Down-to-earth searches for cosmological dark matter
|
|
- Julia Morgan
- 5 years ago
- Views:
Transcription
1 Down-to-earth searches for cosmological dark matter Carter Hall, University of Maryland October 19, 2016
2 Astrophysical evidence for dark matter Galaxy cluster collisions Rotation curves Ω
3 380,000 years after the big bang 13.9 billion years Today Credit: Andrey Kravtsov, KICP, U. Chicago 1970 s s: Cold dark matter is needed to seed the formation of galaxy clusters 3
4 Temperature and density fluctuations are 1 part in The cosmic microwave background anisotropy imaged Planck (2014). 4
5 CMB multipole expansion - measured by Planck (2014) ~ 1 Prominent 3 rd peak indicates presence of matter which did not rebound. ~ 1/2 ~ 1/3 5
6 Neutrinos? not heavy enough generalize Weakly Interacting Massive Particle
7 The thermal hypothesis: Was the dark matter an interacting component in the very early universe? Early universe plasma Dark matter annihilation Dark matter Normal matter? Age of universe ~ 1 nanosecond; Temperature ~ 100 GeV Dark matter Dark matter creation Normal matter
8 The thermal hypothesis: Was the dark matter an interacting component in the very early universe? Small annihilation cross section Typical weak nuclear force cross sections Correct dark matter abundance Large annihilation cross section J. Feng, Annu. Rev. Astron. Astrophys :
9 The Milky Way s dark matter halo Typical orbital vel. = 230 km/sec ~ 0.1% speed of light Density: ~ 300 m proton / liter WIMPs (~100 GeV): 3 per liter debroglie wavelength: WIMPs: larger than a nucleus. Coherent scalar scattering on ordinary nuclear matter, σ ~ A 2 Production: WIMPs: thermal
10 Dark matter annihilation Dark matter Normal matter? Dark matter Normal matter Dark matter creation
11
12 HAWC projected five-year sensitivity (start 2015)
13
14
15 Direct detection Dark matter Normal matter? Dark matter Normal matter
16 Direct Detection WIMP nuclear recoil signal γ,β electron recoil background
17 The parameter space of direct detection & XENONNT
18 Nuclear recoil energy spectra A 2 dependence From: arxiv:
19 Calibration of LUX: Beta spectrum of Carbon-14 Carbon-14 beta decay Detector threshold = 1.3 kev Xenon-131 Gamma line (164 kev) 1-8 kev: x-ray region
20 Detection modes for ionizing radiation Nuclear recoils vs. electron recoils "Division of energy "Timing "Stopping power Two-phase noble liquids (PandaX, XENON, LUX) Ionization Target WIMP Cryogenic semiconductors (CDMS) Phonons/heat 100% energy slowest cryogenics Single-Phase noble liquids (XMASS, DEAP/CLEAN) Light WIMP scintillating bolometers (CRESST) 20
21
22 Typical Event in LUX S1 S2 22
23 Strong background rejection from kinematics ~ kev deposition must cross full volume without interacting again ~ MeV γ forward scattering 23
24 Simulation of self-shielding in liquid xenon Volume cut rejects most gamma backgrounds. 24
25 Particle ID: recoil discrimination in LUX Charge/Light Electron recoils (background) Charge/Light Nuclear recoils (signal) Charge/Light Difference Electron recoil rejection factor: Light 25
26 LUX assembly kg of liquid xenon 26
27 27
28 Sanford Underground Research Facility Davis Cavern 1480 m (4200 mwe) LUX Water Tank South Dakota USA 28
29 Davis SURF, March
30 Davis Campus dedication, May 30, 2012 Davis Campus water tank, home of LUX Ana Davis, widow of Ray Davis 30
31 On top of the water shield, Sept
32 LUX installed underground, Sept
33 LUX recoil bands and energy scales electron recoil band less charge recombination nuclear recoil band more charge recombination 33
34 LUX WIMP search data (2013) 1.3 kev ee events observed 85.3 days kg = 10,090 kgdays Charge Light log 10 (S2 b /S1) x,y,z corrected kevnr S1 x,y,z corrected (phe) Light 2013 initial results (Run 3): Phys.Rev.Lett. 112 (2014) re-analysis of Run 3: Phys.Rev.Lett. 116 (2016)
35 October 30, 2013
36 Calibration: external gamma sources ( 137 Cs) Calibration source guide tubes Self-shielding makes external gamma sources mostly ineffectual
37 Tritium: an ideal electron-recoil band calibration source Tritium Beta Spectrum (Q=18.6 kev, T1/2=12.3 years) 2 Counts/keV/day/ atoms WIMP search range H H C T H Electron Kinetic Energy [kev] 37
