XMASS Projects. Hiroyuki Sekiya. ICRR & Kavli-IPMU, University of Tokyo. for the XMASS Collaboration
|
|
|
- Harvey Harvey
- 5 years ago
- Views:
Transcription
1 XMASS Projects Hiroyuki Sekiya ICRR & Kavli-IPMU, University of Tokyo for the XMASS Collaboration Aug st International Conference on Supersymmetry and Unification of Fundamental Interactions (SUSY2013)
2 Introduction Recent physics results From 2012 commissioning run Light WIMP search Phys. Lett. B719 (2013) 78 Solar axion search Phys. Lett. B724 (2013) 46 Current status Detector refurbishment Future prospects XMASS-1.5 Contents SUSY2013 8/29/2013 H. Sekiya 2
3 XMASS Projects Multipurpose low BG experiment with single phase (liquid) Xe Xenon MASSive detector for Solar neutrino (pp/ 7 Be) Xenon neutrino MASS detector (double beta decay) Xenon detector for Weakly Interacting MASSive Particles(DM) neutrinos, axions dark matters, neutrinos The ultimate XMASS Y. Suzuki, hep-ph/ Xe 24t (10t fiducial) Ø 2.5m SUSY2013 8/29/2013 H. Sekiya 3
4 XMASS-1 835kg LXe detector for Dark Matter search 80cm SUSY2013 8/29/2013 H. Sekiya 4
5 Why Single Phase Xe? Simple and Clean for Large Scalability Simplicity Single phase LXe scintillator Simple structure like Super-K Cleanliness Made of pure materials Development of low BG PMTs Xe purification technologies distillation system Xe has the advantage for Spin Independent interacting WIMPs Counts/day/kg/keV Expected WIMP spectrum SUSY2013 8/29/2013 H. Sekiya 5
6 Kamioka Observatory Located underground in Mozumi zinc mine at a 2700 m.w.e. depth. 2km horizontal access by cars Kamioka Tokyo Kyoto Mt. Ikenoyama (1369m) Surface Lab. 1000m Entrance 1800m Underground Lab.s TPC Paris /19/2012 H. Sekiya 6
7 XMASS-1 Detector 10m x φ10m water shield for external BG 1050 kg Liquid Xe within the chamber. Largest mass among DM detectors 642 hexagonal PMTs on 80cm pentakisdodecahedron Construction was completed in Oct 2010 SUSY2013 8/29/2013 H. Sekiya 7
8 Inside of the pentakisdodecahedron Photo coverage is 62.4% SUSY2013 8/29/2013 H. Sekiya 8
![25% 25% 27-39% RI: w/ PMT base U [mbq/pmt] 50 18±2 0.70±0.](/docs-images/86/93322554/images/9-3.jpg "28 Th [mbq/pmt] 13 6.9±1.3 1.51±0.")
![31 40 K [mbq/pmt] 610 140±20 9.10±2.15 60 Co [mbq/pmt] <1.](/docs-images/86/93322554/images/9-4.jpg "8 5.5±0.9 2.92±1.61 Clean PMT Base has also been developed.")
