=> Ωmatter >> Ωbaryon
|
|
- Alannah Spencer
- 5 years ago
- Views:
Transcription
1 Cryogenic Detectors Direct Search Cryogenic Detectors CRESST Project
2 Cosmic Microwave Background Matter-Density Ωmatter Anisotropy: Angular scale => geometry, Ωtot Wilkinson Microwave Anisotropy Probe Ωtot=1 Intensities => gravitational potentials, matter densities - gravitation Ωmatter - coupling to radiation Ωbaryon Ωmatter = 0.27 => Ωmatter φ Ωlum = 0.01 mostly Ωbaryon = u d e => Ωmatter >> Ωbaryon
3 Structure in the Universe and Neutrinos Ω matter ~ 0.30 Ω ν < 0.02 Ω < 0.02 ν Σmν i < 1.2eV
4 Cosmic Microwave Background Nucleosynthesis Large Scale Structure Gravitational Lensing Hot Gas kinetic Energy Cluster Velocity Dispersion Galaxy Rotation Curves Ω matter >Ω lum dark Ω Ω matter >Ω baryons exotic non-baryonic, not neurtinos
5 Matter in the Universe - Composition d u e normal baryonic matter < ν < 0.02 (HDM) from ν oscillations => Σm ν > 0.05eV Ω mat = ν e? cold (CDM) 0.23 ν too light => most of the is cold Axions, weakly interacting, massive particles WIMPs (50GeV~1000GeV Neutralino?) physics beyond standard model supersymmetry?
6 Dark Matter search for physics beyond the Standard Model new elementary particles AXIONs??? Supersymmetry???.
7 Cosmology and Dark Energy structure formation nucleosynthesis leptogenesis, baryon-asymmetry supernovae UHE cosmic rays Beyond the Standard Model SUSY, unification of fundamental interactions why flavour-symmetry, CPT & Lorentz inv. extra dimensions Experiments Neutrino Physics search for: - neutrino less double beta decay - particles high energy high precision rare effects rare events => very good knowledge on background neutrino-oscillations finite neutrino mass => SM? absolute mass scale? Majorana- or Dirac? right handed neutrinos? CP violation?
8 How to detect WIMP Weakly Interacting Massive Particles = WIMPs elastic scattering on nuclei nuclear recoils: reduced efficiency of charge or light production -mass 50 GeV - ~ 1000 TeV - relative speed 270 km/s χ only a few kev of energy - cross section - local WIMP-density σ χ < cm 2 ρ χ =0.3 GeV / cm 3 - corresp. 3 WIMPs (100GeV) / liter /s /cm 2 very very rare scattering events (< 1 / week / kg)
9 WIMP Direct Detection - Low Temperature Calorimeter particle absorption => phonons (~heat) phonon-absorption in thermometer => temperature rise low temperatures (~20mK) => high sensitivity, small C absorber-crystal detected particle (WIMP) thermometer coupling to heat sink high sensitivity to nuclear recoils no quenching low energy threshold wide choice of absorber materials thermometer types: superconducting phase transition thermometers (SPT) NTD - Ge thermistors (highly doped semiconductors)
10 Superconducting Phase Transition Thermometer superconducting phase transition thermometer Tungsten Tc 15mK heat capacity Sapphire 250gr 2 MeV / 25mK 130 GeV / 1K Sapphire- or CaWO 4 -absorber 250gr, 4cm x 4cm x 4cm CRESST-Collaboration Cryogenic Rare Event Search with Superconducting Thermometers Max-Planck-Institut München, TU München Universität Tübingen, Oxford University, Gran Sasso Lab
11 WIMP Direct Detection - Signal and Background Detector rate, spectrum required sensitivity ~ 1 event / kg / week (future experiments even 100 x less) radioactivity: > 1Hz/kg ~ 10 6 events /kg /week => clean shielding: (old) Pb, Cu muons ~ 0.1Hz/kg: ~ 10 5 events /kg /week, => needs ~ 1.5 km Rock => Underground-Laboratory
12 WIMP Direct Detection - Underground Laboratory shielding from cosmic rays Soudan Mine USA Modane Gran Sasso Lab
13 electromagnetic γ, β nuclear recoils e - χ e - ionisation (charge, scintillation light) phonons only little ionisation
14 Phonon + Charge / Light Measurement => recognize Background thermometer χ CRESSTII-detectors simultaneous light and phonon measurement thermometer absorber CaWO 4 phonon-detector light detector (low T calorimeter) reflecting foil CRESST Cryogenic Rare Event Search with Superconducting Thermometers
15 CRESST Light Phonon Detectors
16 CRESST Light Phonon Detectors - Particle Identification γ α CaWO 4 n
17 WIMP Direct Detection Event by Event Discrimination EDELWEISS (France) und CDMS (USA) Projects Ioniosation-Phonon 320g Ge-Detector Low Background Data Testmessung mit Neutronen (=> Kernrückstöße) Ionisation/Recoil Ratio EDELWEISS 2002 PRELIMINARY γ band Neutron calibration GGA1 nuclear recoil band Ionisation/Recoil Ratio Thermometer Ge 300gr oder Si 300gr Ionisation EDELWEISS 2002 PRELIMINARY γ band GGA1 60 Co Calibration nuclear recoil band Recoil Energy (kev) Recoil Energy (kev)
18 Heat / Charge - reduced charge collection from surface