38 Injection and removal of tritium from LUX, August Fiducial S1 count <150 [Phe]. rate Fiducial for S1 Volume < 150 PE Rate τ 1 =6.0 ±0.5Hours τ 2 =6.4 ±0.1 Hours August 8, 2013 Rate (Hz) 10 2 Success /21/ Time (hours) 38
39 Tritium event locations in LUX August 2013 y (cm) x (cm) drift time (µs) radius squared (cm 2 ) 39
40 Charge vs Light from tritium in LUX at 170 V/cm 10/21/16 178,000 fiducial tritium events 40
41 Tritium combined-energy spectrum 178,000 fiducial tritium events 41
42 Light yield of liquid xenon LUX tritium (100 & 180 V/cm)
43 Nuclear-recoil calibration w/mono-energetic neutrons D + D n + 3 He E n = 2.45 MeV
44 Nuclear-recoil calibration of LUX Neutron scattering with a neutron generator
45 LUX final WIMP search results Run 3 & 4 combined, LUX Run 3 & 4 (2016): arxiv:
46 LUX -> LZ (2020) Scale up LUX fiducial mass by x40 LZ: Total Xe - 10 Ton Ac5ve Xe 7 Ton Fiducial Xe 5.6 Ton LUX LUX 46
47 The LZ Experiment coming in 2020 Xe TPC existing LUX water shield 50 kv high voltage Gd-doped liquid scintillator outer detector 47
48 LZ Sensitivity (5.6 Tonnes, 1000 live days) cm 2 48
49 History of WIMP 50 GeV Ge, NaI no discrimination Ge, w/discrim. ZEPLIN XENON100 LXe, w/discrim. LUX (2013) LUX & PandaX-II (2016) LZ XENON 1T
50
51 Uranium-238 decay chain start Thorium-232 decay chain start gamma sources end end 51
52 Ordinary radioactive decay here on earth K-40 Bi-214 (U-238) Tl-208 (Th-232) WIMP scattering ββ0ν Q values: Ge-76 Xe-136 Te
53 Two problems from particle physics 1) Why is the weak scale so light? è New weak physics? è WIMPs 2) Why no CP violation in QCD? è Peccei-Quinn symmetry?è Axions
54 Electron-recoil and nuclear-recoil calibration data 54
55 Is LUX a success?
56 July 22, 2016
Axion search with Dark Matter detector
Axion search with Dark Matter detector Paolo Beltrame Durham IPPP, 14th March 2016 1 Direct DM search Dark matter (DM) Milky Way s halo => flux on Earth ~ 10 5 cm -2 s -1 ρχ ~ 0.3 GeV/cm 3 and 100 GeV/c
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 informationLUX-ZEPLIN (LZ) Status. Attila Dobi Lawrence Berkeley National Laboratory June 10, 2015 WIN Heidelberg
LUX-ZEPLIN (LZ) Status Attila Dobi Lawrence Berkeley National Laboratory June 10, 2015 WIN-2015. Heidelberg 1 LZ = LUX + ZEPLIN 29 institutions currently About 160 people Continuing to expand internationally
More informationLARGE UNDERGROUND XENON
LARGE UNDERGROUND XENON Cláudio Silva (LIP Coimbra) On behalf of the LUX Collaboration IDPASC Dark Matter Workshop 17 December 2011 1 THE LUX COLLABORATION Collaboration was formed in 2007 and fully funded
More informationThe LZ Experiment Tom Shutt SLAC. SURF South Dakota
The LZ Experiment Tom Shutt SLAC SURF South Dakota 1 LUX - ZEPLIN 31 Institutions, ~200 people 7 ton LXe TPC ( tons LXe total) University of Alabama University at Albany SUNY Berkeley Lab (LBNL), UC Berkeley
More informationBackground Characterization and Rejection in the LZ Detector. David Malling Brown University IDM 2012 July 25, 2012
Background Characterization and Rejection in the LZ Detector David Malling Brown University IDM 2012 July 25, 2012 LZ Construction 2 Background Sources Ti cryostats 1500 kg
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 informationTWO-PHASE DETECTORS USING THE NOBLE LIQUID XENON. Henrique Araújo Imperial College London
TWO-PHASE DETECTORS USING THE NOBLE LIQUID XENON Henrique Araújo Imperial College London Oxford University 18 th October 2016 OUTLINE Two-phase xenon for (dark) radiation detection Instrumenting a liquid
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 informationDarkSide. Bianca Bottino Università di Genova and INFN Sezione di Genova on behalf of the DarkSide collaboration 1
DarkSide Bianca Bottino Università di Genova and INFN Sezione di Genova on behalf of the DarkSide collaboration 1 DARKSIDE MAIN FEATURES Dark Matter direct detection WIMP induced nuclear recoils Double
More informationCurrent status of LUX Dark Matter Experiment
Current status of LUX Dark Matter Experiment by A. Lyashenko Yale University On behalf of LUX collaboration LUX Large Underground Xenon experiment LUX Collaboration: Yale, CWRU, UC Santa Barbara, Brown,
