Pandax-III: Searching for Neutrinoless Double Beta Decay with High Pressure 136Xe Gas Time Projection Chambers
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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. -
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). -
Neutrinoless Double Beta Decay Searches
FLASY2019: 8th Workshop on Flavor Symmetries and Consequences in 2016 Symmetry Magazine Accelerators and Cosmology Neutrinoless Double Beta Decay Ke Han (韩柯) Shanghai Jiao Tong University Searches: Status and Prospects 07/18, 2019 Outline .General considerations for NLDBD experiments .Current status and plans for NLDBD searches worldwide .Opportunities at CJPL-II NLDBD proposals in China PandaX series experiments for NLDBD of 136Xe 07/22/19 KE HAN (SJTU), FLASY2019 2 Majorana neutrino and NLDBD From Physics World 1935, Goeppert-Mayer 1937, Majorana 1939, Furry Two-Neutrino double beta decay Majorana Neutrino Neutrinoless double beta decay NLDBD 1930, Pauli 1933, Fermi + 2 + (2 ) Idea of neutrino Beta decay theory 136 136 − 07/22/19 54 → KE56 HAN (SJTU), FLASY2019 3 ̅ NLDBD probes the nature of neutrinos . Majorana or Dirac . Lepton number violation . Measures effective Majorana mass: relate 0νββ to the neutrino oscillation physics Normal Inverted Phase space factor Current Experiments Nuclear matrix element Effective Majorana neutrino mass: 07/22/19 KE HAN (SJTU), FLASY2019 4 Detection of double beta decay . Examples: . Measure energies of emitted electrons + 2 + (2 ) . Electron tracks are a huge plus 136 136 − 54 → 56 + 2 + (2)̅ . Daughter nuclei identification 130 130 − 52 → 54 ̅ 2νββ 0νββ T-REX: arXiv:1512.07926 Sum of two electrons energy Simulated track of 0νββ in high pressure Xe 07/22/19 KE HAN (SJTU), FLASY2019 5 Impressive experimental progress . ~100 kg of isotopes . ~100-person collaborations . Deep underground . Shielding + clean detector 1E+27 1E+25 1E+23 1E+21 life limit (year) life - 1E+19 half 1E+17 Sn Ca νββ Ge Te 0 1E+15 Xe 1E+13 1940 1950 1960 1970 1980 1990 2000 2010 2020 Year . -
Diurnal Effect of Sub-Gev Dark Matter Boosted by Cosmic Rays
Diurnal Effect of Sub-GeV Dark Matter Boosted by Cosmic Rays Shao-Feng Ge,1,2, ∗ Jianglai Liu,2,1, † Qiang Yuan,3, 4, 5, ‡ and Ning Zhou2, § 1Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai 200240, China 2School of Physics and Astronomy, Shanghai Jiao Tong University, Key Laboratory for Particle Astrophysics and Cosmology (MOE) & Shanghai Key Laboratory for Particle Physics and Cosmology, Shanghai 200240, China 3Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210033, China 4School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China 5Center for High Energy Physics, Peking University, Beijing 100871, China We point out a new type of diurnal effect for the cosmic ray boosted dark matter (DM). The DM- nucleon interactions not only allow the direct detection of DM with nuclear recoils, but also allow cosmic rays to scatter with and boost the nonrelativistic DM to higher energies. If the DM-nuclei scattering cross sections are sufficiently large, the DM flux is attenuated as it propagates through the Earth, leading to a strong diurnal modulation. This diurnal modulation provides another prominent signature for the direct detection of boosted sub-GeV DM, in addition to signals with higher recoil energy. Introduction – Overwhelming evidence from astrophys- signals in large neutrino experiments [44–46]. ical and cosmological observations supports the existence For sub-GeV DM, the DM-nucleon scattering cross sec- of dark matter (DM) [1], which is gravitationally interact- tion with a contact interaction can be quite sizable, e.g., ing but invisible via electromagnetic interactions. -
27. Dark Matter