9 Clean PMT XMASS PMT HISTORY YEAR Model Prototype R8778 R10789 Material:Body glass Kovar Kovar QE 25% 25% 27-39% RI: w/ PMT base U [mbq/pmt] 50 18±2 0.70±0.28 Th [mbq/pmt] ± ± K [mbq/pmt] ± ± Co [mbq/pmt] < ± ±1.61 Clean PMT Base has also been developed. SUSY2013 8/29/2013 H. Sekiya 9
10 Xe Distillation System Commercial pure Xe contains ~0.1ppm Kr 85 K / K = τ =10.8 year, Q β = 687keV 5 order reduction was indispensable. Astoparticle Physics 31, (2009) 290 Xe Kr Boiling point (@0.2MPa) 178K 140K~150K 4m We established Xe purifiaction by distillation 1 ton LXe = 170 m 3 gas Xe Process speed: 4.7kg/hr 10 days Confirmed Kr < 2.7ppt by API-MS SUSY2013 8/29/2013 H. Sekiya 10
11 Detector Response Top PMT manipulator real data 57 Co simulation Calibration spectrum 59.3keV of W 122keV ~4% rms 136keV Reconstructed vertex real data simulation total photoelectrons Trigger efficiency energy kevee SUSY2013 8/29/2013 Highest LXe scintillation yields: 14.7p.e./keVee Lowest threshold: 4hits 0.3keVee H. Sekiya 11
12 Unexpected BG BG is 2 order higher than that had been expected. counts/day/p.e. Data BG simulation 238U & 210Pb of PMT Al seal expected BG (PMT & components) ~1MeV(60Co peak) total photoelectrons GORE-TEX? ~5keV SUSY2013 8/29/2013 Major origin of BG was considered to be γ from PMTs, but the observed data seemed to have additional surface contamination. Aluminum sealing parts for the PMT (btw metal body and quartz glass) contains 238U and 210Pb (>5keV) GORE-TEX between PMT and holder is suspicious below 5keV. H. Sekiya 12
13 XMASS Full Volume: Low BG w/o PID Although extra BG sources were found, XMASS BG level is still competitive w/o rejecting electronic events. XMASS has a competitive sensitivity to Light WIMPs & Axions Evens/kg/day/keV XMASS full volume kg days Fiducial volume analyses are on-going and will be released. E. Aprile, 2010 Princeton SUSY2013 8/29/2013 H. Sekiya 13
14 Phys. Lett. B719 (2013) 78 Light WIMPs Set an upper limit on the WIMP-nucleon cross section for WIMPs with masses below 20GeV w/o PID and excludes part of the parameter space allowed by DAMA PRL 109, (2012) /kg/kevee/day data σ WIMP-n cm CoGeNT DAMA 5σ 90%CL XMASS Band:Q.F uncertainty CDMS 1 7GeV 12GeV 18GeV [kevee] 2 SUSY2013 8/29/ WIMP mass [GeV/c 2 ] H. Sekiya 14
15 Solar Axions JETP Lett., 95, 379 (2012) A. V. Derbin et al., arxiv: XMASS has also sensitivity to solar axions that would be produced by Bremsstrahlung and Compton effects (g aee ) in the Sun through the axio-electric effect in Xe N.B. Not g aγγ through Primakoff effect Expected flux g aee = SUSY2013 8/29/2013 H. Sekiya 15
16 Phys. Lett. B724 (2013) 46 Solar Axions Same data set as Light WIMP search No indication of signals. Bound in gaee vs. mass. Better than any other constraint in 10-40keV. Better than any other experimental constraint Data Signal MC SUSY2013 8/29/2013 H. Sekiya 16
17 Countermeasures XMASS-1 Refurbishment for Background reduction PMT+Cu surface cleanup Remove GORE-TEX Cover PMT Aluminum seal Cu ring around aluminum seal Electropolished Cu cover above Cu rings SUSY2013 8/29/2013 H. Sekiya 17
18 After Cu ring attachment SUSY2013 8/29/2013 H. Sekiya 18
19 After thin Cu plate attachment SUSY2013 8/29/2013 H. Sekiya 19
20 Almost finished Will resume data taking in this autumn. SUSY2013 8/29/2013 H. Sekiya 20
21 Next step: XMASS-1.5 Inner Ø: 1.5 m contains 5 tons of LXe fiducial mass 1 ton Lessons from XMASS-1 Still Dark matter detector New PMT Flat photocathode cannot catch Plano-concave photocathode can catch SUSY2013 8/29/2013 H. Sekiya 21
22 XMASS-1.5 Actively being developed w/ Hamamatsu Effectiveness is verified by MC SUSY2013 8/29/2013 H. Sekiya 22
23 XMASS projects and timeline XMASS-1-RFB XMASS-1.5 x10 x10 XMASS-2 The ultimatum H. Sekiya 23
