DOCSLIB.ORG

Event Rates for the Scattering of Weakly Interacting Massive Particles from $^{23} $ Na and $^{40} $ Ar

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Event Rates for the Scattering of Weakly Interacting Massive Particles from $^{23} $ Na and $^{40} $ Ar Event rates for the scattering of weakly interacting massive particles from 23Na and 40Ar R. Sahu1∗, V.K.B. Kota2† 1 National Institute of Science and Technology, Palur Hills, Berhampur-761008, Odisha, India and 2Physical Research Laboratory, Ahmedabad 380 009, India (Dated: September 23, 2020) Detection rates for the elastic and inelastic scattering of weakly interacting massive particles (WIMP) off 23Na are calculated within the framework of Deformed Shell Model (DSM) based on Hartree-Fock states. First the spectroscopic properties like energy spectra and magnetic moments are calculated and compared with experiment. Following the good agreement for these, DSM wave functions are used for obtaining elastic and inelastic spin structure functions, nuclear structure coefficients etc. for the WIMP-23Na scattering. Then, the event rates are also calculated with a given set of supersymmetric parameters. In the same manner, using DSM wavefunctions, nuclear structure coefficients and event rates for elastic scattering of WIMP from 40Ar are also obtained. These results for event rates and also for annual modulation will be useful for the upcoming and future WIMP detection experiments involving detectors with 23Na and 40Ar. I. INTRODUCTION the NaI(Tl) detector. In these experiments, the predicted annual modulation was not yet confirmed [11]. Other re- There is now universal agreement among the cosmolo- lated experiments with NaI detectors are ANAIS [18] and gists, astronomers and physicists that most of the mass DM-Ice [19]. Also, there are the important DARKSIDE- 50 [20] and DEAP-3600 [21] experiments using lquid Ar- of the universe is dark [1–3]. There are overwhelming 40 evidences to believe that the dark matter is mostly non- gon (with Ar) as detector. baryonic. Also, data from the Cosmic Background Ex- Let us add that direct detection experiments are ex- plorer (COBE) [4] and Supernova Cosmology project [5] posed to various neutrino emissions. The interaction suggest that most of the dark matter is cold. The non- of these neutrinos especially the astrophysical neutrinos baryonic cold dark matter is not yet observed in earth- with the material of the dark matter detectors known as bound experiments and hence its nature is still a mys- the neutrino floor is a serious background source. Re- tery. Axions are one of the candidates for dark matter cently the coherent elastic scattering of neutrinos off nu- but they are not yet observed [1, 6]. However, the most clei (CEνNS) has been observed at the Spallation Neu- promising nonbaryonic cold dark matter candidates are tron Source at the Oak Ridge National Laboratory [22] the Weakly Interacting Massive Particles (WIMP) which employing the technology used in the direct detection of arise in super symmetric theories of physics beyond the dark matter searches. The impacts of the neutrino floor standard model. The most appealing WIMP candidate on the relevant experiments looking for cold dark matter is the Lightest Supersymmetric Particle (LSP) (lightest was investigated for example in [23]. neutralino) which is expected to be stable and interacts There are many theoretical calculations which de- weakly with matter [1, 7]. scribe different aspects of direct detection of dark mat- There are many experimental efforts [8–11] to detect ter through the recoil of the nucleus in WIMP-nucleus WIMP via their scattering from the nuclei of the detector scattering. For elastic scattering, we need to consider providing finger-prints regarding their existence. Some of spin-spin interaction coming from the axial current and these are Super CDMS SNOLAB project, XENON1T, also the more dominant scalar interaction. For inelastic arXiv:2009.10522v1 [nucl-th] 19 Sep 2020 PICO-60, EDELWEISS and so on; see for example part, scalar interaction practically does not contribute. [11–14]. Nuclei 23Na, 40Ar, 71Ga, 73Ge, 75As, 127I, The scalar interaction can arise from squark exchange, 133Cs and 133Xe are among the popular detector nu- Higgs exchange, the interaction of WIMPs with gluons clei; see [10, 11, 15] and references there in. Our fo- etc. Suhonen and his collaborators have performed a cus in this paper is on 23Na and 40Ar. The Sodium series of truncated shell model calculations for this pur- Iodide (NaI) Advanced Detector (NAID) array experi- pose [24–28]. In these studies, for example they have ment is a direct search experiment for WIMP operated by calculated the event rates for WIMP-nucleus elastic and 83 125 127 UK Dark Matter Collaboration in North Yorkshire [16]; inelastic scattering for Kr and Te [28] and also I, 