Worldwide Underground Facilities Jaret Heise, Science Director (On Behalf of Many!)
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Future Plan of the Pandax Experiment
Future plan of the PandaX Experiment - report at the CJPL International Advisory Committee meeting PandaX Collaboration, 9 Nov., 2016 The PandaX (Particle and astrophysical Xenon) observatory uses xenon as target and detector to search for WIMP particles as well as neutrinoless double beta decay (NLDBD) in 136Xe. At present, the PandaX-II experiment is in operation in CJPL-I. The future PandaX program will pursue the following three main directions: 1. Continue the operation of PandaX-II until a total of 2-year exposure; 2. Develop and operate a multi-ton multi-purpose liquid xenon experiment, PandaX-xT, to push further the dark matter search; 3. Develop and operate a 200-kg (upgradable to ton-scale) high pressure gas TPC (HpgTPC), PandaX-III, to search for NLDBD in 136Xe. Each direction is elaborated below. PandaX-II operation PandaX-II has published the world leading WIMP limit with a 99-day exposure, reaching an upper limit to spin-independent WIMP-nucleon cross section of 2.5x10-46cm2 [1]. The current plan is to maintain stable operation until we have data with a 2-year total live time. Calibration runs will be interleaved to monitor the detector response. The wealth of low background data will allow us to pursue many different physics analyses (in additional to the standard WIMP- nucleon elastic scattering), including constraints to generic WIMP-nucleon operators, light WIMPs, inelastic WIMPs, limits to solar and galactic axions, etc. We will also use the PandaX-II detector to test new technologies for a future multi-ton detector, e.g. online Kr removal, upgrade of the trigger/electronics system to achieve a lower threshold and a higher data bandwidth, alternative electron recoil and nuclear recoil calibrations, etc. -
Particle Dark Matter an Introduction Into Evidence, Models, and Direct Searches
Particle Dark Matter An Introduction into Evidence, Models, and Direct Searches Lecture for ESIPAP 2016 European School of Instrumentation in Particle & Astroparticle Physics Archamps Technopole XENON1T January 25th, 2016 Uwe Oberlack Institute of Physics & PRISMA Cluster of Excellence Johannes Gutenberg University Mainz http://xenon.physik.uni-mainz.de Outline ● Evidence for Dark Matter: ▸ The Problem of Missing Mass ▸ In galaxies ▸ In galaxy clusters ▸ In the universe as a whole ● DM Candidates: ▸ The DM particle zoo ▸ WIMPs ● DM Direct Searches: ▸ Detection principle, physics inputs ▸ Example experiments & results ▸ Outlook Uwe Oberlack ESIPAP 2016 2 Types of Evidences for Dark Matter ● Kinematic studies use luminous astrophysical objects to probe the gravitational potential of a massive environment, e.g.: ▸ Stars or gas clouds probing the gravitational potential of galaxies ▸ Galaxies or intergalactic gas probing the gravitational potential of galaxy clusters ● Gravitational lensing is an independent way to measure the total mass (profle) of a foreground object using the light of background sources (galaxies, active galactic nuclei). ● Comparison of mass profles with observed luminosity profles lead to a problem of missing mass, usually interpreted as evidence for Dark Matter. ● Measuring the geometry (curvature) of the universe, indicates a ”fat” universe with close to critical density. Comparison with luminous mass: → a major accounting problem! Including observations of the expansion history lead to the Standard Model of Cosmology: accounting defcit solved by ~68% Dark Energy, ~27% Dark Matter and <5% “regular” (baryonic) matter. ● Other lines of evidence probe properties of matter under the infuence of gravity: ▸ the equation of state of oscillating matter as observed through fuctuations of the Cosmic Microwave Background (acoustic peaks). -
Dark Matter, Oscillations, Exotics Subgroup