24 Conclusion XMASS-1 obtained light WIMP and solar axion result by using 835kg of LXe with very low threshold (0.3keVee) Phys. Lett B 719(2013)78, Phys. Lett B 724 (2013) 46 Initial contamination problems are understood and being addressed. The refurbishment of XMASS-1 is on-going and data taking will resume soon. XMASS-1.5 is planned and the projects move on. SUSY2013 8/29/2013 H. Sekiya 24
25 Extra slides SUSY2013 8/29/2013 H. Sekiya 25
26 Kamioka Observatory, ICRR, Univ. of Tokyo: Y. Suzuki (Spokesperson), M. Nakahata, S. Moriyama, M. Yamashita, Y. Kishimoto, A. Takeda, K. Abe, H. Sekiya, H. Ogawa, K. Kobayashi, K. Hiraide, B. Yang, A. Shinozaki, k. Hieda, O. Takachio, D. Umemoto, N. Oka, K. Nakagawa Kavli-IPMU, University of Tokyo: K. Martens, J.Liu Tokai University: K. Nishijima,F. Kusaba Gifu University: S. Tasaka XMASS Collaboration Yokohama National University: S. Nakamura,I. Murayama,K. Fujii Miyagi University of Education: Y. Fukuda STEL, Nagoya University: Y. Itow, K. Masuda, H. Uchida, Y. Nishitani, H. Takiya Kobe University: Y. Takeuchi, K. Miuchi, O. Yosuke, K. Hosokawa, A. Murata Sejong University: Y.D. Kim, N.Y.Kim Korea Research Institute of Standards and Science (KRISS): Y. H. Kim, M. K. Lee, K. B. Lee, J. S. Lee 42 researchers form 10 institutes SUSY2013 8/29/2013 H. Sekiya 26
27 Pure components More than 250 components RIs of all the components were measured with HPGe and low RI materials were selected. PMT(R10789) 3 HPGe detectors in Kamioka C1020(OFHC) RI: /one PMT Sum of other components RI: Compared w/ SUS304 screws 642 PMTs U 0.70±0.28 mbq Th 1.51±0.31 mbq 40K 9.10±2.15 mbq 60Co 2.92±1.61 mbq SUSY2013 8/29/2013 LEDs H. Sekiya U Th 40K 60Co <35% <35% <20% <20% 27
28 Dark Matter Axion DAMA signal can be explained by electromagnetic interactions of non-relativistic Axions and NaI. [J. Collar, arxiv: ] XMASS has sensitivity to dark matter Axion through Axio-electric effect. g aee /kg/kev/day data g aee Limits on g aee 90%CL XMASS DAMA allowed CoGeNT 2011 CDMS 2009 m a =3keV [kevee] H. Sekiya 28
29 Rn H. Sekiya 29
30 Quenching Factor/Leff uncertainty H. Sekiya 30
31 Energy scale calibration 31
32 Self-shielding for detector material BG High density Xe itself is the shield for γ,n from PMT/OFHC/ 20cm Xe is used for shields Fiducail Volume is 100kg Thicker shield makes lower BG region in center H. Sekiya 32
33 Ex.) Most dirty component : PMT 238 U Chain 1.8mBq/PMT 5cm Original expectation 10cm 20cm Full MC, assuming abs. 100cm, scat. 30cm for photon tracking Counts/day/kg/keV 20cm Xe is used for shield Fiducail Volume is 100kg (Full Volume is 857kg) kev gammas < 10-5 counts/day/kg/kev neutrons < 10-6 counts/day/kg/kev H. Sekiya 33
34 Cable line Calibration line Xe circulation system Gas circulation 30L/min filters gas pump 4 x 180W refrigerator PTR developed by KEK emergency gas pump 100L/min Water tank 800kg 1050kg Condenser 360W evaporator filters 10 m 3 x 2 Outer vacuum liquid pump Liquid circulation 5L/min 700L Liq. Storage gas storage H. Sekiya 34
35 Lab-C Xe Circulation system Water tank LXe tank Distillation Tower Gas Xe tank H. Sekiya 35
36 Water shields for external BG Active for µ, passive for γ,n 10m Ex.) Fast n mine: ( ) x10-5 /cm 2 /sec Assuming all neutron s energies are 10 MeV very conservatively 10 7 n generated 10m y [cm] with 70 PMTs (20 inch) to detect Cerenkov light Water purification system keeps Rn < 1mBq/m 3 water Liq. Xe < 10-4 count/day/kg X [cm] 5m tank is enough large to shield n and γ H. Sekiya 36
37 U chain Th chain GLA2010 3/29/2010 H. Sekiya 37
![intensity [Hz] diameter [mm] (1) Fe-55 5.9 350 1.](/docs-images/86/93322554/images/38-4.jpg "42 (2) Cd-109 22, 25, 88 800 1.42 (3) Am-241 59.5 485 0.")