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 informationStatus of DM Direct Detection. Ranny Budnik Weizmann Institute of Science
Status of DM Direct Detection Ranny Budnik Weizmann Institute of Science DM evidence on one slide Thermal freeze out of dark matter in the standard cosmological model Weakly Interacting Massive Particles
More informationRecent results from PandaX- II and status of PandaX-4T
Recent results from PandaX- II and status of PandaX-4T Jingkai Xia (Shanghai Jiao Tong University) On behalf of PandaX Collaboration August 2-5, Mini-Workshop@SJTU 2018/8/4 1 Outline Dark Matter direct
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 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 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 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 informationLow Energy Particles in Noble Liquids
Low Energy Particles in Noble Liquids Antonio J. Melgarejo Fernandez Columbia University Invisibles School, July 14th 2013, Durham Explaining the title I Noble gases are a group of elements found at the
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 informationPANDA-X A New Detector for Dark Matter Search. Karl Giboni Shanghai Jiao Tong University
PANDA-X A New Detector for Dark Matter Search Karl Giboni Shanghai Jiao Tong University Seminar at KEK, Tsukuba Japan 3 February, 2011 Jin Ping Laboratory Newly constructed deep underground lab In the
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 informationDo WIMPs Rule? The LUX & LZ Experiments and the Search for Cosmic Dark Matter
Do WIMPs Rule? The LUX & LZ Experiments and the Search for Cosmic Dark Matter!" Dan Akerib! SLAC National Accelerator Laboratory Kavli Insitute for Particle Astrophysics & Cosmology Standard cosmology:
More informationBackground and sensitivity predictions for XENON1T
Background and sensitivity predictions for XENON1T Marco Selvi INFN - Sezione di Bologna (on behalf of the XENON collaboration) Feb 19 th 016, UCLA Dark Matter 016 1 Outline Description of the detector;
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 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 informationLZ and Direct Dark Matter Detection
LZ and Direct Dark Matter Detection Kimberly J. Palladino February 14, 2017 What is the universe made of? Abell 2218 Reconciling what we measure on Earth with what we see in the cosmos 2 Outline Dark Matter
More informationAfter LUX: The LZ Program. David Malling, Simon Fiorucci Brown University APS DPF Conference August 10, 2011
After LUX: The LZ Program David Malling, Simon Fiorucci Brown University APS DPF Conference August 10, 2011 The LZ Program LZ LUX-ZEPLIN LUX (14 U.S. institutions) + new collaborators from ZEPLIN, other
More informationThe Neutron/WIMP Acceptance In XENON100
The Neutron/WIMP Acceptance In XENON100 Symmetries and Fundamental Interactions 01 05 September 2014 Chiemsee Fraueninsel Boris Bauermeister on behalf of the XENON collaboration Boris.Bauermeister@uni-mainz.de
More informationDirect Detection of Dark Matter with LUX
Direct Detection of Dark Matter with LUX we are a collaboration of 50+ scientists, please see http://lux.brown.edu for more information Peter Sorensen Lawrence Livermore National Laboratory DNP October
More informationDARWIN. Marc Schumann. U Freiburg PATRAS 2017 Thessaloniki, May 19,
DARWIN Marc Schumann U Freiburg PATRAS 2017 Thessaloniki, May 19, 2017 marc.schumann@physik.uni-freiburg.de www.app.uni-freiburg.de 1 Dark Matter Searches: Status spin-independent WIMP-nucleon interactions
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 informationThe XENON1T experiment
The XENON1T experiment Ranny Budnik Weizmann Institute of Science For the XENON collaboration 1 The XENON1T experiment Direct detection with xenon The XENON project XENON1T/nT 2 Quick introduction and
More informationLZ and Direct Dark Matter Detection. Kimberly J. Palladino May 1, 2018
LZ and Direct Dark Matter Detection Kimberly J. Palladino May 1, 2018 What is the universe made of? Abell 2218 Reconciling what we measure on Earth with what we see in the cosmos 2 Outline Dark Matter