129,131 133 the NaI contains 23Na. Similarly, the DAMA/NaI and Xe and Cs [26]. In addition, recently Vergados DAMA/LiBRA [17] experiments investigated the pres- et al [29] examined the possibility of detecting electrons ence of dark matter particles in the galactic halo using in the searches for light WIMP with a mass in the MeV region and found that the events of 0.5-2.5 per kg-y would be possible. Few years back full large-scale shell-model calculations are carried out in [15, 30] for WIMP scat- 129,131 127 73 19 23 27 29 ∗[email protected] tering off Xe, I, Ge, F, Na, Al and Si †[email protected] nuclei. Finally, using large scale shell model [31] and 2 75 coupled cluster theory [32] WIMP-nucleus and neutrino- 6 As 40 nucleus scattering respectively, with Ar, are studied. 9/2+ In recent years, the deformed shell model (DSM), 4 based on Hartree-Fock (HF) deformed intrinsic states with angular momentum projection and band mixing, 7/2+ 2 + has been established to be a good model to describe 9/2 5/2− the properties of nuclei in the mass range A=60-90 [33]. 5/2+ 0 − Among many applications, DSM is found to be quite suc- x x 1/2 + + 3/2 7/2 xx − cessful in describing spectroscopic properties of medium xx 3/2 x x 1/2+ heavy N=Z odd-odd nuclei with isospin projection [34], −2 double beta decay half-lives [35, 36] and µ e conversion 5/2+ − − 5/2 x x 3/2− in the field of the nucleus [37]. Going beyond these ap- −4 x x 1/2− Energy (MeV) plications, recently we have studied the event rates for 1/2−,3/2+ 73 + − WIMP with Ge as the detector [38]. In addition to the 1/2 ,3/2 −6 energy spectra and magnetic moments, the model is used x x 1/2− to calculate the spin structure functions, nuclear struc- 3/2− o −8 − ture factors for the elastic and inelastic scattering. Fol- 1/2 o o lowing this successful study, we have recently used DSM for calculating the neutrino-floor due to coherent elastic −10 neutrino-nucleus scattering (CEνNS) [23] for the candi- 1/2− o o date nuclei 73Ge, 71Ga, 75As and 127I. We found that E=−30.23 (MeV) Q=28.02 the neutrino-floor contributions may lead to a distortion K=3/2− of the expected recoil spectrum limiting the sensitivity of the direct dark matter search experiments. In [10], FIG. 1: HF single-particle spectra for 75As corresponding to DSM results for WIMP scattering from 127I, 133Cs and lowest prolate configuration. In the figure, circles represent 133Xe are described in detail. To complete these stud- protons and crosses represent neutrons. The HF energy E in ies that use DSM for the nuclear structure part, in the MeV, mass quadrupole moment Q in units of the square of the present paper we will present results for WIMP- 23Na oscillator length parameter and the total azimuthal quantum elastic and inelastic scattering and WIMP-40Ar elastic number K are given in the figure. scattering. Now we will give a preview. Section II gives, for completeness and easy reading of pleteness we give here a few important steps. In the case the paper, a brief discussion of the formulation of WIMP- of spin-spin interaction, the WIMP couples to the spin nucleus elastic and inelastic scattering and event rates. In of the nucleus and in the case of scalar interaction, the Section III the DSM formulation is described with exam- WIMP couples to the mass of the nucleus. In the ex- ples drawn from 75As spectroscopic results. In Section pressions for the event rates, the super-symmetric part is IV, spectroscopic results and also the results for elas- separated from the nuclear part so that the role played tic and inelastic scattering of WIMP from 23Na are pre- by the nuclear part becomes apparent. sented. Similarly, WIMP-40Ar elastic scattering results are presented in Section V. The results in Sections IV and V are the main results of this paper. Finally, concluding A. Elastic scattering remarks are drawn in Sect. VI. The differential event rate per unit detector mass for a WIMP with mass mχ can be written as [1], II. EVENT RATES FOR WIMP-NUCLEUS SCATTERING dσ dR = N φf d3v d q 2 (1) t d q 2 | | WIMP flux on earth coming from the galactic halo | | 5 2 is expected to be quite large, of the order 10 per cm Here, φ which is equal to ρ0v/mχ is the dark matter flux per second. Even though the interaction of WIMP with with ρ0 being the local WIMP density. Similarly, Nt matter is weak, this flux is sufficiently large for the galac- stands for the number of target nuclei per unit mass and tic WIMPs to deposit a measurable amount of energy in f is the WIMP velocity distribution which is assumed to an appropriately sensitive detector apparatus when they be Maxwell-Boltzmann type. It takes into account the scatter off nuclei. Most of the experimental searches of distribution of the WIMP velocity relative to the detector WIMP is based on the direct detection through their in- (or earth) and also the motion of the sun and earth.