19 CDMS Charge & Phonon Detectors I bias SQUID array R bias R feedback Phonon D 250 g Ge or 100 g Si crystal 1 cm thick x 7.5 cm diameter Photolithographic patterning Phonon sensors: 4 quadrants with each 888 sensors (TES) operated in parallel D A TES: 1-μm-thick strip of W connected to 8 superconducting Al collection fins C B z y x V qbias Q outer Q outer Q inner inner Measure ionization in low-field (~volts/cm) with segmented contacts to allow rejection of events near outer edge 2 charge electrodes: Inner fiducial electrode Outer guard ring 1 μ tungsten 380μ x 60μ aluminum fins
20 CDMS Timing Cut remove near surface events charge / heat ~ rise time
21 CDMS data 2004/2005 Prior to timing cuts After timing cuts Charge Yield Charge Yield
22 CRESST at Gran Sasso Underground Laboratory Max-Planck-Institut München TU München Universität Tübingen Oxford University Gran Sasso Lab
23 CRESST at Gran Sasso Underground Laboratory
24 CRESST at Gran Sasso Underground Laboratory
25 Nuclear Recoils - Examples data end 2003: 8.1 kg days 46 kev Linie von externer 210 Pb Kontamination no Beta-Tail => external recoiling nuclei from α-decays below region of O-recoils (CaWO 4, O-recoils dominatte calibration with AmBe-source) countrate as expected from external neutrons (1 count/kg/day) CRESST I at that time no neutron shield only γ: Pb/Cu shield detector α reflector larger quenching for heavy nucleii? meanwhile PE moderator shield and muon-veto
26 CRESST: Results with Phonon-Light Detectors data spring 2004: kg days different quenching factors for O- and W-recoils O-recoils => distinguish neutrons (O-recoils) from WIMPs (W-recoils ~A 2 )? W-recoils data taken without neutron shield => neutron rate as expected from radioactivity in rock now: 40cm polyethylene around set-up
27 CRESST 66 channel SQUID system and detectors
28 CaWO 4 - α Nachweis Light γ band α band α-spectrum t 1/2 ( 180 W) = (1.7 ± 0.2) y U/Th 1,7 10 Recoil 18 a energy [kev] σ ~ 4 Phys.Rev.C 70 (2004) und nucl-ex/
29 CRESST 2004 no neutron shield Run28, 2004, 10.5 kg d light / heat γ, β nuclear recoils: dark matter, neutrons heat / kev CaWO 4 crystals as target 90% O-recoils 90% W-recoils
30 CRESST neutron shield Shielded cryostat PE neutron moderator Plastic scintill. μ-veto
31 CRESST 2007 preliminary (only 3kg d) vorläufig, Januar 2007, 3 kg d (Zora) Licht-/Phononenergie with neutron shield and alpha recoil rejection Energie im Phononendetektor / kev
32 Future so far : ~ 1kg targets in preparation: ~ 10kg targets => expect new results soon long term: increase sensitivity 1/week/kg to a few/year/100kg go from <1kg towards 10kg - very very good background control - some 100kg of cryogenic detectors EURECA => EURECA Collaboration
33 European Underground Rare Event Calorimeter Array Search and Find Particles Based on CRESST and EDELWEISS expertise, with additional groups joining. Target materials: Ge, CaWO 4, etc (A dependence) Mass: above 100 kg towards 1 ton Timescale: after CRESST-II and EDELWEISS-II R&D: demonstrate CRESST / EDELWEISS Collaboration started March 2005 and has formed since then
34 EURECA Collaboration CRESST + EDELWEISS + new groups United Kingdom Oxford (H Kraus, coordinator) Germany MPI für Physik, Munich Technische Universität München Universität Tübingen Universität Karlsruhe Forschungszentrum Karlsruhe Russia DLNP Dubna France CEA/DAPNIA Saclay CEA/DRECAM Saclay CNRS/CRTBT Grenoble CNRS/CSNSM Orsay CNRS/IPNL Lyon CNRS/IAP Paris CERN
35 Dark Matter search for physics beyond the Standard Model new elementary particles
Cryogenic Detectors Direct Dark Matter Search. Dark Matter
Cryogenic Detectors Direct Search Matter in the Universe - Composition ν too light => most of the is cold Ωmat = 0.27 0.04 u d of so far unknown weakly interacting, massive particles WIMPs normal baryonic
More informationDirekte Suche nach Dark Matter
Direkte Suche nach Dark Matter WIMP über elastische Streuung an Kernen HDMS Ge 10% energy Ionization Ge, Si Edelweiss, CDMS liquid Xe Zeplin-2, US-Xenon NaI, liqu.xe Target Light 1% energy fastest no surface
More informationLatest results of EDELWEISS II
Latest results of EDELWEISS II Ana Torrentó CEA/IRFU/SPP Saclay Rencontres de Moriond 2011 «EW and Unified Theories» WIMP search Motivated by the «WIMP miracle» Very small rate of WIMPnucleus scattering
More informationResults from 730 kg days of the CRESST-II Dark Matter Search
Results from 730 kg days of the CRESST-II Dark Matter Search Federica Petricca on behalf of the CRESST collaboration: Max-Planck-Institut für Physik, München TU München University of Oxford Universität
