DOCSLIB.ORG

Direct Detection of Cold Dark Matter

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Direct Detection of Cold Dark Matter Direct Detection of Cold Dark Matter Laura Baudis a Physik Institut, University of Zurich, Winterthurerstr. 190, CH-8057 Zurich Abstract. We know from cosmological and astrophysical observations that more than 80% of the matter density in the Universe is non-luminous, or dark. This non-baryonic dark matter could be composed of neutral, heavy particles, which were non-relativistic, or ’cold’, when they decoupled from ordinary matter. I will review the direct detection methods of these hypothetical particles via their interactions with nuclei in ultra-low background, deep underground experiments. The emphasis is on most recent results and on the status of near future projects. PACS. 95.35.+d dark matter – 95.55.Vj, 29.40.Mc detectors 1 Introduction in the galactic halo, v and f(v) are the WIMP velocity and velocity distribution function in the Earth frame In the Standard Model of cosmology the Universe is and dσ/dER is the WIMP-nucleus differential cross flat and made of 4% baryons, 20% non-baryonic dark 2 2 section. The nuclear recoil energy is ER = mr v (1 − matter and 76% dark energy [1]. Generic candidates cos θ)/mN , where θ is the scattering angle in the WIMP- for non-baryonic dark matter, which thus makes more nucleus center-of-mass frame, mN is the nuclear mass than 80% of the total matter density in the Universe, and mr is the WIMP-nucleus reduced mass.1 The ve- are axions [2] and weakly interacting massive particles 2 2 locity vmin is defined as vmin = (mN Eth/2mr ) , where (WIMPs) [3]. WIMPs could have been thermally pro- Eth is the energy threshold of the detector, and vmax duced in the very early universe. If their mass and cross is the escape WIMP velocity in the Earth frame. The section is determined by the weak scale, the freeze-out simplest galactic model assumes a Maxwell-Boltzmann relic density is around the observed value, Ω ∼0.1 [4]. distribution for the WIMP velocity in the galactic rest −1 The best studied WIMP candidates are the neutralino, frame, with a velocity dispersion of vrms ≈ 270kms −1 or the lightest supersymmetric particle, and the light- and an escape velocity of vesc ≈ 650kms . (1) est Kaluza-Klein particle, for instance the B , which The differential WIMP-nucleus cross section has is the first excitation of the hypercharge gauge boson two separate components: an effective scalar coupling in theories with universal extra dimensions. A recent between the WIMP and the nucleus and an effective comprehensive review of particle dark matter candi- coupling between the spin of the WIMP and the total dates has been provided by Bertone, Hooper and Silk arXiv:0711.3788v1 [astro-ph] 25 Nov 2007 spin of the nucleus. In general the coherent part dom- [5]. A recent review on axions as cold dark matter can- inates the interaction (depending however on the con- didates can be found in [6]. In this review I will focus tent of the neutralino) for target masses with A≥30 [3]. on the direct detection of WIMPs, with emphasis on The cross section can be expressed as the sum of both most recent experimental results and on the status of dσ ∝ 0 2 0 2 contributions dER σSI FSI (ER)+σSDFSD(ER), where projects which are now under construction. 0 σSI,SD are the WIMP-nucleus cross sections in the 2 limit of zero momentum transfer and FSI,SD(ER) de- 2 Direct Detection of WIMPs note the nuclear form factors, expressed as a function of the recoil energy. WIMPs can be detected directly, via their elastic colli- The left side of equation 1 is the measured spec- sions with nuclei in terrestrial targets [7]. The differen- trum in a detector, while the right side represents tial rate for WIMP elastic scattering off nuclei is given the theoretical prediction. It includes WIMP proper- by [8] ties which are completely unknown, such as the mass mW and elastic cross section σ0, quantities in princi- vmax ple accessible from astrophysics, such as the density of dR ρ0 dσ = NT dv f(v) v (1) WIMPs in the halo ρ0, the WIMP velocity distribu- dER mW Zvmin dER tion f(v) and the escape velocity (which are however still prone to large uncertainties) and detector specific where NT represents the number of the target nuclei, m is the WIMP mass and ρ the local WIMP density parameters: mass of target nucleus, energy threshold W 0 and nuclear form factors. The nuclear form factors be- a Email: [email protected] come significant at large WIMP and nucleus masses, Laura Baudis Review and lead to a suppression of the differential scattering surrounding