Load more

Recommended publications
  • 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).
    [Show full text]
  • 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.
    [Show full text]
  • 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
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • The Current Status and Planned Developments for Deep Underground Astro-Particle Physics Science Facilities
    12th International Conference on Topics in Astroparticle and Underground Physics (TAUP 2011) IOP Publishing Journal of Physics: Conference Series 375 (2012) 042059 doi:10.1088/1742-6596/375/4/042059 The Current Status and Planned Developments for Deep Underground Astro-particle Physics Science Facilities N.J.T.Smith SNOLAB, 1039 Regional Road 24, Lively, Ontario, P3Y 1N2, Canada E-mail: [email protected] Abstract. The rigorous radiation background constraints imposed by several studies in particle and astro-particle physics, such as Galactic dark matter searches, man-made, terrestrial, solar and supernova neutrino studies and 0νββ-decay studies, require deep underground science facilities to afford shielding from penetrating cosmic rays and their secondary by-products. New threads of research focused on deep sub-surface biology, chemistry, geology and engineering have also been developing rapidly at several sites, benefitting from the significant investment in underground access and infrastructure developed. In addition to planned, or completed, expansion at several of these deep underground facilities, additional new facilities are in early stages of construction or well advanced planning. These developments provide significant additional capability to these fields of study. This paper summarises the developments at these facilities, focused on those extremely deep uderground laboratories where expansion is underway or planned. 1. Introduction Searches for rare decay channels or weak interactions in particle or astro-particle physics studies require the observation of rare events in dedicated detector systems. These rare events need to be observed against the significant backgrounds created by cosmic-ray and radioactive- contaminant generated signals. To enable the observation of these exquisite signal events, experiments must therefore be operated in the quiet environment afforded by shielded facilities in deep underground laboratories.
    [Show full text]
  • Results from the DAMA/LIBRA Experiment R Bernabei, P Belli, F Cappella Et Al
    Journal of Physics: Conference Series OPEN ACCESS Related content - DAMA/LIBRA results and perspectives Results from the DAMA/LIBRA experiment R Bernabei, P Belli, F Cappella et al. - Performances of the new high quantum To cite this article: R Bernabei et al 2010 J. Phys.: Conf. Ser. 203 012003 efficiency PMTs in DAMA/LIBRA R Bernabei, P Belli, A Bussolotti et al. - ANAIS status report J Amaré, S Borjabad, S Cebrián et al. View the article online for updates and enhancements. Recent citations - Flavored dark matter in direct detection experiments and at the LHC Jennifer Kile and Amarjit Soni - Singlet Majorana fermion dark matter, DAMA, CoGeNT, and CDMS-II C. de S. Pires et al - Effect of low mass dark matter particles on the Sun Marco Taoso et al This content was downloaded from IP address 170.106.202.226 on 30/09/2021 at 09:16 Topics in Astroparticle and Underground Physics (TAUP 2009) IOP Publishing Journal of Physics: Conference Series 203 (2010) 012003 doi:10.1088/1742-6596/203/1/012003 Results from the DAMA/LIBRA experiment RBernabei1,2, P Belli 2, F Cappella 3,4,RCerulli5,CJDai6,A d’Angelo 3,4,HLHe6, A Incicchitti 4, H H Kuang 6,XHMa6,F Montecchia 2,7, F Nozzoli 1,2,DProsperi3,4, X D Sheng6 and Z P Ye6,8 1 Dip. di Fisica, Universit`a di Roma “Tor Vergata”, I-00133 Rome, Italy 2 INFN, sez. Roma “Tor Vergata”, I-00133 Rome, Italy 3 Dip. di Fisica, Universit`a di Roma “La Sapienza”, I-00185 Rome, Italy 4 INFN, sez.