More informationDirect Search for Dark Matter
Direct Search for Dark Matter Direct Dark Matter Search Dark Matter in the Universe Ω = 0.23 non-baryonic not neutrinos physics beyond the standard model thermal relics from Big Bang weakly interacting
More informationChapter 12. Dark Matter
Karl-Heinz Kampert Univ. Wuppertal 128 Chapter 12 Dark Matter Karl-Heinz Kampert Univ. Wuppertal Baryonic Dark Matter Brightness & Rotation Curve of NGC3198 Brightness Rotation Curve measured expected
More informationDirect Search for Dark Matter
Direct Search for Dark Matter Dark Matter Search Dark Matter in the Universe physics beyond the standard model how to detect Dark Matter particles Josef Jochum Eberhard Karls Universität Tübingen Kepler
More informationEsperimenti bolometrici al Gran Sasso: CUORE e CRESST
Esperimenti bolometrici al Gran Sasso: CUORE e CRESST Marco Vignati 24 Ottobre 2011 0νDBD in Theory Nuclear process: (A,Z) (A,Z+2) + 2 e - Can only happen if lepton number is not conserved. The decay probability
More informationTechnical Specifications and Requirements on Direct detection for Dark Matter Searches
Technical Specifications and Requirements on Direct detection for Dark Matter Searches Jin Li THU/IHEP Symposium of the Sino-German GDT Cooperation 04/08/2013 Tübingen Outline Introduction Direct detection
More informationDirect Search for Dark Matter
Direct Search for Dark Matter Direct Dark Matter Search Dark Matter in the Universe Ω = 0.23 non-baryonic not neutrinos physics beyond the standard model thermal relics from Big Bang weakly interacting
More informationDark Matter Searches. Marijke Haffke University of Zürich
University of Zürich Structure Ι. Introduction - Dark Matter - WIMPs Ι Ι. ΙΙΙ. ΙV. V. Detection - Philosophy & Methods - Direct Detection Detectors - Scintillators - Bolometer - Liquid Noble Gas Detectors
More informationarxiv:astro-ph/ v1 24 Jun 2004
LATEST RESULTS OF THE EDELWEISS EXPERIMENT arxiv:astro-ph/46537v 24 Jun 24 V. SANGLARD for the Edelweiss collaboration Institut de Physique Nucléaire de Lyon, 4 rue Enrico Fermi, 69622 Villeurbanne, France
More informationCryogenic Dark Matter Search in Europe
Cryogenic Dark Matter Search in Europe Wolfgang Rau Queen s University Kingston, Canada Introduction W. Rau 2 Search for nuclear recoils (NR) from WIMP interactions. Background mostly electron recoils
More informationDown-to-earth searches for cosmological dark matter
Down-to-earth searches for cosmological dark matter Carter Hall, University of Maryland October 19, 2016 Astrophysical evidence for dark matter Galaxy cluster collisions Rotation curves Ω 380,000 years
More informationDetectors for astroparticle physics
Detectors for astroparticle physics Teresa Marrodán Undagoitia marrodan@physik.uzh.ch Universität Zürich Kern und Teilchenphysik II, Zürich 07.05.2010 Teresa Marrodán Undagoitia (UZH) Detectors for astroparticle
More informationLooking for WIMPs A Review
Looking for WIMPs A Review Beatriz E. Burrola Gabilondo There is currently a race to find out what dark matter actually is. Weakly Interacting Massive Particles (WIMPs) are a strong candidate for dark
More informationLow Background Experiments and Material Assay. Tessa Johnson NSSC Summer School July 2016
Low Background Experiments and Material Assay Tessa Johnson NSSC Summer School July 2016 Outline How do we detect particles? Some interesting questions relating to particle physics How can particle detection
More informationStatus of the EDELWEISS Dark Matter search
Status of the EDELWEISS Dark Matter search KIT Institute Centre for Particle Nuclear and Physics Astroparticle Physics KIT University of the State of Baden-Wuerttemberg and National Research Center of
More informationThe EDELWEISS DM search Phase II to Phase III
The EDELWEISS DM search Phase II to Phase III Adam Cox Karlsruhe Institute for Technology (KIT) on behalf of the EDELWEISS Collaboration CEA, Saclay (IRFU and IRAMIS) IPNL (CNRS/IN2P3 and Université de
More informationSuperCDMS SNOLAB: A G2 Dark Matter Search. Ben Loer, Fermilab Center for Particle Astrophysics On behalf of the SuperCDMS Collaboration
SuperCDMS SNOLAB: A G2 Dark Matter Search Ben Loer, Fermilab Center for Particle Astrophysics On behalf of the SuperCDMS Collaboration A bit of background Astronomical data at all scales indicates dark
More informationCryogenic Dark Matter Searches
Cryogenic Dark Matter Searches Galaxy NGC 3349, HST F. Pröbst MPI für Physik Outline Direct detection Major direct searches with cryogenic detectors: results and performance critical factors CMDS EDELWEISS,
More informationNetwork on Direct Dark Matter Search ILIAS N3