the detector. An additional advantage is rate. Figure 1 shows differential spectra for Si, Ar, Ge provided by a highly granular detector (or good timing and Xe, calculated for a WIMP mass of 100GeV, a and position resolution), since multiple scatters within scalar WIMP-nucleon cross section of σ = 10−43 cm2, the detector volume allow both background reduction 3 using standard halo parameters ( ρ0 = 0.3 GeV/cm , and a direct measurement of the neutron background −1 v0 = 220 km s ). for experiments with an event-by-event discrimination against electron recoils. Finally, the position resolu- tion leads to the identification of events clustered at −2 10 the detector surfaces, which are quite unlikely to be m = 100 GeV Si WIMP WIMPs. Ar σ = 1e−43 cm−2 In order to convincingly detect a WIMP signal, a Ge WIMP−n Xe specific signature from a particle populating our galac- tic halo is important. The Earth’s motion through the galaxy induces both a seasonal variation of the total event rate [9,10] and a forward-backward asymmetry in a directional signal [11,12]. The annual modulation −3 10 of the WIMP signal arises because of the Earth’s mo- tion in the galactic frame, which is a superposition of the Earth’s rotation around the Sun and the Sun’s ro- tation around the galactic center: Counts [/kg/keV/day] vE = v⊙ + vorb cos γ cos ω(t − t0), (2) −1 −1 where v⊙ = v0 + 12 km s (v0 ≈ 220 km s ), −4 −1 10 vorb ≈ 30 km s denotes the Earth’s orbital speed around the Sun, the angle γ ≈ 600 is the inclination of the Earth’s orbital plane with respect to the galactic nd plane and ω =2π/1yr, t0 = June 2 . The expected time dependence of the count rate 0 10 20 30 40 50 60 70 80 Recoil Energy [keV] can be approximated by a cosine function with a pe- nd riod of T = 1year and a phase of t0 = June 2 : Fig. 1. Differential WIMP recoil spectrum for a WIMP mass of 100 GeV and a WIMP-nucleon cross section σ = −43 2 S(t)= S0 + Smcosω(t − t0), (3) 10 cm . The spectrum was calculated for illustrative nuclei such as Si (light solid), Ar (light dot-dashed), Ge where S0, Sm are the constant and the modulated (dark solid), Xe (dark dashed). amplitude of the signal, respectively. In reality, an ad- ditional contribution to S(t) from the background must be considered. The background should be constant A WIMP with a typical mass between a few GeV in time or at least not show the same time depen- and 1 TeV will deposit a recoil energy below 50 keV dency as the predicted WIMP signal. The expected in a terrestrial detector. The predicted event rates for seasonal modulation effect is very small (of the order −6 neutralinos range from 10 to 10 events per kilogram of vorb/v0 ≃ 0.07), requiring large masses and long detector material and day [3]. Evidently, in order to counting times as well as an excellent long-term sta- observe a WIMP spectrum, low energy threshold, low bility of the experiment. background and high mass detectors are essential. In A much stronger signature would be given by the such a detector, the recoil energy of the scattered nu- ability to detect the axis and direction of the recoil cleus is transformed into a measurable signal, such nucleus. It has been shown [11], that the WIMP in- as charge, light or phonons, and at least one of the teraction rate as a function of recoil energy and angle above quantities is detected. Observing two signals si- θ between the WIMP velocity and recoil direction (in multaneously yields a powerful discrimination against the galactic frame) is: background events, which are mostly interactions with electrons, as opposed to WIMPs and neutrons scatter- 2 2 d R (v⊙cosθ − v ) ing off nuclei. Even for experiments with good event ∝ − min exp 2 , (4) by event discrimination, an absolute low background dERdcosθ v0 is still important, given the small size and rate of the 2 2 2 2 expected WIMP signal. It can be achieved in both pas- where vmin = (mN + mW ) ER/2mN mW and v0 2 sive and active ways. Passive methods range from high =3v⊙/2. The forward-backward asymmetry yields a material selection of detector components to various large effect of the order of O(v⊙/v0)≈ 1. Thus fewer specific shields against the natural radioactivity of the events are needed to discover a WIMP signal than in environment and against cosmic rays and secondary the case where the seasonal modulation effect is ex- particles produced in their interactions. Active back- ploited [12]. The challenge is to build massive detec- ground reduction implies an active shield, commonly a tors capable of detecting the direction of the incoming plastic or liquid scintillator, or a water Cerenkov shield WIMP.