More informationDARWIN. Marc Schumann. U Freiburg LAUNCH 17 Heidelberg, September 15,
DARWIN Marc Schumann U Freiburg LAUNCH 17 Heidelberg, September 15, 2017 marc.schumann@physik.uni-freiburg.de www.app.uni-freiburg.de 1 Marc Schumann U Freiburg LAUNCH 17 Heidelberg, September 15, 2017
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 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 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 detection: results from liquid noble-gas experiments
Direct detection: results from liquid noble-gas experiments Teresa Marrodán Undagoitia marrodan@mpi-hd.mpg.de DM@LHC Heidelberg, April 5th, 2018 Teresa Marrodán Undagoitia (MPIK) Liquid noble gases Heidelberg,
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 informationShedding Light on Dark Matter from Deep Underground with XENON. Kaixuan Ni (Columbia)
Shedding Light on Dark Matter from Deep Underground with XENON Kaixuan Ni (Columbia) University of Maryland, 11-25-2008 A well-known mystery for astronomers Fritz Zwicky, The Astrophysical Journal, 85
More informationDARWIN: dark matter WIMP search with noble liquids
DARWIN: dark matter WIMP search with noble liquids Physik Institut, University of Zurich E-mail: laura.baudis@physik.uzh.ch DARWIN (DARk matter WImp search with Noble liquids) is an R&D and design study
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 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 informationDirect dark matter search using liquid noble gases
Universität Zürich E-mail: marrodan@physik.uzh.ch Liquid noble gases have proven a great potential as detector medium for dark matter searches. Particles interacting in these media produce ionized and
More informationWhither WIMP Dark Matter Search? Pijushpani Bhattacharjee AstroParticle Physics & Cosmology Division Saha Institute of Nuclear Physics Kolkata
Whither WIMP Dark Matter Search? AstroParticle Physics & Cosmology Division Saha Institute of Nuclear Physics Kolkata 1/51 2/51 Planck 2015 Parameters of the Universe 3/51 Discovery of Dark Matter Fritz
More informationRecent Results from the PandaX Experiment
Recent Results from the PandaX Experiment Changbo Fu Shanghai Jiao Tong University On Behalf of Collaboration 25May2017 1 Outline 1. Introduciton Dark Matter: WIMPs, Axion, PandaX at China Jinping Underground
More informationDirect Detection of Dark Matter. Lauren Hsu Fermilab Center for Particle Astrophysics TRISEP Summer School, June 10, 2014
Direct Detection of Dark Matter Lauren Hsu Fermilab Center for Particle Astrophysics TRISEP Summer School, June 10, 2014 Direct Detection of Dark Matter Lecture 1 How to detect dark matter Lecture 2 Review
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 informationBackground Modeling and Materials Screening for the LUX and LZ Detectors. David Malling Brown University LUX Collaboration AARM Meeting February 2011
Background Modeling and Materials Screening for the LUX and LZ Detectors David Malling Brown University LUX Collaboration AARM Meeting February 2011 1 Summary LUX screening program limits background contributions
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 informationNeutrino and Dark Matter Detections via Atomic Ionizations at sub-kev Sensitivities
Neutrino and Dark Matter Detections via Atomic Ionizations at sub-kev Sensitivities Chih-Pan Wu Dept. of Physics, National Taiwan University Collaborators: Jiunn-Wei Chen, Chih-Liang Wu (NTU) Chen-Pang
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 informationDARK MATTER SEARCH AT BOULBY MINE
DARK MATTER SEARCH AT BOULBY MINE R. LUSCHER on behalf of the Boulby Dark Matter Collaboration (RAL, Imperial College, Sheffield, UCLA, Texas A&M, Pisa, ITEP, Coimbra, Temple and Occidental) Rutherford
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 informationThe next generation dark matter hunter: XENON1T status and perspective
The next generation dark matter hunter: XENON1T status and perspective A. Rizzo a on behalf of the XENON Collaboration Department of Astrophysics, Columbia University in the City of New York, USA Abstract.