1 27. Dark Matter 27. Dark Matter Written August 2019 by L. Baudis (Zurich U.) and S. Profumo (UC Santa Cruz). 27.1 The case for dark matter Modern cosmological models invariably include an electromagnetically close-to-neutral, non- baryonic matter species with negligible velocity from the standpoint of structure formation, gener- ically referred to as “cold dark matter” (CDM; see The Big-Bang Cosmology—Sec. 22 of this Re- view). For the benchmark ΛCDM cosmology adopted in the Cosmological Parameters—Sec. 25.1 of this Review, the DM accounts for 26.4% of the critical density in the universe, or 84.4% of the total matter density. The nature of only a small fraction, between at least 0.5% (given neutrino os- cillations) and at most 1.6% (from combined cosmological constraints), of the non-baryonic matter content of the universe is known: the three Standard Model neutrinos (see the Neutrino Masses, Mixing, and Oscillations—Sec. 14 of this Review) ). The fundamental makeup of the large majority of the DM is, as of yet, unknown. Assuming the validity of General Relativity, DM is observed to be ubiquitous in gravitation- ally collapsed structures of size ranging from the smallest known galaxies [1] to galaxies of size comparable to the Milky Way [2], to groups and clusters of galaxies [3]. The mass-to-light ratio is observed to saturate at the largest collapsed scales to a value indicative, and close to, what inferred from other cosmological observations for the universe as a whole [4]. In such collapsed structures, the existence of DM is inferred directly using tracers of mass enclosed within a certain radius such as stellar velocity dispersion, rotation curves in axisymmetric systems, the virial theorem, gravitational lensing, and measures of the amount of non-dark, i.e. -
Neutrino Oscillations: the Rise of the PMNS Paradigm Arxiv:1710.00715
Neutrino oscillations: the rise of the PMNS paradigm C. Giganti1, S. Lavignac2, M. Zito3 1 LPNHE, CNRS/IN2P3, UPMC, Universit´eParis Diderot, Paris 75252, France 2Institut de Physique Th´eorique,Universit´eParis Saclay, CNRS, CEA, Gif-sur-Yvette, France∗ 3IRFU/SPP, CEA, Universit´eParis-Saclay, F-91191 Gif-sur-Yvette, France November 17, 2017 Abstract Since the discovery of neutrino oscillations, the experimental progress in the last two decades has been very fast, with the precision measurements of the neutrino squared-mass differences and of the mixing angles, including the last unknown mixing angle θ13. Today a very large set of oscillation results obtained with a variety of experimental config- urations and techniques can be interpreted in the framework of three active massive neutrinos, whose mass and flavour eigenstates are related by a 3 3 unitary mixing matrix, the Pontecorvo- × Maki-Nakagawa-Sakata (PMNS) matrix, parameterized by three mixing angles θ12, θ23, θ13 and a CP-violating phase δCP. The additional parameters governing neutrino oscillations are the squared- mass differences ∆m2 = m2 m2, where m is the mass of the ith neutrino mass eigenstate. This ji j − i i review covers the rise of the PMNS three-neutrino mixing paradigm and the current status of the experimental determination of its parameters. The next years will continue to see a rich program of experimental endeavour coming to fruition and addressing the three missing pieces of the puzzle, namely the determination of the octant and precise value of the mixing angle θ23, the unveiling of the neutrino mass ordering (whether m1 < m2 < m3 or m3 < m1 < m2) and the measurement of the CP-violating phase δCP. -
35. Particle Detectors for Non-Accelerator Physics
1 35. Particle Detectors for Non-Accelerator Physics 35. Particle Detectors for Non-Accelerator Physics 35.1 Introduction . 1 35.2 High-energy cosmic-ray hadron and gamma-ray detectors . 2 35.2.1 Atmospheric fluorescence detectors . 2 35.2.2 Atmospheric Cherenkov telescopes for high-energy gamma ray astronomy . 5 35.3 Large neutrino detectors . 8 35.3.1 Deep liquid detectors for rare processes . 8 35.3.2 Neutrino telescopes . 12 35.3.3 Radio emission from (ultra-)high energy particle showers . 20 35.4 Large time-projection chambers for rare event detection . 27 35.4.1 Dark matter and other low energy signals . 28 35.4.2 0νββ Decay . 31 35.5 Sub-Kelvin detectors . 32 35.5.1 Equilibrium thermal detectors . 