Load more

Recommended publications
  • Dark Matter Sensitivity of Multi-Ton Liquid Xenon Detectors
    Prepared for submission to JCAP Dark matter sensitivity of multi-ton liquid xenon detectors Marc Schumann,a;1 Laura Baudis,b Lukas Bütikofer,a Alexander Kish,b Marco Selvic aAlbert Einstein Center for Fundamental Physics, Universität Bern, Switzerland bPhysik-Institut, Universität Zürich, Switzerland cINFN Bologna, Italy E-mail: [email protected], [email protected], [email protected], [email protected], [email protected] Abstract. We study the sensitivity of multi ton-scale time projection chambers using a liquid xenon target, e.g., the proposed DARWIN instrument, to spin-independent and spin- dependent WIMP-nucleon scattering interactions. Taking into account realistic backgrounds from the detector itself as well as from neutrinos, we examine the impact of exposure, energy threshold, background rejection efficiency and energy resolution on the dark matter sensitivity. With an exposure of 200 t × y and assuming detector parameters which have been already demonstrated experimentally, spin-independent cross sections as low as 2:5×10−49 cm2 can be probed for WIMP masses around 40 GeV/c2. Additional improvements in terms of background rejection and exposure will further increase the sensitivity, while the ultimate WIMP science reach will be limited by neutrinos scattering coherently off the xenon nuclei. arXiv:1506.08309v2 [physics.ins-det] 3 Sep 2015 1Corresponding author. Contents 1 Introduction1 2 Light and Charge Signal Generation2 3 Energy Scale and Energy Resolution3 4 Evaluation of the spin-independent WIMP-nucleon Sensitivity4 5 Backgrounds6 6 Electronic Recoil Rejection 10 7 WIMP Sensitivity 12 8 Summary and Discussion 15 1 Introduction The nature of dark matter, contributing about 27% to the matter and energy content of our Universe [1], is one of the outstanding open questions in physics.
    [Show full text]
  • The Great Debate Page 6 in This Issue: CLAS Welcomes New Faculty
    November 2004 Volume 18 notes CLASThe University of Florida College of Liberal Arts and Sciences The Great Debate page 6 In this Issue: CLAS Welcomes New Faculty ........... 3 The Great Debate ............................. 6 Around the College ......................... 8 Grants .............................................. 10 Bookbeat ........................................ 11 The Dean’s Junk Mail Be Gone! ....................... 12 Musings The Fundamentals As important as our cross-disciplinary interactions are, E-mail [email protected] with your news and especially in the applied sciences and social sciences, events information for publication in CLAS- we need to remind ourselves of the critical importance notes. The deadline for submissions is the 15th of the month prior to the month you would of the fundamental academic disciplines—the essential like your information published. Don’t wait! units of mathematics, English, philosophy, history, the Send us your news and events today! languages, natural sciences, behavioral sciences and social studies. It is these core units that engage in the basic research that historically has led to some of the most far-reaching discoveries and the formation of new interdisciplinary programs. Inventions which have led to revolutionary technologies and analyses that College of Liberal Arts and Sciences News and Publications have changed our understanding of societies and their 2008 Turlington Hall behaviors have often had their as their origin the PO Box 117300 Gainesville FL 32611-7300 research of a challenging academic problem. [email protected] Our college has the responsibility of advancing http://clasnews.clas.ufl.edu these basic areas of inquiry by energizing fundamental CLASnotes is published by the College of Liberal research with support for promising interdisciplinary Arts and Sciences to inform faculty, staff and stu- programs.