38 Calibration source rod Calibration System source+holder (Exchangeble) adopter (SUS304) OFHC (C1020) rod Source list Isotopes Energy [kev] intensity [Hz] diameter [mm] (1) Fe (2) Cd , 25, (3) Am (4) Co H. Sekiya 38
The XMASS 800kg Dark Matter Detector in Kamioka, Japan
The XMASS 800kg Dark Matter Detector in Kamioka, Japan Kai Martens Kavli-IPMU (WPI) The University of Tokyo for the XMASS collaboration The XMASS collaboration: Kamioka Observatory, ICRR, Univ. of Tokyo
The XMASS Experiment. Jing LIU Kavli IPMU, Univ. of Tokyo PPC2013, Jul Deadwood, SD, USA
The XMASS Experiment Jing LIU Kavli IPMU, Univ. of Tokyo PPC2013, Jul. 8-13 Deadwood, SD, USA XMASS collaboration: Kamioka Observatory, ICRR, Univ. of Tokyo: K. Abe, K. Hieda, K. Hiraide, Y. Kishimoto,
XMASS 1.5: The Next Step in Kamioka, Japan
XMASS 15: The Next Step in Kamioka, Japan Benda Xu on behalf of XMASS collaboration XIV International Conference on Topics in Astroparticle and Underground Physics Torino, Italy September 10, 2015 Benda
XMASS. Masaki Yamashita. Kamioka observatory, ICRR, Univ. Of Tokyo On behalf of XMASS collaboration
XMASS Kamioka observatory, ICRR, Univ. Of Tokyo On behalf of XMASS collaboration 6th Patras Workshop on Axions, WIMPs, WISPs 5-9/July/2010 Zurich University Outline Kamioka Observatory XMASS 800 kg liquid
Quest for Dark Matter by direct detection experiments with noble liquids
Quest for Dark Matter by direct detection experiments with noble liquids Hiroyuki Sekiya ICRR & Kavli-IPMU, University of Tokyo from XMASS collaboration Dec. 12 2013 KMI International Symposium 2013(KMI2013)
Direct 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.
Shigetaka MORIYAMA Kamioka Observatory, Institute for Cosmic Ray Research, The University of Tokyo 21 st Oct Korea-Japan Joint Session
1. Introduction 2. Direct detection experiments in Japan 1. NEWAGE (Kyoto University) 2. NIT (Nagoya University) 3. PICO-LON (The University of Tokushima) 4. CARRACK (Kyoto University) 5. XMASS (The University
Direct Dark Matter Search with XMASS --- modulation analysis ---
Direct Dark Matter Search with XMASS --- modulation analysis --- ICRR, University of Tokyo K. Kobayashi On behalf of the XMASS collaboration September 8 th, 2015 TAUP 2015, Torino, Italy XMASS experiment
XMASS at Kamioka Large Scale Cryogenic detector in the underground laboratory
XMASS at Kamioka Large Scale Cryogenic detector in the underground laboratory Kamioka observatory, ICRR, Univ. Of Tokyo at LNGS, Italy Outline Kamioka Observatory XMASS 800 kg liquid xenon detector Experimental
XMASS. 12/07/25 Y. in Chicago 1
XMASS Y. Suzuki Kamioka Observatory, Ins;tute for Cosmic Ray Research ICRR), University of Tokyo And Kamioka Satellite, Kavli Ins;tute for the Physics and Mathema;cs of the Universe (IPMU), University
XMASS 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
The XMASS Experiment to search for Dark Matter at the Kamioka Observatory. Status and Previous Results
The XMASS Experiment to search for Dark Matter at the Kamioka Observatory Status and Previous Results Kai Martens Kavli IPMU The University of Tokyo Outline - Kavli IPMU: a word about my institute - Dark
XMASS: 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