Network on Direct Dark Matter Search ILIAS N3 N3 Dark Matter 2/25/2008 ILIAS 1 ILIAS-N3 Dark Matter Network Participating Institutions France: CNRS/CEA CNRS/SPM/CRTBT Grenoble CNRS/IN2P3/IPN Lyon CNRS/IN2P3/CSNSM
More informationCryodetectors, CRESST and Background
Cryodetectors, CRESST and Background A cryogenic detector for Dark Matter with heat (phonon) readout and light (scintillation) readout MPI, TUM, Oxford, Tübingen, LNGS What we re looking for: M W imp =
More informationStatus of Dark Matter Detection Experiments
Status of Dark Matter Detection Experiments Debasish Majumdar Astroparticle Physics and Cosmology Division Saha Institute of Nuclear Physics Kolkata WIMP Hunting Going beyond gravity, three ways to detect
More informationEdelweiss-II : status and first results A new generation of background-free bolometers for WIMP search
Edelweiss-II : status and first results A new generation of background-free bolometers for WIMP search From EDWI to EDW II New ID detectors Some current results Outlook G. Gerbier CEA Saclay, IRFU, France
More informationDirect Dark Matter and Axion Detection with CUORE
Direct Dark Matter and Axion Detection with CUORE Marco Vignati University of Rome La Sapienza & INFN Rome on behalf of the CUORE collaboration Panic 11, July 5, MIT 988 TeO crystals Ton scale bolometric
More informationSensitivity of sodium iodide cryogenic scintillation-phonon detectors to WIMP signals
Journal of Physics: Conference Series PAPER OPEN ACCESS Sensitivity of sodium iodide cryogenic scintillation-phonon detectors to WIMP signals To cite this article: M Clark et al 2016 J. Phys.: Conf. Ser.
More informationThe Search for Dark Matter with the XENON Experiment
The Search for Dark Matter with the XENON Experiment Elena Aprile Columbia University Paris TPC Workshop December 19, 2008 World Wide Dark Matter Searches Yangyang KIMS Homestake LUX SNOLAB DEAP/CLEAN
More informationDirect Dark Matter and Axion Detection with CUORE
Direct Dark Matter and Axion Detection with CUORE Europhysics Conference on High-Energy Physics 2011 Cecilia G. Maiano on behalf of CUORE collaboration Contents The Bolometric Technique The CUORE experiment
More informationPoS(VERTEX 2009)026. Dark Matter search with Ge detectors. Paul L. Brink 1
Dark Matter search with Ge detectors Paul L. Brink 1 Dept. of Physics, Stanford University 382 Via Pueblo Mall, Stanford, CA 943405, USA E-mail: pbrink@stanford.edu The direct detection of Dark Matter,
More informationA survey of recent dark matter direct detection results
A survey of recent dark matter direct detection results I where we stand II recent results (CDMS, XENON10, etc) III DAMA results IV a bit about modulation V issues with DAMA results VI what to look for
More informationPHY326/426 Dark Matter and the Universe. Dr. Vitaly Kudryavtsev F9b, Tel.:
PHY326/426 Dark Matter and the Universe Dr. Vitaly Kudryavtsev F9b, Tel.: 0114 2224531 v.kudryavtsev@sheffield.ac.uk Indirect searches for dark matter WIMPs Dr. Vitaly Kudryavtsev Dark Matter and the Universe
More informationMeasurement of 39 Ar in Underground Argon for Dark Matter Experiments
Measurement of 39 Ar in Underground Argon for Dark Matter Experiments Jingke Xu Princeton University June 7 th, 2013 1 Evidences for Dark Matter Rotation Curve Gravitational Lensing CMB Power Spectrum
More informationDark Matter. and TPC Technologies
Dark Matter and TPC Technologies The Physics Case for WIMPs Status of the Field:event by event discrimination Elements of a roadmap Bernard Sadoulet Dept. of Physics /LBNL UC Berkeley UC Institute for
More informationThe EDELWEISS III Experiment Status
Quentin ARNAUD for the Edelweiss Collaboration The EDELWEISS III Experiment Status Les Rencontres de Moriond 2014 Cosmology Session 27/03/2014 Dark Matter Search Evidences for Dark Matter Galaxy Clusters
More informationDARK MATTER SEARCHES AT CANFRANC: ANAIS AND ROSEBUD: an update INTRODUCTION AND EXPERIMENTAL GOALS SUMMARY OF RECENT ACHIEVEMENTS AND EFFORTS
DARK MATTER SEARCHES AT CANFRANC: ANAIS AND ROSEBUD: an update María Luisa Sarsa (Universidad de Zaragoza) On behalf of ANAIS & ROSEBUD Collaborations OUTLINE ANAIS INTRODUCTION AND EXPERIMENTAL GOALS
More informationThe Direct Search for Dark Matter
picture: Thomas Tuchan The Direct Search for Dark Matter with special emphasis on the XENON project Rafael F. Lang Purdue University rafael@purdue.edu IPMU Tokyo, March 8, 2013 1 baryon fraction Dark Matter
More informationDark Matter search with bolometric detectors. PhD Student: Filippo Orio Dottorato in Fisica XXIII Ciclo Supervisor: prof.