    [Show full text]
  • Dark Matter Lecture 1: Evidence and Candidates
    Dark Matter Lecture 1: Evidence and candidates March 27, 2012 Dark matter lectures University of Sao Paulo Laura Baudis, Universität Zürich 1 Content: first lecture • Overview: cosmological parameters in the standard model of cosmology • Dark matter in galaxies and in the Milky Way structure of the Milky Way galactic rotation curve and what can we learn from it dark matter distribution simulations of the Milky Way’s dark halo - spatial distribution of dark matter - velocity distribution of dark matter - the dark matter disk • Candidates for dark matter, overview neutrinos WIMPs and freeze-out candidates from supersymmetry - allowed parameter space in a constrained SUSY model 2 Content: second lecture • Direct detection of WIMPs: principles expected rates in a terrestrial detector kinematics of elastic WIMP-nucleus scattering differential rates corrections I: movement of the Earth corrections II: form factors cross sections for scattering on nucleons - spin independent - spin dependent • Expected WIMP signal and backgrounds time and directional signal dependance quenching factors and background discrimination background sources in direct detection experiments detector strategies: overview 3 Content: third lecture • Overview of experimental techniques example: theoretical predictions and experimental limits vanilla exclusion plot WIMP mass and cross section determination complementarity between different targets and astrophysical uncertainties • Cryogenic experiments at mK temperatures Principles of phonon mediated detectors Detection of
    [Show full text]
  • DARWIN: Dark Matter WIMP Search with Noble Liquids
    DARWIN: dark matter WIMP search with noble liquids Laura Baudis∗† Physik Institut, University of Zurich E-mail: [email protected] DARWIN (DARk matter WImp search with Noble liquids) is an R&D and design study towards the realization of a multi-ton scale dark matter search facility in Europe, based on the liquid argon and liquid xenon time projection chamber techniques. Approved by ASPERA in late 2009, DAR- WIN brings together several European and US groups working on the existing ArDM, XENON and WARP experiments with the goal of providing a technical design report for the facility by early 2013. DARWIN will be designed to probe the spin-independent WIMP-nucleon cross sec- tion region below 10−47cm2 and to provide a high-statistics measurement of WIMP interactions in case of a positive detection in the intervening years. After a brief introduction, the DARWIN goals, components, as well as its expected physics reach will be presented. arXiv:1012.4764v1 [astro-ph.IM] 21 Dec 2010 Identification of Dark Matter 2010-IDM2010 July 26-30, 2010 Montpellier France ∗Speaker. †DARWIN Project Coordinator; on behalf of the DARWIN consortium. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/ DARWIN: dark matter WIMP search with noble liquids Laura Baudis 1. Introduction One of the most exciting topics in physics today is the nature of Dark Matter in the Universe. Although indirect evidence for cold dark matter is well established, its true nature is not yet known. The most promising explanation is Weakly Interacting Massive Particles (WIMPs), for they would naturally lead to the observed abundance and they arise in many of the potential extensions of the Standard Model of particle physics.