The XMASS Experiment to search for Dark Matter at the Kamioka Observatory. Status and Results. Kai Martens Kavli IPMU The University of Tokyo
The XMASS Experiment to search for Dark Matter at the Kamioka Observatory Status and Results Kai Martens Kavli IPMU The University of Tokyo Outline - Kavli IPMU: introducing the institute - Dark Matter:
The XMASS Dark Matter Experiment in Kamioka, Japan: Status and Results. Kai Martens Kavli IPMU The University of Tokyo
The XMASS Dark Matter Experiment in Kamioka, Japan: Status and Results Kai Martens Kavli IPMU The University of Tokyo Outline - Kavli IPMU: introducing the institute - Dark Matter: setting the stage -
The XMASS experiment. Y. Kishimoto for the XMASS collaboration March 24 th, 2014 Recontres de Moriond, Cosmology
The XMASS experiment Y. Kishimoto for the XMASS collaboration March 24 th, 2014 Recontres de Moriond, Cosmology Contents Introduction to the XMASS Results from XMASS commissioning run Light mass WIMPs
Search 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
Distillation purification and radon assay of liquid xenon
Distillation purification and radon assay of liquid xenon Yasuo Takeuchi Kamioka Observatory, ICRR, Univ. of Tokyo, Kamioka-cho, Hida-shi, Gifu 56-125, Japan Abstract. We succeeded to reduce the Kr contamination
Rn assay and distillation purification
Rn assay and distillation purification of Lq. Xe for Kr Introduction Distillation purification of Xe for Kr Kr assay with API-MS detector Rn assay with XMASS prototype detector Summary Yasuo Takeuchi (Kamioka
The 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
The 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
Nuclear Instruments and Methods in Physics Research A
Nuclear Instruments and Methods in Physics Research A 716 (2013) 78 85 Contents lists available at SciVerse ScienceDirect Nuclear Instruments and Methods in Physics Research A journal homepage: www.elsevier.com/locate/nima
Background study for solar neutrino measurement in Super Kamiokande
Background study for solar neutrino measurement in Super Kamiokande 2 nd Topical Workshop in Low Radioactivity Techniques 3 rd Oct. 2006 Aussis, France Hiroyuki Sekiya ICRR, The University of Tokyo Outline
arxiv: v1 [astro-ph.co] 19 Aug 2018
![arxiv: v1 [astro-ph.co] 19 Aug 2018](/thumbs/83/88766359.jpg "arxiv: v1 [astro-ph.co] 19 Aug 2018")
Search for sub-gev dark matter by annual modulation using XMASS-I detector M. Kobayashi a, K. Abe a,d, K. Hiraide a,d, K. Ichimura a,d, Y. Kishimoto a,d, K. Kobayashi a,d, S. Moriyama a,d, M. Nakahata
Search for solar axions in XMASS, a large liquid-xenon detector arxiv: v3 [astro-ph.co] 29 May 2013
![Search for solar axions in XMASS, a large liquid-xenon detector arxiv: v3 [astro-ph.co] 29 May 2013](/thumbs/88/115961236.jpg "Search for solar axions in XMASS, a large liquid-xenon detector arxiv: v3 [astro-ph.co] 29 May 2013")
Search for solar axions in XMASS, a large liquid-xenon detector arxiv:22.653v3 [astro-ph.co] 29 May 23 K. Abe a,c, K. Hieda a, K. Hiraide a,c, S. Hirano a, Y. Kishimoto a,c, K. Kobayashi a,c, S. Moriyama
XENON100. 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)
XENONNT 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
The 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.