Dark Matter search with bolometric detectors PhD Student: Filippo Orio Dottorato in Fisica XXIII Ciclo Supervisor: prof. Fernando Ferroni Seminario di Dottorato - 4 giugno 29 1 Outline Introduction to
More informationSterile Neutrinos & Neutral Current Scattering
Sterile Neutrinos & Neutral Current Scattering SNAC 2011 Virginia Tech, VA J. A. Formaggio MIT Motivation for Measurement Technique Sources and Detectors Projected Sensitivity Motivation for Measurement
More informationWIMP: direct and indirect detection Results and perspectives
WIMP: direct and indirect detection Results and perspectives G. Gerbier CEA/Saclay, DAPNIA LSM (Fréjus Lab) - Introduction for -not so- pedestrians - Summary of direct detection exp status : few focus
More informationThe Search for Dark Matter. Jim Musser
The Search for Dark Matter Jim Musser Composition of the Universe Dark Matter There is an emerging consensus that the Universe is made of of roughly 70% Dark Energy, (see Stu s talk), 25% Dark Matter,
More informationStatus of the AMoRE experiment searching for neutrinoless double beta decay of 100 Mo
Status of the AMoRE experiment searching for neutrinoless double beta decay of 100 Mo Hyon-Suk Jo Center for Underground Physics Institute for Basic Science INPC 2016 - Adelaide Convention Centre, Australia
More informationThe CUORE Detector: New Strategies
The CUORE Detector: New Strategies Chiara Brofferio on behalf of the CUORE collaboration Università di Milano Bicocca Milano Italy INFN Milano Italy The context: Recent developments in ν Physics Oscillation
More informationStatus of CUORE and Results from CUORICINO. SERGIO DI DOMIZIO UNIVERSITÀ & INFN GENOVA On behalf of the CUORE Collaboration
Status of CUORE and Results from CUORICINO SERGIO DI DOMIZIO UNIVERSITÀ & INFN GENOVA On behalf of the CUORE Collaboration 11th Seminar on Innovative Particle and Radiation Detectors Siena, 1 October 2008
More informationThe GERmanium Detector Array
The GERmanium Detector Array n n ν=v p e - e - p Outline: Exp. issues of 0νββ-decay of 76 Ge Concept of GERDA Status of the experiment Summary and conclusions Kevin Kröninger (Max-Planck-Institut für Physik,
More informationGERDA experiment A search for neutrinoless double beta decay. Roberto Santorelli (Physik-Institut der Universität Zürich)
GERDA experiment A search for neutrinoless double beta decay Roberto Santorelli (Physik-Institut der Universität Zürich) on behalf of the GERDA collaboration ÖPG/SPS/ÖGAA meeting 04/09/09 Neutrinos mixing
More informationStudies of the XENON100 Electromagnetic Background
Studies of the XENON100 Electromagnetic Background Daniel Mayani Physik-Institut University of Zurich PhD Seminar PSI, August 26-27, 2015 Searching for elusive particles The main challenge for experiments
More informationSearch for Inelastic Dark Matter with the CDMS experiment. Sebastian Arrenberg Universität Zürich Doktorierendenseminar 2010 Zürich,
Search for Inelastic Dark Matter with the CDMS experiment Sebastian Arrenberg Universität Zürich Doktorierendenseminar 2010 Zürich, 30.08.2010 The CDMS experiment - 19 Ge and 11 Si semiconductor detectors
More informationDirect Detection in the next five years: Experimental challenges and Phonon Mediated Detectors
Direct Detection in the next five years: Experimental challenges and Phonon Mediated Detectors Complementarity between Dark Matter Searches & Collider Experiments Miniworkshop before SUSY06 at Irvine -
More informationDark Matter -- Astrophysical Evidences and Terrestrial Searches
Dark Matter -- Astrophysical Evidences and Terrestrial Searches Klaus Eitel, Karlsruhe Institute of Technology, KCETA, IK KIT University of the State of Baden-Württemberg and National Large-scale Research
More informationBackground rejection techniques in Germanium 0νββ-decay experiments. ν=v
Background rejection techniques in Germanium 0νββ-decay experiments n p ν=v n eep II. Physikalisches Institut Universität Göttingen Institutsseminar des Inst. für Kern- und Teilchenphysik, Outline Neutrinos
More informationWeek 3 - Part 2 Recombination and Dark Matter. Joel Primack
Astro/Phys 224 Spring 2012 Origin and Evolution of the Universe Week 3 - Part 2 Recombination and Dark Matter Joel Primack University of California, Santa Cruz http://pdg.lbl.gov/ In addition to the textbooks
More informationDUSEL NATIONAL LAB ROLE ESSENTIAL FOR SNOLAB AND DUSEL EXPERIMENTS SLUO