    [Show full text]
  • Neutrino Physics with Multi-Ton Scale Liquid Xenon Detectors
    Prepared for submission to JCAP Neutrino physics with multi-ton scale liquid xenon detectors L. Baudis,a;1 A. Ferella,a;b A. Kish,a A. Manalaysay,a;e T. Marrodán Undagoitiaa;c and M. Schumanna;d aPhysik Institut, University of Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland bLaboratorio Nazionale del Gran Sasso, 67010 Assergi, Italy cMax-Planck-Institut für Kernphysik, 69117 Heidelberg, Germany dAlbert Einstein Center for Fundamental Physics, Universität Bern, 3012 Bern, Switzerland eDepartment of Physics, University of California Davis, 95616 Davis, CA, USA E-mail: [email protected], [email protected], [email protected], [email protected], [email protected], [email protected] Abstract. We study the sensitivity of large-scale xenon detectors to low-energy solar neu- trinos, to coherent neutrino-nucleus scattering and to neutrinoless double beta decay. As a concrete example, we consider the xenon part of the proposed DARWIN (Dark Matter WIMP Search with Noble Liquids) experiment. We perform detailed Monte Carlo simula- tions of the expected backgrounds, considering realistic energy resolutions and thresholds in the detector. In a low-energy window of 2–30 keV, where the sensitivity to solar pp and 7Be-neutrinos is highest, an integrated pp-neutrino rate of 5900 events can be reached in a fiducial mass of 14 tons of natural xenon, after 5 years of data. The pp-neutrino flux could thus be measured with a statistical uncertainty around 1%, reaching the precision of so- lar model predictions. These low-energy solar neutrinos will be the limiting background to the dark matter search channel for WIMP-nucleon cross sections below ∼2×10−48 cm2 and WIMP masses around 50 GeV·c−2, for an assumed 99.5% rejection of electronic recoils due to elastic neutrino-electron scatters.
    [Show full text]
  • Swiss Neutrino Programme Laura Baudis Nicola Serra Alain Blondel
    Swiss Neutrino Programme Laura Baudis Nicola Serra Alain Blondel Teresa Montaruli Antonio Ereditato André Rubbia Swiss Neutrino Programme Basic Neutrino Properties Neutrino Oscillation Physics (supported by relevant theoretical activities) Year 2015 FTE: 19 PhD students, 21.5 PostDocs, 10.25 Senior, 9 Technicians. (30 June 2015, CHIPP) I. Kreslo, 1.04.2016 RECFA visit to Switzerland -- ETHZ 2 Past results from experiments on neutrino properties Search for Majorana neutrinos with the first two years of EXO-200 data, J. B. Albert et al, (EXO collaboration), Nature 510, (2014) 229±234 First Search for Lorentz and CPT Violation in Double Beta Decay with EXO-200, J. B. Albert et al, (EXO collaboration), arXiv:1601.07266 (2016) 6 pp. Results on Neutrinoless Double-β Decay of Ge76 from Phase I of the GERDA Experiment M. Agostini et al. (GERDA Collaboration) Phys. Rev. Lett. 111 (2013) 122503 I. Kreslo, 1.04.2016 RECFA visit to Switzerland -- ETHZ 3 Past results from neutrino oscillation experiments Measurement of Neutrino Oscillation by the K2K Experiment, M. H. Ahn et al. (K2K Collaboration), Phys. Rev. D 74 (2006), 072003 Indication of Electron Neutrino Appearance from an Accelerator-Produced Off-Axis Muon Neutrino Beam K. Abe et al. (T2K Collaboration), Phys. Rev. Lett. 107 (2011) 041801 Observation of Electron Neutrino Appearance in a Muon Neutrino Beam K. Abe et al. (T2K Collaboration), Phys. Rev. Lett. 112 (2014) 061802 Measurements of π± differential yields from the surface of the T2K replica target for incoming 31 GeV/c protons with the NA61/SHINE spectrometer at the CERN SPS N. Abgrall et al., CERN-EP-2016-057, arXiv:1603.06774 Discovery of tau neutrino appearance in the CNGS neutrino beam with the OPERA experiment, N.