XMASS/NEWAGE Dark Matter Search
XMASS/NEWAGE Dark Matter Search Kentaro Miuchi Particle Physics Group Department of Physics, Kobe University June 30 th, 2016 Kick Off Symposium for Honolulu Office of Kobe University 1 Dark Matter Group
Dark Matter Search * in China
Dark Matter Search * in China Jianglai Liu 刘江来 Shanghai Jiao Tong University Member of the PandaX collaboration * Disclaimer: focused on direct detection The 7th Workshop on Hadron Physics in China and
Studies 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
DARWIN. 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
Light 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
Current 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,
Recent 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
DARWIN. 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
After 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
Status of KIMS-NaI experiment
Status of KIMS-NaI experiment Hyun Su Lee Institute for Basic Science, Korea On behalf of the KIMS Collaboration XIV International Conference on Topics in Astroparticle and Underground Physics KIMS-NaI
Dark 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
Background 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
A 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
The XENON100 Dark Matter Experiment at LNGS: Status and Sensitivity
The XENON100 Dark Matter Experiment at LNGS: Status and Sensitivity Elena Aprile (on behalf of the XENON Collaboration) Columbia University,Physics Department, New York,NY, USA E-mail: age@astro.columbia.edu
Background 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;
The XENON Dark Matter Project: Status of the XENON100 Phase. Elena Aprile Columbia University
The XENON Dark Matter Project: Status of the XENON100 Phase Elena Aprile Columbia University 8th UCLA Symposium Marina del Rey, Feb 22, 2008 The XENON Dark Matter Phased Program Detect WIMPS through their
The 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
Quest for dark matter by direct detection experiments with noble liquids
Quest for dark matter by direct detection experiments with noble liquids ICRR and Kavli IPMU, The University of Tokyo E-mail: sekiya@icrr.u-tokyo.ac.jp Recently so many dark matter direct search expriments
arxiv: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
Background 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
Direct 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
LUX-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
CANDLES 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
Backgrounds and Sensitivity Expectations for XENON100
Backgrounds and Sensitivity Expectations for XENON100 IDM08, Stockholm, August 19, 2008 Laura Baudis University of Zurich For the XENON100 Collaboration LNGS collaboration meeting, Oct. 2007 1 ??? The
UCLA 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
can be read by PMTs w/o wave length shifter
Liquid-Xe Solar pp 7 Be neutrino detector Y.Suzuki Kamioka Obs. ICRR, U.Tokyo @LowNu 2000-06-15 Detector 1) Liquid Xenon with 10 ton fiducial volume 2) Scintillation detector: 42,000 photons/mev similar
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
XAX The Ultimate Multi-Purpose Detector for Dark Matter, Double Beta Decay and Solar Neutrino
2008/5/14 Katsushi Arisaka 1 XAX (Xenon-Argon-Xenon) on) XAX The Ultimate Multi-Purpose Detector for Dark Matter, Double Beta Decay and Solar Neutrino Katsushi Arisaka University of California, Los Angeles
ANAIS: Status and prospects
LSC Laboratorio Subterráneo de Canfranc ANAIS: Status and prospects Miguel Ángel Oliván on behalf of the ANAIS team Universidad de Zaragoza Laboratorio Subterráneo de Canfranc RICAP 2014 Roma International
TWO-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
Sensitivity 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
Recent 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
Prospects for WIMP Dark Matter Direct Searches with XENON1T and DARWIN
Via Lactea 2 (2008) Prospects for WIMP Dark Matter Direct Searches with XENON1T and DARWIN NASA/WMAP 8th Patras Workshop on Axions, WIMPs, and WISPs Chicago, 21-July-2012 http://xenon.physik.uni-mainz.de
Dark matter search with the SABRE experiment
Dark matter search with the SABRE experiment Giulia D Imperio* for the SABRE collaboration *INFN Roma 1 25-07-2017 TAUP 2017 Sudbury, Canada 1 Dark matter detection through annual modulation WIMP is one
Measurements 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
June 10 morning session 9:00-
ABSTRACT BOOK June 10 morning session 9:00-10A1 Title: Welcome / CYGNUS: where we are Author: Kentaro Miuchi Abstract: Welcome to CYGNUS 2013! The status and aim of the CYGNUS workshop will be discussed
PANDA-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
The 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
Direct 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,
Direct 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
LUX: 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
Direct WIMP Detection in Double-Phase Xenon TPCs
Outline PMTs in the XENON dark matter experiment XENON100 and the weekly gain calibration XENON1T and candidates for the light sensors Tests of Hamamatsu R11410 2 Direct WIMP Detection in Double-Phase