Dark matter from ZeV to aeV: 3rd IBS-MultiDark-IPPP Workshop Durham, November 2016 Juande ZZornozaornoza (IFIC, UV-CSIC) Introduction X-rays and sterile neutrinos Neutrino telescopes Results . Sun . Earth . Milky Way . Extra-galactic Future Summary The evidence for the existence Virial theorem of dark matter is very solid and, which is very important, at many different scales Rotation curves Comma Cluster Cosmic Microwave Background Bullet Cluster Gravitational Lensing + BNN, N-body simulations… We do not know what is dark matter, so it is hard to say which is the winning strategy: multi-front attack! PAMELA, AMS FERMI, MAGIC ANTARES, IceCube… Indirect detection XENON χ q, W+, Z… CDMS In any case: CoGENT -we want more than one DAMA “detection” +astrophysical ANAIS -results (constraints) of each … probes ( self- strategy are input for the others interaction of χ Directdetection q, W-, Z… DM affecting dark matter densities in Accelerators LHC galaxies…) Credit: Sky & Telescope / Gregg Dinderman X-ray astronomy (1-100 keV) differs from gamma ray astronomy in the detection strategy Atmosphere absorbs X-rays and fluxes are high, so observation is based on balloons and satellites X-rays cannot be focused by lenses, so focusing is based on total reflection (Wolter telescope) Projects: Chandra, XMM-Newton, Suzaku XMM-Newton: Large collecting area Simultaneous imaging and high resolution spectroscopy Monochromatic 3.5 keV photon line observed in data of XMM-Newton from 73 galaxy clusters Located within 50-100 eV of several known faint lines Interpreted as decay from sterile Bulbul, arxiv:1402.2301 neutrinos with ms=7.1 keV, which would be dark matter Boyarsky, arxiv:1402.4119 Also observed in Andromeda and Perseus Interpretation as sterile neutrino (sin2 (2θ)∼7x10-11) consistent with present constraints However, significant astrophysical unknowns involved (for instance, potassium XVIII line) Bulbul, arxiv:1402.2301 Boyarsky, arxiv:1402.4119 Astro-H Chandra Astro-H satellite (aka Hitomi), equipped with a X-ray spectrometer, was launched in Feb 2016. -
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) . -
Gustavo Marques-Tavares, Stanford Institute for Theoretical Physics
Detecting dark particles from Supernovae Gustavo Marques-Tavares, Stanford Institute for Theoretical Physics In collaboration with W. deRocco, P. Graham, D. Kasen and S. Rajendran Dark matter WIMP searches 5 -37 ACKNOWLEDGMENTS 10 -38 10 PandaX-II 2016 10-39 LUX 2016 ) 2 10-40 CDMSLite 2015 CRESST-II 2015 10-41 10-42 -43 10 SuperCDMS Post LHC1 mSUSY constraint 1700 kg-days 10-44 10-45 -46 10 6 t-y PandaX-4T 10-47 XENON1T 2 t-y LZ 15.6 t-y SI WIMP-nucleon cross section (cm XENONnT 20 t-y 10-48 200 t-y xenon (DARWIN or PandaX-30T) 10-49 Neutrino coherent scattering 10-50 1 10 102 103 WIMP mass (GeV/c2) *Figure taken from arxiv:1709.00688 This work is supported by grants from the Na- FIG. 4. The projected sensitivity (dashed curves) on the spin- tional Science Foundation of China (Nos. 11435008, independent WIMP-nucleon cross-sections of a selected num- ber of upcoming and planned direct detection experiments, 11455001, 11505112 and 11525522), a grant from the including XENON1T [34], PandaX-4T, XENONnT [34], Ministry of Science and Technology of China (Grant No. LZ [35], DARWIN [36] or PandaX-30T, and SuperCDMS [56]. 2016YFA0400301), and in part by the Chinese Academy Currently leading limits in Fig. 1 (see legend), the neutrino of Sciences Center for Excellence in Particle Physics ‘floor’ [20], and the post-LHC-Run1 minimal-SUSY allowed (CCEPP), the Key Laboratory for Particle Physics, As- contours [21] are overlaid in solid curves for comparison. The trophysics and Cosmology, Ministry of Education, and di↵erent crossings of the experimental sensitivities and the Shanghai Key Laboratory for Particle Physics and Cos- 2 neutrino floor at around a few GeV/c are primarily due to mology (SKLPPC). -
José Ángel Villar Rivacoba Was ANAIS Spokesperson and Chair Professor of Atomic, Molecular and Nuclear Physics at the Theo