    [Show full text]
  • European Astroparticle Physics Strategy
    European priorities for Astroparticle Physics M. Spiro IN2P3/CNRS AppEC Chairman 1 What is ApPEC? ¾ ApPEC created in 2001 by the national funding agencies of France, Germany, Italy, the Netherlands and UK. ¾ Since then Spain, Belgium, Portugal, Greece, Switzerland and Poland have joined ¾ ApPEC aims to ¾ Promote and facilitate co-operation within the European Particle Astrophysics (PA) community ¾ Develop and promulgate long term strategies for European PA, offering advice to national funding agencies and EU ¾ Assist in improving links and co-ordination between European PA and the scientific programmes of organisations such as CERN, ESA, and ESO ¾ Express their collective views on PA in appropriate international forums, such as OECD, UNESCO etc. 2 Operation ¾ ApPEC operates ¾ Strategically through its Steering Committee, ¾ Operationally through its Peer Review Committee ¾ Steering Committee (SC): ¾ France: M.Spiro, P.Chomaz, S.Katsanevas Germany: T. Berghöfer, R.Köpke, H. Bluemer, Netherlands: F. Linde, UK: D. Miller, J. Womerseley , Italy: R. Petronzio B. Dettore, Spain: J. Fuster, A.Ferrer, Switzerland: M. Bourquin, Belgium: D. Bertrand, C. DeClerq, Portugal K. Gaspar Greece: D. Nanopoulos Poland S. Pokorski , Romania NV. Zamfir, CERN: D. Schlatter ¾ Peer Review Committee (PRC) ¾ Elena Aprile, Laura Baudis, Jose Bernabeu, Pierre Binetruy,Christian Spiering, Franz v. Feilitzsch, Enrique Fernandez,Andrea Giuliani, Werner Hofmann, Uli Katz, Paul Kooijman, Paolo Lipari, Manel Martinez, Antonio Masiero,Benoit Mours, Francesco Ronga, Sheila Rowan, Andre Rubbia, Subir Sarkar, Guenther Sigl, Gerard Smadja, Nigel Smith, Lucia Votano 3 The ASPERA program ¾ ASPERA, 14 countries ( ApPEC+ Czech republic +Sweden + CERN) funded by EU in 2006 for 3 years for coordination actions ¾ Coordinator S.
    [Show full text]
  • DARWIN Dark Matter Wimp Search with Noble Liquids
    DARWIN DARk matter WImp search with Noble liquids Laura Baudis University of Zurich (on behalf of the DARWIN Consortium) darwin.physik.uzh.ch IDM2010 University of Montpellier, July 30, 2010 Friday, July 30, 2010 1 ARRENBERG, BAUDIS, KONG, MATCHEV, AND YOO PHYSICAL REVIEW D 78, 056002 (2008) proportional light signals induced by particles interacting sensitive to both SD and SI WIMP-nucleon couplings. The in the sensitive liquid xenon (LXe) volume. The 3D posi- production of bubbles is monitored optically and via sound tion sensitivity, the self-shielding of LXe, and the prompt emission, reaching a reconstructed 3D spatial resolution of versus proportional light ratio are the most important back- 1 mm. It allows one to reject boundary events and to ground rejection features. The first results, using identify multiple neutron interactions. The most recent 136 kg-days exposure after cuts, demonstrated that COUPP results set the most sensitive limit on SD WIMP- LXe can be used for stable, homogeneous, large scale proton cross sections for a WIMP mass below 30 GeV. As dark matter detectors, providing excellent position resolu- an example, the upper bound on the SD coupling is 2:7 1  tion and discrimination against the electron recoil back- 10À pb at a WIMP mass of 40 GeV. ground. The derived upper bound on SI cross sections on In Fig. 8 we show the current CDMS and XENON10 8 nucleons is 4:5 10À pb for a WIMP mass of 30 GeV. upper bounds for the SI cross section together with pro- Since natural Xe contains 129Xe (26.4%) and 131Xe jected sensitivities for SuperCDMS 25 kg, XENON100, (21.2%) isotopes, each of these having an unpaired neu- and for a ton-scale detector.