Search for Dark Matter WIMPs: SuperCDMS Soudan Soudan and SNOLAB leading to GEODM at DUSEL NATIONAL LAB ROLE ESSENTIAL FOR SNOLAB AND DUSEL EXPERIMENTS SLUO - September 17, 2009 Blas Cabrera - Stanford
More informationThe CDMS-II Dark Matter Search and SuperCDMS
The CDMS-II Dark Matter Search and SuperCDMS R. W. Ogburn IV Stanford University, Stanford, CA 94305, USA For the CDMS and SuperCDMS collaborations The Cryogenic Dark Matter Search (CDMS) currently sets
More informationSearch for Weakly Interacting Massive Particles with CDMS and XENON
Search for Weakly Interacting Massive Particles with CDMS and XENON Elena Aprile 1,2, Laura Baudis 3,4, Blas Cabrera 5,6 1 Physics Department and Columbia Astrophysics Laboratory, Columbia University,
More informationPosition calibration of cryogenic dark matter detectors
Abstract Position calibration of cryogenic dark matter detectors Aliya Merali University of Florida REU Participant, Summer 2010 Advisor: Dr. Tarek Saab Preparations for a position calibration of cryogenic
More informationGERDA: The GERmanium Detector Array for the search for neutrinoless decays of 76 Ge. Allen Caldwell Max-Planck-Institut für Physik
GERDA: The GERmanium Detector Array for the search for neutrinoless decays of 76 Ge Allen Caldwell Max-Planck-Institut für Physik What we know Mass Scale NORMAL INVERTED m 12 2 known m 13 2 known Mixing
More informationDavid Reyna Belkis Cabrera-Palmer AAP2010, Japan
David Reyna Belkis Cabrera-Palmer AAP2010, Japan Sandia is a multiprogram laboratory operated by Sandia Corporation, a Lockheed Martin Company, for the United States Department of Energy s National Nuclear
More informationNEUTRON BACKGROUND STUDIES FOR THE EDELWEISS WIMP SEARCH
NEUTRON BACKGROUND STUDIES FOR THE EDELWEISS WIMP SEARCH G. CHARDIN AND G. GERBIER FOR THE EDELWEISS COLLABORATION DSM/DAPNIA/SPP, CEA/Saclay. F-91191 Gif-sur-Yvette Cedex, France E-mail: gabriel.chardin@cea.fr
More informationThe GERDA Experiment:
The GERDA Experiment: a search for neutrinoless double beta decay Max-Planck-Institute for Physics, Munich now at University of Wisconsin, Madison on behalf of the GERDA Collaboration Outline: Motivation
More informationThe COSINUS project. development of new NaI- based detectors for dark ma6er search. STATUS report Karoline Schäffner
The COSINUS project development of new NaI- based detectors for dark ma6er search STATUS report 2016 Karoline Schäffner SCATTERING SCENARIO Dark matter particles scatter off nuclei elastically coherently:
More informationRecent results from the second CDMSlite run and overview of SuperCDMS SNOLAB project
Recent results from the second CDMSlite run and overview of SuperCDMS SNOLAB project SLAC National Accelerator Laboratory/Kavli Institute for Particle Astrophysics and Cosmology, Menlo Park, CA 94025,
More informationDark Matter Search Results from the Silicon Detectors of the Cryogenic Dark Matter Search Experiment
Dark Matter Search Results from the Silicon Detectors of the Cryogenic Dark Matter Search Experiment Kevin A. McCarthy Massachusetts Institute of Technology On behalf of the SuperCDMS and CDMS Collaborations
More informationcomponents Particle Astrophysics, chapter 7
Dark matter and dark energy components Particle Astrophysics, chapter 7 Overview lecture 3 Observation of dark matter as gravitational ti effects Rotation curves galaxies, mass/light ratios in galaxies
More informationLight Dark Matter and XENON100. For the XENON100 Collaboration Rafael F. Lang Columbia University
Light Dark Matter and XENON100 For the XENON100 Collaboration Rafael F. Lang Columbia University rafael.lang@astro.columbia.edu The XENON Collaboration ~60 scientists from 12 institutions: University of
More informationcryogenic calorimeter with particle identification for double beta decay search
cryogenic calorimeter with particle identification for double beta decay search Cuore Upgrade with Particle IDentification In the middle of 2015 INFN decided to support CUPID activity to develop: CUPID-0:
More informationTHE CRYOGENIC UNDERGROUND OBSERVATORY FOR RARE EVENTS: STATUS AND PROSPECTS
THE CRYOGENIC UNDERGROUND OBSERVATORY FOR RARE EVENTS: STATUS AND PROSPECTS Eric B. Norman Dept. of Nuclear Engineering Univ. of California, Berkeley, CA U. S. A. Recent results in n physics Neutrinos
More informationSuperCDMS: Recent Results for low-mass WIMPS
SuperCDMS: Recent Results for low-mass WIMPS David G. Cerdeño Institute for Theoretical Physics Universidad Autónoma de Madrid for the SuperCDMS Collaboration Hints for low-mass WIMPs in direct detection