DarkSide-50: performance and results from the first atmospheric argon run
DarkSide-50: performance and results from the first atmospheric argon run Yann Guardincerri on behalf of the DarkSide Collaboration August 27th, 2014 1 / 21 DarkSide Direct detection search for WIMP dark
Background 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
The XENON1T Experiment
The XENON1T Experiment Ranny Budnik Columbia University On behalf of the XENON1T collaboration 1 Status in WIMP DM Sensitivities (2012) Spin-independent Spin-dependent, n-coupling preliminary Spin-dependent,
Direct Dark Matter Search with Noble Liquids
Direct Dark Matter Search with Noble Liquids Marc Schumann Physik Institut, Universität Zürich Recontres de Moriond 2012, Cosmology Session, La Thuile, March 2012 marc.schumann@physik.uzh.ch www.physik.uzh.ch/groups/groupbaudis/xenon/
DARK 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
Technical 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
Direct 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
Direct 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
THE 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
Recent 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
Search for Dark Matter with Liquid Argon and Pulse Shape Discrimination
Search for Dark Matter with Liquid Argon and Pulse Shape Discrimination Results from DEAP-1 and Status of DEAP-3600 Pierre Gorel for the DEAP collaboration University of Alberta Dark matter Experiment
Prospects for kev-dm searches with the GERDA experiment
Physik-Institut Prospects for kev-dm searches with the GERDA experiment Roman Hiller for the GERDA collaboration 29/03/2017 Page 1 GERDA concept Cleanroom Lock systen Enriched 76 Ge detectors Cryostat
Ge and Dark Matter Searches: CDEX, present and future
Ge and Dark Matter Searches: CDEX, present and future -Ge detectors at LN temperature Lin, Shin-Ted / Sichuan University On behalf of CDEX Collaboration Oct. 19, 2015 (Materials Provided by Prof. Qian
Dark Matter Detection with XENON100 Accomplishments, Challenges and the Future
Dark Matter Detection with XENON0 Accomplishments, Challenges and the Future http://xenon.astro.columbia.edu Kaixuan Ni Columbia University TeV Particle Astrophysics IHEP, Beijing, Sep.4-8, 008 The Challenges
XMASS experiment Dark matter search with liquid Xe detector
experiment Dark matter search with liquid Xe detector Akihiro MINAMINO (ICRR) for collaboration Contents Direct search of Dark matter experiment Dark matter search with 800kg detector R&D status of prototype
Esperimenti 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
( Some of the ) Lateset results from Super-Kamiokande
1 ( Some of the ) Lateset results from Super-Kamiokande Yoshinari Hayato ( Kamioka, ICRR ) for the SK collaboration 1. About Super-Kamiokande 2. Solar neutrino studies in SK 3. Atmospheric neutrino studies
Nuclear Instruments and Methods in Physics Research A
Nuclear Instruments and Methods in Physics Research A 659 (2011) 161 168 Contents lists available at SciVerse ScienceDirect Nuclear Instruments and Methods in Physics Research A journal homepage: www.elsevier.com/locate/nima
DarkSide 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
Status and Sensitivity Projections for the XENON100 Dark Matter Experiment
Status and Sensitivity Projections for the XENON Dark Matter Experiment Elena Aprile Columbia Astrophysics Laboratory, Columbia University, New York, NY 27, USA E-mail: age@astro.columbia.edu Laura Baudis
Measurement 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
Search for Astrophysical Neutrino Point Sources at Super-Kamiokande
Search for Astrophysical Neutrino Point Sources at Super-Kamiokande Yusuke Koshio for Super-K collaboration Kamioka, ICRR, Univ. of Tokyo LNGS, INFN Super-Kamiokande detector Recent results of search for
Collaborazione DAMA & INR-Kiev. XCVIII Congresso SIF Napoli, 18 Settembre F. Cappella
Collaborazione DAMA & INR-Kiev http://people.roma2.infn.it/dama XCVIII Congresso SIF Napoli, 18 Settembre 2012 F. Cappella Based on the study of the correlation between the Earth motion in the galactic
PandaX Dark Matter Search
PandaX Dark Matter Search Xiangdong Ji Shanghai Jiao Tong University University of Maryland On Behalf of the PandaX Collaboration 2017/8/7 1 Outline Introduction to WIMP search and liquid xenon experiments
Search 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
DARK 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
LUX: The next stage(s) Multi-tonne LXe TPC s (DM08, Marina del Rey, 21 Feb 08)
LUX: The next stage(s) Multi-tonne LXe TPC s (DM08, Marina del Rey, 21 Feb 08) Rick Gaitskell Particle Astrophysics Group, Brown University, Department of Physics (Supported by US DOE HEP) see information
The Factors That Limit Time Resolution for Photon Detection in Large Cherenkov Detectors
The Factors That Limit Time Resolution for Photon Detection in Large Cherenkov Detectors Kate Scholberg, Duke University Chicago, April 2011 OUTLINE - Overview/physics motivation - Event reconstruction
Down-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
The 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,