    [Show full text]
  • Underground Searches for Cold Relics of the Early Universe Laura Baudis University of Florida, Gainesville, FL 32611, USA
    22nd Texas Symposium on Relativistic Astrophysics at Stanford University, Dec. 13-17, 2004 Underground Searches for Cold Relics of the Early Universe Laura Baudis University of Florida, Gainesville, FL 32611, USA We have strong evidence on all cosmic scales, from galaxies to the largest structures ever observed, that there is more matter in the universe than we can see. Galaxies and clusters would fly apart unless they would be held together by material which we call dark, because it does not shine in photons. Although the amount of dark matter and its distribution are fairly well established, we are clueless regarding its composition. Leading candidates are Weakly Interacting Massive Particles (WIMPs), which are ’cold’ thermal relics of the Big Bang, ie moving non-relativistically at the time of structure formation. These particles can be detected via their interaction with nuclei in deep-underground, low-background detectors. Experiments dedicated to observe WIMP interactions for the first time reach sensitivities allowing to probe the parameter space predicted by supersymmetric theories of particle physics. Current results of high sensitivity direct detection experiments are discussed and the most promising projects of the future are presented. If a stable new particle exists at the weak scale, it seems likely to expect a discovery within this decade. 1. Introduction fundamental physics at the weak scale. More than seventy years after Zwicky’s first ac- counts of dark matter in galaxy clusters [1], and thirty 2. Direct Detection of WIMPs five years after Rubin’s measurements of rotational ve- locities of spirals [2], the case for non-baryonic dark WIMPs can be detected directly, via their scatter- matter remains convincing.
    [Show full text]
  • Input from the DARWIN Collaboration to the European Strategy for Particle Physics
    Input from the DARWIN collaboration to the European Strategy for Particle Physics The DARWIN principal investigators: Elena Aprile (Columbia University), Francesco Arneodo (New York University Abu Dhabi), Laura Baudis (University of Zurich), Amos Breskin (Weizmann Institute of Science), Ethan Brown (Rensse- laer Polytechnic Institute), Ranny Budnik (Weizmann Institute of Science), Auke-Pieter Colijn (Nikhef and the University of Amsterdam), Jan Conrad (Stockholm University), Patrick Decowski (Nikhef and the University of Amsterdam), Guido Drexlin (Karlsruhe Institute of Technology), Klaus Eitel (Karlsruhe Institute of Technology), Ralph Engel (Karlsruhe Institute of Technology), Alfredo Ferella (Stockholm University), Walter Fulgione (INFN-Laboratori Nazionali del Gran Sasso), Horst Fischer (Universit¨atFreiburg), Peter Fischer (Heidelberg University), Michelle Galloway (University of Zurich), Luca Grandi (University of Chicago), Stephanie Hansmann-Menzemer (Heidelberg University), Bernhard Holzapfel (Karlsruhe Institute of Technology), Ben Kilminster (University of Zurich), Lawrence Krauss (Arizona State University), Rafael Lang (Purdue University), Manfred Lindner (Max-Planck-Institute f¨urNuclear Physics, Heidelberg), Teresa Marrod´anUndagoitia (Max- Planck-Institute f¨urNuclear Physics, Heidelberg), Jos´eA. Matias Lopez (University of Coimbra), Carla Macolino (LAL, Uni- versit´eParis-Sud), Kaixuan Ni (University of California, San Diego), Uwe Oberlack (Johannes Gutenberg-Universit¨atMainz), Gabriella Sartorelli (University of Bologna
    [Show full text]
  • Underground Facilities and Infrastructure Laura Baudis (U