More informationSearch for Low Energy Events with CUORE-0 and CUORE
Search for Low Energy Events with CUORE-0 and CUORE Kyungeun E. Lim (on behalf of the CUORE collaboration) Oct. 30. 015, APS Division of Nuclear Physics meeting, Santa Fe, NM The CUORE Experiment CUORE
More informationCANDLES Experiment Current Status and Future Plan. X. Li for the CANDLES Collaboration
CANDLES Experiment Current Status and Future Plan X. Li for the CANDLES Collaboration 1 Neutrinoless Double Beta Decay (0νββ) 2νββ decay 0νββ decay (A, Z) => (A, Z+2) + 2e - process beyond Standard Model
More informationDevelopment of a New Paradigm
P599 Seminar, April 9, 2014 Development of a New Paradigm for Direct Dark Matter Detection Jason Rose / UTK (working with Dr. Kamyshkov) Dark Matter Recap Evidence: Galactic Rotation Curves Gravitational
More informationDark Matter in Particle Physics
High Energy Theory Group, Northwestern University July, 2006 Outline Framework - General Relativity and Particle Physics Observed Universe and Inference Dark Energy, (DM) DM DM Direct Detection DM at Colliders
More informationDarkSide new results and prospects
DarkSide new results and prospects Stefano Davini - INFN Genova on behalf of the DarkSide collaboration La Thuile, March 20, 2018 The DarkSide WIMP-argon program at LNGS 2011 2012 2013 2014 2015 2016 2017
More informationXMASS: a large single-phase liquid-xenon detector
XMASS: a large single-phase liquid-xenon detector Katsuki Hiraide, the university of Tokyo for the XMASS Collaboration October 3 rd, 2016 IPRD16@Siena, Italy 1 XMASS project XMASS: a multi purpose experiment
More informationStatus of the CUORE and CUORE-0 experiments at Gran Sasso
Status of the CUORE and CUORE-0 experiments at Gran Sasso S. Di Domizio INFN and University of Genova for the CUORE collaboration Weak Interactions and Neutrinos Natal, September 19 2013 Neutrinoless double
More informationSuperCDMS SNOLAB: Goals, Design, and Status. Sunil Golwala Caltech DM /02/19
SuperCDMS SNOLAB: Goals, Design, and Status Caltech DM2016 2016/02/19 SuperCDMS SNOLAB Science Goals - [ ] HV detectors: lowest masses - ( ) - - - [ ] [ / ] SuperCDMS SNOLAB/DM2016 2 SuperCDMS SNOLAB Science
More informationA multipurpose detector for low energy
A multipurpose detector for low energy neutrino physics: Teresa Marrodán Undagoitia tmarroda@ph.tum.de Institut E15 Physik-Department Technische Universität München DPG Teilchenphysik Heidelberg, 09.03.07
More informationThe Search for Dark Matter, and Xenon1TP
The Search for Dark Matter, and Xenon1TP by Jamin Rager Hillsdale College Assistant Prof. Rafael Lang Purdue University Dept. of Physics Galaxy NGC 3198 2 Galaxy NGC 3198 Rotation Curves http://bustard.phys.nd.edu/phys171/lectures/dm.html
More informationDirect dark matter search using liquid noble gases
Direct dark matter search using liquid noble gases Teresa Marrodán Undagoitia marrodan@physik.uzh.ch Physik Institut Universität Zürich Texas Symposium 2010, Heidelberg, 09.11.2010 Teresa Marrodán Undagoitia
More informationDark Matter Detection and the XENON Experiment. 1 Abstract. 2 Introduction
Dark Matter Detection and the XENON Experiment Elena Aprile Physics Department and Columbia Astrophysics Laboratory Columbia University New York, New York 10027 1 Abstract Observations on all fronts strongly
More informationStatus of the CUORE and CUORE-0 experiments at Gran Sasso
Status of the CUORE and CUORE-0 experiments at Gran Sasso S. Di Domizio INFN and University of Genova for the CUORE collaboration Les Rencontres de Physique de la Vallée d'aoste La Thuile, February 25
More informationDARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1
DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark
More informationMeasurements of liquid xenon s response to low-energy particle interactions
Measurements of liquid xenon s response to low-energy particle interactions Payam Pakarha Supervised by: Prof. L. Baudis May 5, 2013 1 / 37 Outline introduction Direct Dark Matter searches XENON experiment
More informationNeutrinoless double beta decay with CUPID-Mo
Neutrinoless double beta decay with CUPID-Mo Pia Loaiza ANDES workshop, Sao Paulo, 4-6 August 2018 Two neutrino double beta decay Certain isotopes are forbidden from decaying through standard beta decay