32 35.5.2 Nonequilibrium Detectors . 34 35.6 Low-radioactivity background techniques . 36 35.6.1 Defining the problem . 37 35.6.2 Environmental radioactivity . 37 35.6.3 Radioactive impurities in detector and shielding components . 39 35.6.4 Radon and its progeny . 40 35.6.5 Cosmic rays . 41 35.6.6 Neutrons . 42 35.1 Introduction Non-accelerator experiments have become increasingly important in particle physics. These include cosmic ray experiments (with surface, space and underground detectors), neutrino oscilla- tion measurements with solar and atmospheric neutrinos in underground laboratories, searches for neutrino-less double beta decays and dark matter candidates again in underground laboratories, and searches for more exotic phenomena. The detectors are in the majority of the cases differ- ent from those used at accelerators. Even when the detectors are based on the same physics (e. -
An Improved Design of the Readout Base Board of the Photomultiplier Tube for Future Pandax Dark Matter Experiments
Prepared for submission to JINST An improved design of the readout base board of the photomultiplier tube for future PandaX dark matter experiments Qibin Zheng,0,2 Yanlin Huang,0 Di Huang,1 Jianglai Liu,1,3 Xiangxiang Ren,4 Anqing Wang,4 Meng Wang,4 Jijun Yang,1 Binbin Yan,1 Yong Yang1 0Institute of Biomedical Engineering, University of Shanghai for Science and Technology, Shanghai 200093, China 1INPAC, Department of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai Laboratory for Particle Physics and Cosmology, Shanghai 200240, China 2Terahertz Technology Innovation Research Institute, University of Shanghai for Science and Technology, Shanghai 200093, China 3Tsung-Dao Lee Institute, Shanghai Jiaotong University, Shanghai, 200240, China 4School of Physics and Key Laboratory of Particle Physics and ParticleIrradiation (MOE), Shandong University, Jinan 250100, China E-mail: [email protected] Abstract: The PandaX project consists of a series of xenon-based experiments that are used to search for dark matter (DM) particles and to study the fundamental properties of neutrinos. The next DM experiment PandaX-4T will be using 4 ton liquid xenon in the sensitive volume, which is nearly a factor of seven larger than that of the previous experiment PandaX-II. Due to the increasing target mass, the sensitivity of searching for both DM and neutrinoless double-beta decay (0aVV) signals in the same detector will be significantly improved. However, the typical energy of interest for 0aVV signals is at the MeV scale, which is much higher than that of most popular DM signals. In the baseline readout scheme of the photomultiplier tubes (PMTs), the dynamic range is very limited. -
The Majorana Zero-Neutrino Double-Beta Decay Experiment
White Paper on The Majorana Zero-Neutrino Double-Beta Decay Experiment The Majorana Collaboration: Brown University, Providence, RI Institute for Theoretical and Experimental Physics, Moscow, Russia Joint Institute for Nuclear Research, Dubna, Russia Lawrence Berkeley National Laboratory, Berkeley, CA Lawrence Livermore National Laboratory, Livermore, CA Los Alamos National Laboratory, Los Alamos, NM New Mexico State University, Carlsbad, NM Oak Ridge National Laboratory, Oak Ridge, TN Osaka University, Osaka, Japan Pacific Northwest National Laboratory, Richland, WA Queen’s University, Kingston, Canada Triangle Universities Nuclear Laboratory, Durham, NC University of Chicago, Chicago, IL University of South Carolina, Columbia, SC University of Tennessee, Knoxville, TN University of Washington, Seattle, WA November 3, 2003 Approved for public release: LA-UR-2003-7709 and PNNL-14420 The Majorana Zero Neutrino Double-Beta Decay Experiment Abstract The objective of the Majorana Experiment is to study neutrinoless double beta decay (0νββ) with an effective Majorana-neutrino mass sensitivity below 50 meV in order to characterize the Majorana nature of the neutrino, the Majorana mass spectrum, and the absolute mass scale. An experimental study