    [Show full text]
  • How Zwicky Already Ruled out Modified Gravity Theories Without Dark Matter
    How Zwicky already ruled out modified gravity theories without dark matter Theodorus Maria Nieuwenhuizen1,2 1Institute for Theoretical Physics, University of Amsterdam, Science Park 904, 1090 GL Amsterdam, The Netherlands 2International Institute of Physics, UFRG, Lagoa Nova, Natal - RN, 59064-741, Brazil Various theories, such as MOND, MOG, Emergent Gravity and f(R) theories avoid dark matter by assuming a change in General Relativity and/or in Newton’s law. Galactic rotation curves are typically described well. Here the application to galaxy clusters is considered, focussed on the good lensing and X-ray data for A1689. As a start, the no-dark-matter case is confirmed to work badly: the need for dark matter starts near the cluster centre, where Newton’s law is still supposed to be valid. This leads to the conundrum discovered by Zwicky, which is likely only solvable in his way, namely by assuming additional (dark) matter. Neutrinos with eV masses serve well without altering the successes in (dwarf) galaxies. Keywords: MOND, MOG, f(R), Emergent Gravity, galaxy cluster, Abell 1689, dark matter, neutrinos I. INTRODUCTION Niets is gewichtiger dan donkere materie52 Dark matter enters the light in 1922 when Jacobus Kapteyn employs this term in his First Attempt at a Theory of the Arrangement and Motion of the Sidereal System1. It took a decade for his student Jan Oort to work out the stellar motion perpendicular to the Galactic plane, and to conclude that invisible mass should exist to keep the stars bound to the plane2. Next year, in 1933, Fritz Zwicky applied the idea to the Coma galaxy cluster and concluded that it is held together by dark matter.
    [Show full text]
  • Radiopurity Measurement of Acrylic for the DEAP-3600 Dark Matter Experiment
    Radiopurity measurement of acrylic for the DEAP-3600 dark matter experiment by Corina Michelle Nantais A thesis submitted to the Department of Physics, Engineering Physics & Astronomy in conformity with the requirements for the degree of Master of Science Queen's University Kingston, Ontario, Canada January 2014 Copyright c Corina Michelle Nantais, 2014 Abstract The liquid argon target of the DEAP-3600 dark matter detector is contained by an extremely radiopure acrylic vessel. Alpha decays from the inner surface of the acrylic vessel are a source of background. If a fraction of the alpha energy is observed, or if the recoiling nucleus from the alpha decay is observed, the event will not be separated from a dark matter candidate event. In addition to the low level of inherent contamination from uranium and thorium, the 210Pb from 222Rn diffusion during manufacturing must be measured. The limit for the DEAP-3600 acrylic vessel is 1:1 × 10−20 g/g 210Pb. By vaporizing a large quantity of acrylic and counting the concentrated residue with an ultralow background HPGe well detector and a low background alpha spectrometer, the bulk acrylic was found to have an upper limit of 10−19 g/g 210Pb. The design, installation, commissioning, operation, and analysis for various aspects of the acrylic assay are described. i Acknowledgments I'd like to thank the following people: my supervisor, Mark Boulay, for his contagious enthusiasm for DEAP and for sending me to many conferences to advertise; Chris Jillings, for his encouragement; Bruce Cleveland, for
    [Show full text]
  • Open Problems in Dark Matter Phenomenology
    Open problems in dark matter phenomenology G. Bélanger LAPTH Annecy-le-Vieux DMAstroLHC GGI, Firenze, 29 August 2017 What do we know about dark matter? It has gravitational interactions (galaxies – rotation curves- galaxy clusters, - Xray, gravitational lensing) No electromagnetic interactions It is cold (or maybe warm) and collisionless What do we know about dark matter? Within LCDM model – precisely know its relic density 2 Wcdm h =0.1193+/- 0.0014 (PLANCK – 1502.01589) That’s it !! Leaves us with a lot of possibilities for dark matter In particular from the particle physics point of view (Cannot be baryons, neutrinos (too hot)) Open problems • Is DM a new particle : a fermion, a scalar, a vector? an elementary particle? • DM mass and interaction strength? • One or more dark matter particles? • Large Self-interactions? • DM/anti-DM