More informationPaolo Agnes Laboratoire APC, Université Paris 7 on behalf of the DarkSide Collaboration. Dark Matter 2016 UCLA 17th - 19th February 2016
Paolo Agnes Laboratoire APC, Université Paris 7 on behalf of the DarkSide Collaboration Dark Matter 2016 UCLA 17th - 19th February 2016 The DarkSide program 2 Double Phase Liquid Argon TPC, a staged approach:
More informationDark Matter. Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET)
Dark Matter Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET) 1 Dark Matter 1933 r. - Fritz Zwicky, COMA cluster. Rotation
More informationXI. Beyond the Standard Model
XI. Beyond the Standard Model While the Standard Model appears to be confirmed in all ways, there are some unclear points and possible extensions: Why do the observed quarks and leptons have the masses
More informationBackground simulations and shielding calculations
Background simulations and shielding calculations Vitaly A. Kudryavtsev University of Sheffield Contributions from many others Outline Note 1: results are relevant to many experiments and techniques (mainly
More informationReview of dark matter direct detection experiments
PRAMANA c Indian Academy of Sciences Vol. 79, No. 5 journal of November 2012 physics pp. 1045 1057 Review of dark matter direct detection experiments RUPAK MAHAPATRA Department of Physics and Astronomy,
More informationAMoRE 0 experiment using low temperature 40 Ca 100 MoO 4 calorimeters
AMoRE 0 experiment using low temperature 40 Ca 100 MoO 4 calorimeters Yong-Hamb Kim On behalf of AMoRE collaboration Institute for Basic Science (IBS) Korea Research Institute for Standards and Science
More informationLatest Results on Direct Detection of Dark Matter WIMPs - CDMS & SuperCDMS
Latest Results on Direct Detection of Dark Matter WIMPs - CDMS & SuperCDMS TeV 2006, Madison - August 30, 2006 Blas Cabrera Co-Spokesperson CDMS & Spokesperson SuperCDMS Summary of current status of Direct
More informationSensitivity and Backgrounds of the LUX Dark Matter Search
Sensitivity and Backgrounds of the LUX Dark Matter Search 1 LUX Goal: Direct Detection of Dark Matter WMAP 5-year data (2008) gives matter densities (Ω) based on best fit to Λ-CDM cosmological model: Ω
More informationDark Matter and Dark Energy components chapter 7
Dark Matter and Dark Energy components chapter 7 Lecture 4 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,
More informationNew results of CUORICINO on the way to CUORE
New results of CUORICINO on the way to CUORE Laboratori Nazionali del Gran Sasso of INFN On behalf of the CUORE Collaboration The CUORE experiment CUORE (Cryogenic Underground Observatory for Rare Events)
More informationProject Paper May 13, A Selection of Dark Matter Candidates
A688R Holly Sheets Project Paper May 13, 2008 A Selection of Dark Matter Candidates Dark matter was first introduced as a solution to the unexpected shape of our galactic rotation curve; instead of showing
More informationNeutrino Physics: an Introduction
Neutrino Physics: an Introduction Lecture 3: Neutrinos in astrophysics and cosmology Amol Dighe Department of Theoretical Physics Tata Institute of Fundamental Research, Mumbai SERC EHEP School 2017 NISER
More informationDark Matter - III. Workshop Freudenstadt September 30, GRK 1694: Elementarteilchenphysik bei höchster Energie und höchster Präzision
Dark Matter - III GRK 1694: Elementarteilchenphysik bei höchster Energie und höchster Präzision Workshop Freudenstadt 2015 September 30, 2015 Guido Drexlin, Institut für Experimentelle Kernphysik KIT University
More informationTowards One Tonne WIMP Direct Detectors: Have we got what it takes?
Towards One Tonne WIMP Direct Detectors: Have we got what it takes? 000922 Center for Particle Astrophysics UC Berkeley source at http://cdms.berkeley.edu/gaitskell/ Gaitskell Future Reach / Lower limit
More informationThe energy calibration system of the CUORE double beta decay bolometric experiment
The energy calibration system of the CUORE double beta decay bolometric experiment Samuele Sangiorgio on behalf of the CUORE collaboration see also, on CUORE, Thomas Bloxham in Session G14, Sunday morning
More informationLUX: A Large Underground Xenon detector. WIMP Search. Mani Tripathi, INPAC Meeting. Berkeley, May 5, 2007
LUX: A Large Underground Xenon detector WIMP Search Mani Tripathi INPAC Meeting Berkeley, New Collaboration Groups formerly in XENON10: Case Western, Brown, Livermore Natl. Lab (major fraction of the US
More information