More informationCryogenic 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 informationDirect dark matter search with XMASS. K. Abe for the XMASS collaboration
Direct dark matter search with XMASS K. Abe for the XMASS collaboration Outline XMASS experiment. Single phase liquid xenon detector Many targets were searched with XMASS. WIMP search fiducialized volume.
More informationXMASS 1.5, the next step of the XMASS experiment
1,2 for the XMASS collaboration 1 Kamioka Observatory, Institute for Cosmic Ray Research, the University of Tokyo, Higashi-Mozumi, Kamioka, Hida, Gifu 506-1205, Japan, 2 Kavli Institute for Physics and
More informationNeutrinos. Why measure them? Why are they difficult to observe?
Outline What is a neutrino? Why do we want to study them? Building a detector to detect the undetectable What does a neutrino detector see? How do you seperate a neutrino signal from the background? Neutrinos
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 informationMeasuring Dark Matter Properties with High-Energy Colliders
Measuring Dark Matter Properties with High-Energy Colliders The Dark Matter Problem The energy density of the universe is mostly unidentified Baryons: 5% Dark Matter: 20% Dark Energy: 75% The dark matter
More informationSolar and atmospheric neutrinos as background for direct dark matter searches
Solar and atmospheric neutrinos as background for direct dark matter searches Achim Gütlein TU-München Joined seminar on neutrinos and dark matter.0.0 utline Direct Dark Matter Search eutrinos as background
More informationPoS(EPS-HEP2017)074. Darkside Status and Prospects. Charles Jeff Martoff Temple University
Temple University E-mail: cmartoff@gmail.com The DarkSide Dark Matter Search Program is a direct-detection search for dark matter using a Liquid Argon Time Projection Chamber. The detector is designed
More information=> Ωmatter >> Ωbaryon
Cryogenic Detectors Direct Search Cryogenic Detectors CRESST Project Cosmic Microwave Background Matter-Density Ωmatter Anisotropy: Angular scale => geometry, Ωtot Wilkinson Microwave Anisotropy Probe
More informationCMB constraints on dark matter annihilation
CMB constraints on dark matter annihilation Tracy Slatyer, Harvard University NEPPSR 12 August 2009 arxiv:0906.1197 with Nikhil Padmanabhan & Douglas Finkbeiner Dark matter!standard cosmological model:
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 informationFURTHER COSMOLOGY Book page T H E M A K E U P O F T H E U N I V E R S E
FURTHER COSMOLOGY Book page 675-683 T H E M A K E U P O F T H E U N I V E R S E COSMOLOGICAL PRINCIPLE Is the Universe isotropic or homogeneous? There is no place in the Universe that would be considered
More informationThe LUX Dark Matter Search Objectives and Status
Northeastern University 2009-06-06 The LUX Dark Matter Search Objectives and Status www.luxdarkmatter.org The Large Underground Xenon (LUX) dark matter search experiment is currently being deployed at
More informationNuclear Recoil Scintillation and Ionization Yields in Liquid Xenon
Nuclear Recoil Scintillation and Ionization Yields in Liquid Xenon Dan McKinsey Yale University Physics Department February, 011 Indirect and Direct Detection of Dark Matter Aspen Center of Physics Energy