24/10/2017 Direct Detection of Dark Matter and present status of ANAIS-112 experiment J. Amaré, I. Coarasa, S. Cebrián, C. Cuesta, E. García, M. Martínez, M.A. Oliván, Y. Ortigoza, A. Ortiz de Solórzano, J. Puimedón, A. Salinas, M.L. Sarsa, J.A. Villar✝, P. Villar In Memoriam In Memoriam • José Ángel Villar Rivacoba was ANAIS spokesperson and chair professor of Atomic, Molecular and Nuclear Physics at the Theoretical Physics Department of the University of Zaragoza • He passed away last August and we are deeply in sorrow 1 24/10/2017 In Memoriam In Memoriam • He was Bachelor and Doctor in Physics (Thesis supervised by Julio Morales) by the University of Zaragoza • He was always deeply involved in academic and research management activities in his University: • Dean of the Science Faculty at the University of Zaragoza (1992-2001) • Research Vice-Probost of the University of Zaragoza (2004-2008) • President of the Research Commission of the University of Zaragoza (2004-2008) • He was also strongly involved in scientific management at national and In Memoriam international level: • He was the coordinator of the national network of astroparticles (RENATA) • Member of the Executive Committee of the National Center for Physics of Astroparticles and Nuclear (CPAN) • Member of the general assembly and Joint Secretariat of the ApPEC Consortium • Organizer of numerous national and international congresses • Member of the Board and Science Assembly of ILIAS • Adviser to the successive Ministries responsible for Science and Technology, the Government -
Astrophysical Uncertainties of Direct Dark Matter Searches
Technische Universit¨atM¨unchen Astrophysical uncertainties of direct dark matter searches Dissertation by Andreas G¨unter Rappelt Physik Department, T30d & Collaborative Research Center SFB 1258 “Neutrinos and Dark Matter in Astro- and Particlephysics” Technische Universit¨atM¨unchen Physik Department T30d Astrophysical uncertainties of direct dark matter searches Andreas G¨unter Rappelt Vollst¨andigerAbdruck der von der Fakult¨atf¨urPhysik der Technischen Universit¨at M¨unchen zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften genehmigten Dissertation. Vorsitzender: Prof. Dr. Lothar Oberauer Pr¨uferder Dissertation: 1. Prof. Dr. Alejandro Ibarra 2. Prof. Dr. Bj¨ornGarbrecht Die Dissertation wurde am 12.11.2019 bei der Technischen Universit¨at M¨unchen eingereicht und durch die Fakult¨atf¨urPhysik am 24.01.2020 angenommen. Abstract Although the first hints towards dark matter were discovered almost 100 years ago, little is known today about its properties. Also, dark matter has so far only been inferred through astronomical and cosmological observations. In this work, we therefore investi- gate the influence of astrophysical assumptions on the interpretation of direct searches for dark matter. For this, we assume that dark matter is a weakly interacting massive particle. First, we discuss the development of a new analysis method for direct dark matter searches. Starting from the decomposition of the dark matter velocity distribu- tion into streams, we present a method that is completely independent of astrophysical assumptions. We extend this by using an effective theory for the interaction of dark matter with nucleons. This allows to analyze experiments with minimal assumptions on the particle physics of dark matter. Finally, we improve our method so that arbitrarily strong deviations from a reference velocity distribution can be considered. -
In-Situ Gamma-Ray Background Measurements for Next Generation CDEX Experiment in the China Jinping Underground Laboratory a a a a ∗ a a A,B a H
In-situ gamma-ray background measurements for next generation CDEX experiment in the China Jinping Underground Laboratory a a a a < a a a,b a H. Ma , Z. She , W. H. Zeng , Z. Zeng , , M. K. Jing , Q. Yue , J. P. Cheng , J. L. Li and a H. Zhang aKey Laboratory of Particle and Radiation Imaging (Ministry of Education) and Department of Engineering Physics, Tsinghua University, Beijing 100084 bCollege of Nuclear Science and Technology, Beijing Normal University, Beijing 100875 ARTICLEINFO ABSTRACT Keywords: In-situ -ray measurements were performed using a portable high purity germanium spectrometer in In-situ -ray measurements Hall-C at the second phase of the China Jinping Underground Laboratory (CJPL-II) to characterise Environmental radioactivity the environmental radioactivity background below 3 MeV and provide ambient -ray background Underground laboratory parameters for next generation of China Dark