asymmetry related to baryon asymmetry? • Density depends on initial asymmetry and freeze-out • Primordial Black Hole? • Revived from LIGO grav.wave obs, I. Cholis et al, PRL116, 201301(2016) • Could make up all of the DM, Kuhmel, Freese, PRD95, 083508 (2017) • What can we learn from collider -astroparticle experiments? Mass scale/Interaction scale WIMPs FIMPs SIMPs GIMPs Asymmetric SIDM L. Roszkowski Progress in last 20 years • 20 years ago we knew what DM was made of: neutralino in supersymmetry • R parity needed to avoid proton decay predicts a stable LSP – WIMP • We knew how to look for it, Direct detection, indirect detection, LHC • Planned to measure its properties : use collider information and confront
    [Show full text]
  • Analysis of Backgrounds for the ANAIS-112 Dark Matter Experiment
    Eur. Phys. J. C (2019) 79:412 https://doi.org/10.1140/epjc/s10052-019-6911-4 Regular Article - Experimental Physics Analysis of backgrounds for the ANAIS-112 dark matter experiment J. Amaré1,2, S. Cebrián1,2,a , I. Coarasa1,2, C. Cuesta1,4, E. García1,2, M. Martínez1,2,3,M.A.Oliván1,5, Y. Ortigoza1,2, A. Ortiz de Solórzano1,2, J. Puimedón1,2, A. Salinas1,2, M. L. Sarsa1,2, J. A. Villar1,2, P. Villar1,2 1 Laboratorio de Física Nuclear y Astropartículas, Universidad de Zaragoza, Calle Pedro Cerbuna 12, 50009 Zaragoza, Spain 2 Laboratorio Subterráneo de Canfranc, Paseo de los Ayerbe s/n, 22880 Canfranc Estación, Huesca, Spain 3 Fundación Agencia Aragonesa para la Investigación y el Desarrollo, ARAID, Gobierno de Aragón, Avenida de Ranillas 1-D, 50018 Zaragoza, Spain 4 Present Address: Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, CIEMAT, 28040 Madrid, Spain 5 Present Address: Fundación CIRCE, 50018 Zaragoza, Spain Received: 5 December 2018 / Accepted: 3 May 2019 / Published online: 15 May 2019 © The Author(s) 2019 Abstract The ANAIS (Annual modulation with NaI(Tl) 1 Introduction Scintillators) experiment aims at the confirmation or refuta- tion of the DAMA/LIBRA positive annual modulation signal Experimental efforts looking for Weakly Interacting Massive in the low energy detection rate, using the same target and Particles (WIMPs), one of the preferred categories of the technique, at the Canfranc Underground Laboratory (LSC) in hypothetical dark matter particles our galactic halo should Spain. ANAIS-112, consisting of nine 12.5 kg NaI(Tl) mod- consist of in order to explain the Milky Way’s rotation ules produced by Alpha Spectra Inc.
    [Show full text]
  • ANAIS-112 Sensitivity in the Search for Dark Matter Annual Modulation
    Eur. Phys. J. C (2019) 79:233 https://doi.org/10.1140/epjc/s10052-019-6733-4 Regular Article - Experimental Physics ANAIS-112 sensitivity in the search for dark matter annual modulation I. Coarasa1,2,a ,J.Amaré1,2, S. Cebrián1,2, C. Cuesta1,2,4, E. García1,2, M. Martínez1,2,3,M.A.Oliván1,5, Y. Ortigoza1,2, A. Ortiz de Solórzano1,2, J. Puimedón1,2, A. Salinas1,2, M. L. Sarsa1,2, P. Villar1,2, J. A. Villar1,2 1 Grupo de Física Nuclear y Astropartículas, Universidad de Zaragoza, Calle Pedro Cerbuna 12, 50009 Zaragoza, Spain 2 Laboratorio Subterráneo de Canfranc, Paseo de los Ayerbe s/n, 22880 Canfranc Estación, Huesca, Spain 3 Fundación Agencia Aragonesa para la Investigación y el Desarrollo, ARAID, Avenida de Ranillas 1-D, 50018 Zaragoza, Spain 4 Present Address: Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, CIEMAT, 28040 Madrid, Spain 5 Present Address: Centro de Investigación de Recursos y Consumos Energéticos, CIRCE, 50018 Zaragoza, Spain Received: 5 December 2018 / Accepted: 28 February 2019 © The Author(s) 2019 Abstract The annual modulation measured by the DAMA/ other target materials and techniques (like those from CDMS LIBRA experiment can be explained by the interaction of [11], CRESST [12], EDELWEISS [13], KIMS [14], LUX dark matter WIMPs in NaI(Tl) scintillator detectors. Other [15], PICO [16], XENON [17] or DarkSide [18,19] collab- experiments, with different targets or techniques, exclude the orations) have been ruling out for years the most plausible region of parameters singled out by DAMA/LIBRA, but compatibility scenarios. Nevertheless, DAMA/LIBRA has the comparison of their results relies on several hypothe- accumulated up to now twenty annual cycles in the [2,6] ses regarding the dark matter model.
    [Show full text]