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 informationDarkSide-20k and the Darkside Program for Dark Matter Searches
DarkSide-20k and the Darkside Program for Dark Matter Searches Cristiano Galbiati Princeton University APC Paris Diderot GDR Neutrinos LPSC Grenoble June 6, 2016 DarkSide-20k Institutions [cm 2 ] σ 41
More informationXENONNT AND BEYOND. Hardy Simgen. WIN 2015 MPIK Heidelberg. Max-Planck-Institut für Kernphysik Heidelberg
XENONNT AND BEYOND Hardy Simgen Max-Planck-Institut für Kernphysik Heidelberg WIN 2015 MPIK Heidelberg THE XENON PROGRAM FOR DIRECT DARK MATTER SEARCH 1 THE PRESENT: XENON1T! LXe TPC under construction
More informationDirect Dark Matter Searches. General Overview LUX-ZEPLIN Hans Kraus, Oxford
Direct Dark Matter Searches General Overview LUX-ZEPLIN Hans Kraus, Oxford How to detect dark matter 1. Direct detection (scattering XS) Nuclear (atomic) recoils from elastic scattering A- & J-dependence,
More informationSearching for Dark Matter From XENON10 to LUX. Luiz de Viveiros
FCT - Universidade de Coimbra - Café com Física Searching for Dark Matter From XENON10 to LUX Luiz de Viveiros Brown University Physics Department De Viveiros - Brown University April 2009 v07 Summary
More informationThreshold optimization and Bayesian inference on the XENON1T experiment
M.Sc. Physics and Astronomy Gravitation, Astro-, and Particle Physics Master Thesis Threshold optimization and Bayesian inference on the XENON1T experiment by Arjen Wildeboer 10269045 August 2017 60 ECTS
More informationSearch for double electron capture on 124 Xe with the XMASS-I detector
Search for double electron capture on 124 Xe with the XMASS-I detector KATSUKI HIRAIDE (ICRR, THE UNIVERSITY OF TOKYO) SEPTEMBER 7 TH, 2015 TAUP2015 1 124 Xe 2n double electron capture Natural xenon contains
More informationDarkside-50, DarkSide-20k and the Global Collaboration to reach the Neutrino Floor with liquid argon
Darkside-5, DarkSide-2k and the Global Collaboration to reach the Neutrino Floor with liquid argon Cristiano Galbiati Gran Sasso Science Institute and Princeton University The quest for dark matter with
More informationNew Physics Results from DarkSide-50. Masayuki Wada Princeton University on behalf of the DarkSide-50 Collaboration Feb
New Physics Results from DarkSide5 Masayuki Wada Princeton University on behalf of the DarkSide5 Collaboration Feb. 8 Lake Louise Winter Institute 8 DETECTOR DARKSIDE 5 Radonfree (Rn levels < 5 mbq/m )
More informationAxion and axion-like particle searches in LUX and LZ. Maria Francesca Marzioni
Axion and axion-like particle searches in LUX and LZ Maria Francesca Marzioni PPE All Group meeting 06/06/2016 Outline Why are we interested in axions How can we detect axions with a xenon TPC Axion signal
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 informationThe XENON Project. M. Selvi The XENON project
The XENON Project M. Selvi Assemblea di Sezione 2011 Dark matter in the Universe Dark matter properties: what we know Direct WIMP search Direct WIMP search Direct WIMP detection Why Xenon? A double-phase
More informationDark Matter Search at Boulby Mine I. Liubarskyy 1, T. Aliz, G. J. Alnerx, B. Ahmedz, G. T. J. Arnisonx, J. C. Bartoní, A. Bewickz, D. Davidgez, G. J.
