 4.1 Solarneutrinos ......................... -
Neutrino Mass Hierarchy Arxiv:1505.01891V3 [Hep-Ex] 30 Jun 2015
Neutrino Mass Hierarchy X. Qian1∗and P. Vogel2y 1 Physics Department, Brookhaven National Laboratory, Upton, NY, USA 2 Kellogg Radiation Laboratory, California Institute of Technology, Pasadena, CA, USA July 1, 2015 Abstract The neutrino mass hierarchy, i.e., whether the ν3 neutrino mass eigenstate is heavier or lighter than the ν1 and ν2 mass eigenstates, is one of the remaining undetermined fundamental features of the neutrino Standard Model. Its determination would represent an important step in the formulation of the generalized model, and would have a profound impact on the quest of the nature of neutrinos (Dirac or Majorana) and the search for a theory of flavor. In this review, we summarize the status of experimental and theoretical work in this field and explore the future opportunities that emerge in light of the recently discovered non-zero and relatively large third neutrino mixing angle θ13. Contents 1 Introduction 2 2 Various Methods to Determine the Mass Hierarchy 9 2.1 The \Large" Third Neutrino Mixing Angle θ13 .......................9 2.2 Mass Hierarchy from Accelerator Neutrinos Appearance . 10 2.3 Mass Hierarchy from Atmospheric neutrinos . 15 2.4 Mass Hierarchy from Reactor Antineutrinos . 19 arXiv:1505.01891v3 [hep-ex] 30 Jun 2015 2.5 Interpretation of Mass Hierarchy Sensitivity . 22 2.5.1 Bayesian Approach to the Mass Hierarchy Determination . 24 2.5.2 Frequentist Approach to the Mass Hierarchy Determination . 24 3 Experiments 26 3.1 Current Status . 27 3.1.1 Atmospheric neutrino results from Super-Kamiokande . 27 2 3.1.2 Global Analysis of the j∆m32j Mass-squared Splitting .