Matter Experiment (CDEX). The integral count rate Rare event physics of the spectrum was 46.8 cps in the energy range of 60 to 2700 keV. Detection efficiencies of the CJPL spectrometer corresponding to concrete walls and surrounding air were obtained from numerical calculation and Monte Carlo simulation, respectively. The radioactivity concentrations of the walls 238 232 in the Hall-C were calculated to be 6:8 , 1:5 Bq/kg for U, 5:4 , 0:6 Bq/kg for Th, 81:9 , 14:3 40 Bq/kg for K. Based on the measurement results, the expected background rates from these primordial radionuclides of future CDEX experiment were simulated in unit of counts per keV per ton per year (cpkty) for the energy ranges of 2 to 4 keV and around 2 MeV. -
Session: Neutrino Astronomy
Session: Neutrino Astronomy Chair: Takaaki Kajita, Institute for Cosmic Ray Research, Univ. of Tokyo Basic natures of neutrinos Neutrino was introduced in 1930 by W. Pauli in order to save the energy conservation law in nuclear beta decay processes, in which the emitted electron exhibits a continuous energy spectrum. It was assumed that the penetration power of neutrinos is much higher than that of the gamma rays. More than 20 years later, the existence of neutrinos was experimentally confirmed by an experiment that measured neutrinos produced by a nuclear power reactor. Since then, the basic nature of neutrinos has been understood through various theoretical and experimental studies: Neutrinos interact with matter extremely weakly. The number of neutrino species is three. They are called electron-neutrino, muon-neutrino and tau-neutrino. In addition, recent neutrino experiments discovered that neutrinos have very small masses. Observing the Universe by neutrinos (1) Because of the extremely high penetration power of neutrinos, neutrinos produced at the center of a star easily penetrate to the outer space. Theories of astrophysics predict that there are various processes that neutrinos play an essential role at the center of stars. For example, the Sun is generating its energy by nuclear fusion processes in the central region. In these processes, low energy electron neutrinos with various energy spectra are generated. Thus the observation of solar neutrinos directly probes the nuclear fusion reactions in the Sun. Another example is the supernova explosion. While the optical measurements observe an exploding star, what is happening in the central region of the star is the collapse of the core of a massive star. -
Carsten Rott Curriculum Vitae Feb 2018
Carsten Rott Curriculum Vitae Feb 2018 Department of Physics, Sungkyunkwan University, Suwon 16419, Korea Tel: +82-31-290-5902 E-mail:[email protected] Experimental astro-particle physics, particle physics, geophysics, neutri- Research nos physics Focus Languages German, English; Elementary: French, Japanese, and Korean Employment 2017 { 2018 Honorary Fellow at Wisconsin IceCube Particle Astrophysics Center (WIPAC) (Sabbatical), University of Wisconsin Madison, USA 2017 { now Associate Professor, Sungkyunkwan University, Korea 2013 { 2017 Assistant Professor, Sungkyunkwan University, Korea 2016 Visiting Researcher (3-month), University of Tokyo, Japan 2009 { 2013 Senior Fellow of the Center for Cosmology and AstroParticle Physics (CCAPP) (5-year term), The Ohio State University, USA 2008 { 2009 CCAPP Fellow (3-year term), The Ohio State University, USA 2005 { 2008 Postdoctoral Fellow, Pennsylvania State University, USA Education 1998 { 2004 Purdue University, Indiana, USA Ph.D in Experimental Particle Physics (December 2004) Title : \Search for Scalar Bottom Quarks from Gluino Decays" at CDF Thesis Adviser : Prof. Daniela Bortoletto 1995 { 1998 Universit¨atHannover, Hannover, Germany Honors and Awards 2011 Recipient of NSF Antarctica Service Medal 2005 \Fermilab's Result of the Week" (FermiNews, August 11, 2005) 2004 George W. Tautfest Award, Purdue University 1998 { 1999 University of Hannover { Purdue University direct exchange fellowship Funds and Grants 2017 { present NRF Midscale Research Fund (PI), Korea { NRF-2017R1A2B2003666 2017 { present Foreign Facility Fund (PI of 7 sub-PIs) { NRF-2017K1A3A7A09015973 2016 { present NRF SRC Korea Neutrino Research Center (KNRC) (Co-I), Korea 2016 { 2017 NRF Individual Researcher (PI), Korea { NRF-2016R1D1A1B03931688 2013 { present BrainKorea (BK21plus) participant, Korea 2013 { 2016 NRF Individual Researcher (PI), Korea { NRF-2013R1A1A1007068 2013 { 2014 SKKU Intramural Faculty Fund Award, Korea 2013 { 2014 Fermi GI Cycle 6 (Co-I with Prof. -