    Report Underground Facilities and Infrastructure Laura Baudis (U. Zurich) Jeter Hall (SNOLAB) Kevin Lesko (LBNL) John Orrell (PNNL) 8 October 2020 1 Underground Facilities and Infrastructure Frontier Laura Baudis (U. Zurich) Jeter Hall (SNOLAB) Kevin Lesko (LBNL) John Orrell (PNNL) Topical Group Topical Group co-Conveners and Liaisons Co-conveners Liaisons Neutrinos Accelerator Neutrinos 0νββ Albert de Roeck UF01 Underground Facilities for Neutrinos Tim Bolton Patrick Decowski Astronomical ν Danielle Speller Gabriel Orebi Gann LXe DM LAr DM Particle DM Kaixuan Ni Emilija Pantic Hugh Lippincott UF02 Underground Facilities for Cosmic Frontier Jodi Cooley Low Mass Instrumentation Scott Hertel Eric Dahl Gravity Waves Instrumentation Frontier UF03 Underground Detectors Laura Cadonati Maurice Garcia-Sciveres Low Background Radon Cleanliness UF04 Supporting Capabilities Assay Richard Schnee Alvine Kamaha Brianna Mount Nuclear Astrophysics Geo-microbiology Geo-engineering QIS, QC UF05 Synergistic Research Daniel Robertson TBD TBD Maurice Garcia-Sciveres Early Career An Integrated Strategy for Underground Laura Baudis Jeter Hall UF06 Pietro Giampa Facilities and Infrastructure Kevin Lesko John Orrell William Thompson UF Topical Areas • UF1 – Neutrinos – Accelerator-based Neutrinos • e.g., LBNF/DUNE, Hyper-K – Non-accelerator Neutrinos • e.g., Supernova, solar, atmospheric, background n’s – Neutrinoless Double-Beta Decay • Nuclear Physics in US, but large HEP & UG overlap • UF2 – Cosmic Frontier – Direct detection of dark matter in underground locations • UF3 – General Underground Detectors – e.g., New technologies, R&D/small-scale exp., QIS, gravity 3 UF Topical Areas • UF4 – Supporting Capabilities – Low-background methods, cryogenics, other supporting… not necessarily UG, but needed for UG experiments • UF5 – Synergistic Research – Non-HEP UG science: Geo., Bio., Eng., Nuc.
    [Show full text]
  • 0.0.1 XENON Articles
    0.0.1 XENON Articles - The Search for Dark Matter Laura Baudis, European Review, Volume 26, Issue 1 February 2018, pp. 70-81, arXiv:1801.08128 - A Dual-phase Xenon TPC for Scintillation and Ionisation Yield Measurements in Liquid Xenon Laura Baudis, Yanina Biondi, Chiara Capelli, Michelle Galloway, Shingo Kazama, Alexander Kish, Payam Pakarha, Francesco Piastra, Julien Wulf, Eur. Phys. J. C78 (2018) no.5, 351, arXiv:1712.08607 - Search for Bosonic Super-WIMP Interactions with the XENON100 Experiment E. Aprile et al. (XENON Collaboration), Phys.Rev. D96 (2017) no.12, 122002, arXiv:1709.02222 - The XENON1T dark matter experiment E. Aprile et al. (XENON Collaboration), Eur. Phys. J. C77 (2017) no.12, 881, arXiv:1705.01828 - First Dark Matter Search Results from the XENON1T Experiment E. Aprile et al. (XENON Collaboration), Phys. Rev. Lett. 119 (2017) no. 18, 181301, arXiv:1705.06655 - Effective field theory search for high-energy nuclear recoils using the XENON100 dark matter detector E. Aprile et al. (XENON Collaboration), Phys. Rev. D96 (2017) no.4, 042004, arXiv:1705.02614 - Material radioassay and selection for the XENON1T dark matter experiment E. Aprile et al. (XENON Collaboration), Eur. Phys. J. C77 (2017) no.12, 890, arXiv:1705.01828 - Search for WIMP Inelastic Scattering off Xenon Nuclei with XENON100 E. Aprile et al. (XENON Collaboration), Phys. Rev. D96 (2017) no.2, 022008, arXiv:1705.05830 1 - Search for magnetic inelastic dark matter with XENON100 E. Aprile et al. (XENON Collaboration), JCAP 1710 (2017) no.10, 039, arXiv:1704.05804 Oral Presentations - L. Baudis: Illuminating the dark side: direct searches for cold dark matter in the Milky Way Elisabeth Spreadbury Lecture, UCL, London, March 14, 2018.
    [Show full text]