of the neutrino mass scale implied by neutrino oscillation results is now technically within our grasp. This exciting physics goal is best pursued using the well-established technique of searching for 0νββ of 76Ge, augmented with recent advances in signal processing and detector design. The Majorana Experiment will consist of a large mass of 76Ge in the form of high-resolution intrinsic germanium detectors located deep underground within a low-background shielding environment. Observation of a sharp peak at the ββ endpoint will quantify the 0νββ half-life and thus the effective Majorana mass of the electron neutrino. -
Search for Neutrinos from Decaying Dark Matter with Icecube
Search for neutrinos from decaying dark matter with IceCube The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Aartsen, M. G. et al. "Search for neutrinos from decaying dark matter with IceCube." European Physical Journal C: Particles and Fields 78 (October 2018): 831 © 2018 The Author(s) As Published https://doi.org/10.1140/epjc/s10052-018-6273-3 Publisher Springer Berlin Heidelberg Version Final published version Citable link http://hdl.handle.net/1721.1/118985 Terms of Use Creative Commons Attribution Detailed Terms http://creativecommons.org/licenses/by/4.0/ Eur. Phys. J. C (2018) 78:831 https://doi.org/10.1140/epjc/s10052-018-6273-3 Regular Article - Experimental Physics Search for neutrinos from decaying dark matter with IceCube IceCube Collaborationa , M. G. Aartsen16, M. Ackermann51, J. Adams16,J.A.Aguilar12, M. Ahlers20, M. Ahrens43, I. Al Samarai25, D. Altmann24, K. Andeen33, T. Anderson48, I. Ansseau12, G. Anton24, C. Argüelles14, J. Auffenberg1, S. Axani14, P. Backes1, H. Bagherpour16,X.Bai40, J. P. Barron23, S. W. Barwick27, V. Baum32, R. Bay8, J. J. Beatty18,19, J. Becker Tjus11, K.-H. Becker50, S. BenZvi42, D. Berley17, E. Bernardini51, D. Z. Besson28, G. Binder8,9, D. Bindig50, E. Blaufuss17,S.Blot51, C. Bohm43, M. Börner21,F.Bos11, S. Böser32, O. Botner49, E. Bourbeau20, J. Bourbeau31, F. Bradascio51, J. Braun31, M. Brenzke1,H.-P.Bretz51,S.Bron25, J. Brostean-Kaiser51, A. Burgman49,R.S.Busse31, T. Carver25, E. Cheung17, D. Chirkin31, A. Christov25, K. Clark29, L. Classen35, G. H. Collin14, J. -
Search for Neutrinoless Double-Beta Decay with CUORE Yury G
Search for Neutrinoless Double-Beta Decay with CUORE Yury G. Kolomensky, for the CUORE Collaboration LBNL and UC Berkeley The observation of 0!"" decays (DBD) would unambiguously establish the violation of lepton number conservation, and indicate that neutrinos are Majorana particles, i.e. they are their own anti-particles. The rate of the process is sensitive to the effective Majorana neutrino mass. Determining whether neutrinos are Majorana or Dirac particles and measuring their masses are among the highest priorities in neutrino physics, as was pointed out in the 2004 APS Multi-Divisional Neutrino Study and well as the 2007 NSAC Long Range Plan. The answer will also have important implications for astrophysics and cosmology. Addressing this question has become an even higher priority since the recent apparent discovery of the long-sought Higgs boson. A Majorana neutrino mass is not generated by the Higgs mechanism and Majorana particles are not accommodated in the Standard Model. Thus, discovery of the Majorana nature of neutrinos would provide a clear indication of new physics beyond the Standard Model. CUORE, the Cryogenic Underground Observatory for Rare Events, promises to be one of the most sensitive 0!"" experiments this decade. It will be sensitive to the neutrino mass values suggested by recent atmospheric neutrino oscillation experiments in the so-called inverted mass hierarchy. CUORE is an established project within the DOE and NSF. The detector is currently under construction at the Laboratori Nazionali del Gran Sasso (LNGS) in Assergi, Italy, and is expected to start operations in 2014. CUORE is a cryogenic-bolometer detector consisting of 988 TeO2 crystals, 750 g each, operated at a temperature of 10mK.