Dark Matter Search at Boulby Mine I. Liubarskyy 1, T. Aliz, G. J. Alnerx, B. Ahmedz, G. T. J. Arnisonx, J. C. Bartoní, A. Bewickz, D. Davidgez, G. J. Daviesy, G. J. Homerx, A. S. Howardz, W. G. Jonesy,
More informationUCLA Dark Matter 2014 Symposium. Origins and Distributions of the Backgrounds. 15 min
S. Fiorucci Brown University UCLA Dark Matter 2014 Symposium Origins and Distributions of the Backgrounds 15 min What is a signal for LUX? Nuclear recoil Single scatter Signal Low energy, typically < 25
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 informationIntroduction to Class and Dark Matter
Introduction to Class and Dark Matter Prof. Luke A. Corwin PHYS 792 South Dakota School of Mines & Technology Jan. 14, 2014 (W1-1) L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 1 / 22
More informationXENON100. Marc Schumann. Physik Institut, Universität Zürich. IDM 2010, Montpellier, July 26 th,
XENON100 Marc Schumann Physik Institut, Universität Zürich IDM 2010, Montpellier, July 26 th, 2010 www.physik.uzh.ch/groups/groupbaudis/xenon/ Why WIMP search with Xenon? efficient, fast scintillator (178nm)
More informationDark Matter, Low-Background Physics
Dark Matter, Low-Background Physics RHUL Jocelyn Monroe Nov. 6, 2012 1. Evidence (Astrophysical Detection) 2. Candidates, Properties 3. Direct Detection (Particle Physics) 1 st Observation: 1930s Fritz
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 informationBackground Studies for the XENON100 Experiment. Alexander Kish Physics Institute, University of Zürich Doktorandenseminar August 30, 2010 UZH
Background Studies for the XENON100 Experiment Alexander Kish Physics Institute, University of Zürich Doktorandenseminar August 30, 2010 UZH The XENON dark matter search program Target Volume 62 kg Total
More informationBubXe: a liquid xenon bubble chamber for Dark Matter detection!
BubXe: a liquid xenon bubble chamber for Dark Matter detection Jeremy Mock, on behalf of Cecilia Levy and Matthew Szydagis SUNY Albany Direct DM Search Today 3 detection channels (light, charge, heat):
More informationarxiv:astro-ph/ v1 15 Feb 2005
The XENON Dark Matter Experiment Elena Aprile (on behalf of the XENON collaboration) Physics Department and Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027 age@astro.columbia.edu
More informationNeutrino coherent scattering in Liquid Xenon
Neutrino coherent scattering in Liquid Xenon 1 Quasi-free electron emission from nonpolar dielectrics p z e 0 V(z) z V(z) (b) e e V o V 1 z 0 dn /dp e z V o V ( z) = V 1 0 V ( z) = ef ef z 1 z + ea + ea,
More informationNucleosíntesis primordial
Tema 5 Nucleosíntesis primordial Asignatura de Física Nuclear Curso académico 2009/2010 Universidad de Santiago de Compostela Big Bang cosmology 1.1 The Universe today The present state of the Universe
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 informationDirect Dark Matter Searches
Direct Dark Matter Searches Marc Schumann Physik Institut, Universität Zürich What is? Invisibles12, GGI Florence, June 27th 2012 marc.schumann@physik.uzh.ch www.physik.uzh.ch/groups/groupbaudis/xenon/
More informationDarkside and the future Liquid Argon Dark Matter program
Darkside and the future Liquid Argon Dark Matter program Giuliana Fiorillo Università di Napoli Federico II & INFN Napoli PM2018-14th Pisa Meeting on Advanced Detectors DM direct detection WIMP χ Low mass
More informationRecent Discoveries in Neutrino Physics
Recent Discoveries in Neutrino Physics Experiments with Reactor Antineutrinos Karsten Heeger http://neutrino.physics.wisc.edu/ Karsten Heeger, Univ. of Wisconsin NUSS, July 13, 2009 Standard Model and
More informationRecent results and status of the XENON program
on behalf of the XENON Collaboration Subatech, Ecole des Mines de Nantes, CNRS/In2p3, Université de Nantes, Nantes, France E-mail: julien.masbou@subatech.in2p3.fr The XENON program aims at the direct detection
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 11 Nov. 13, 2015 Today Cosmic Microwave Background Big Bang Nucleosynthesis Assignments This week: read Hawley and Holcomb,
More information