Strengthening Global Coordination on Large Neutrino Infrastructures”
July 8, 2016 Press Release concerning the 3rd International Neutrino Meeting on Large Neutrino Infrastructures hosted by KEK on the 30-31st of May 2016 “Strengthening global coordination on large neutrino infrastructures” Funding-agency1 and laboratory representatives2 gathered at the 3rd International Meeting on Large Neutrino Infrastructures3 on May 30-31, 2016 at KEK in Tsukuba, Japan to gauge the progress in the global coordination of projects that had been launched during the first and second international meetings4 and to discuss the next steps in the global coordination. The meeting was opened by the 2015 Nobel Prize winner Takaaki Kajita who commented that “Very large-scale experiments will be needed to fully explore neutrino properties. These large-scale experiments will also naturally have astrophysics potential and increase the sensitivity of searches for proton disintegration.” He went on to note that to realise the necessary very large-scale facilities would require “… international coordination and collaboration” and defined the goals of the meeting to be to “… discuss the physics cases and global strategy, including astrophysics and proton decays, which are the part of the aim of this series of meetings; have follow-up discussions of the ICFA Neutrino Panel’s5 roadmap discussion document”6 and to discuss “… the various neutrino experiments, including Hyper- Kamiokande7, toward the realization of an efficient and productive global neutrino program.” In this meeting, the funding-agency and laboratory representatives welcomed the important steps that had been made towards the realisation of the Hyper-Kamiokande (Hyper-K) experiment7. The international proto-collaboration has developed new, high- sensitivity, large-aperture photomultiplier tubes that substantially reduce the total project cost without unduly compromising its potential to address important questions in particle and astroparticle physics and in nucleon decay. -
Possibilities for Underground Physics in the Pyh\" Asalmi Mine
CIPANP2018-Trzaska-374 October 3, 2018 Possibilities for Underground Physics in the Pyhasalmi mine W.H. Trzaska1, L. Bezrukov2, T. Enqvist1, J. Joutsenvaara3, P. Kuusiniemi1, K. Loo1, B. Lubsandorzhiev2, V. Sinev2, M. Slupecki1 1Department of Physics, University of Jyvaskyla, Finland 2Institute for Nuclear Research, Russian Academy of Sciences, Moscow, Russia 3Kerttu Saalasti Institute, University of Oulu, Finland The Pyhasalmi mine is uniquely suited to host new generation of large- scale underground experiments. It was chosen both by the LAGUNA- LBNO and by the LENA Collaboration as the preferred site for a giant neutrino observatory. Regrettably, none of these projects got funded. The termination of the underground excavations in the fall of 2019 marks an important milestone. To maintain the infrastructure in good condi- tion a new sponsor must be found: either a large-scale scientific project or a new commercial operation. The considered alternatives for the commer- cial use of the mine include a pumped-storage hydroelectricity plant and a high-security underground data-storage centre. Without a new sponsor the ongoing experiments, including the cosmic-ray experiment EMMA and the study of C14 content in liquid scintillators, have to be completed within the next few years. PRESENTED AT arXiv:1810.00909v1 [physics.ins-det] 1 Oct 2018 Thirteenth Conference on the Intersections of Particle and Nuclear Physics (CIPANP2018) Palm Springs, CA, USA, May 28 - June 3, 2018 1 Introduction Earth's atmosphere is exposed to a steady flux of energetic particles known as cosmic rays [1]. Cosmic-ray interactions with nuclei in the atmosphere induce intense show- ers of secondary particles.