Two-Phase Xenon Time Projection Chambers for WIMP Searches and Other Applications
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Overview of Dark Matter Searches with Liquid Nobles
Overview of Dark Matter searches with liquid nobles Marcin Kuźniak [email protected] 29-08-2019 Marcin Kuźniak – LIDINE2019, Manchester 1 Outline ● Dark matter detection ● Noble liquid technology ● Physics landscape – High mass WIMPs ● Spin-independent ● Spin-dependent – Low mass WIMPs ● Status of experimental Ar and Xe programs ● Target complementarity ● Main challenges moving forward ● (Biased) selection of new ideas ● Summary 29-08-2019 Marcin Kuźniak – LIDINE2019, Manchester 2 DM direct detection signature Direct detection ● Only through rare interactions with ordinary matter ● After the interaction, recoiling nucleus deposits energy (heat, 100 GeV WIMP light, electric charge, ...) in the detector Nuclear recoil spectrum ● featureless, ~exponential ● lower threshold =>more sensitivity ● natural radioactivity is a background astrophysics detector response particle/nuclear physics 29-08-2019 Marcin Kuźniak – LIDINE2019, Manchester 3 Backgrounds 29-08-2019 Marcin Kuźniak – LIDINE2019, Manchester 4 Liquid noble detectors Excitation Heat Nuclear recoils (NR) Ar and Xe are used for WIMP detection. ● Ar inexpensive and advantageous for purification and background rejection Why noble elements? ● High light yield, transparent to their own scintillation ● Easy to purify and scalable to very high masses ● (At least) two available detection channels: scintillation and ionization 29-08-2019 Marcin Kuźniak – LIDINE2019, Manchester 5 Single or dual phase DEAP gas DarkSide approach approach Detect primary scintillation light (S1) from the original -
Optimizing Tracking Software for a Time Projection Chamber Wilson H
Journal of the Arkansas Academy of Science Volume 49 Article 18 1995 Optimizing Tracking Software for a Time Projection Chamber Wilson H. Howe University of Arkansas at Little Rock Christine A. Byrd University of Arkansas at Little Rock Amber D. Climer University of Arkansas at Little Rock Wilfred J. Braithwaite University of Arkansas at Little Rock Jeffrey T. Mitchell Brookhaven National Laboratory Follow this and additional works at: http://scholarworks.uark.edu/jaas Part of the Nuclear Commons Recommended Citation Howe, Wilson H.; Byrd, Christine A.; Climer, Amber D.; Braithwaite, Wilfred J.; and Mitchell, Jeffrey T. (1995) "Optimizing Tracking Software for a Time Projection Chamber," Journal of the Arkansas Academy of Science: Vol. 49 , Article 18. Available at: http://scholarworks.uark.edu/jaas/vol49/iss1/18 This article is available for use under the Creative Commons license: Attribution-NoDerivatives 4.0 International (CC BY-ND 4.0). Users are able to read, download, copy, print, distribute, search, link to the full texts of these articles, or use them for any other lawful purpose, without asking prior permission from the publisher or the author. This Article is brought to you for free and open access by ScholarWorks@UARK. It has been accepted for inclusion in Journal of the Arkansas Academy of Science by an authorized editor of ScholarWorks@UARK. For more information, please contact [email protected], [email protected]. Journal of the Arkansas Academy of Science, Vol. 49 [1995], Art. 18 a Time Projection Chamber Wilson H. Howe, Christine A.Byrd, Amber D. Climer, W.J. Braithwaite Department of Physics and Astronomy University of Arkansas at Little Rock LittleRock, Ar 72204 Jeffrey T.Mitchell Brookhaven National Laboratory Upton, NY11973 Abstract International research collaborations willbe using accelerators in the U.S. -
First Science Results from the LUX Dark Matter Experiment
First Science Results from the LUX Dark Matter Experiment Daniel McKinsey, LUX Co-Spokesperson, Yale University Richard Gaitskell, LUX Co-Spokesperson, Brown University on behalf of the LUX Collaboration http://luxdarkmatter.org Sanford Underground Research Facility OctoberS 30, 2013 LUX Dark Matter Experiment / Sanford Lab Rick Gaitskell (Brown) / Dan McKinsey (Yale) 1 Composition of the Universe The Higgs particle has been discovered, the last piece of the Standard Model. But as successful as it has been, the Standard Model describes only 5% of the universe. The remaining 95% is in the form of dark energy and dark matter, whose fundamental nature is almost completely unknown. Image: X-ray: NASA/CXC/CfA/M.Markevitch et al.; www.quantumdiaries.org Optical: NASA/STScI; Magellan/U.Arizona/D.Clowe et al.; Lensing Map: NASA/STScI; ESO WFI; Magellan/U.Arizona/D.Clowe et al. LUX Dark Matter Experiment / Sanford Lab 2 Rick Gaitskell (Brown) / Dan McKinsey (Yale) 2 Evidence for Dark Matter Galaxy rotation curves The cosmic microwave background www.quantumdiaries.org Image: ESA and the Planck collaboration Gravitational lensing • 27% of the energy composition of the universe • Properties: • Stable and electrically neutral • Non-baryonic • Non-relativistic • Estimated local density: 0.3±0.1GeV·cm-3 • Candidates: WIMPs, axions, dark photons,... Colley, Turner, Tyson, and NASA LUX Dark Matter Experiment / Sanford Lab 3 Rick Gaitskell (Brown) / Dan McKinsey (Yale) 3 Weakly Interacting Massive Particles (WIMPs) A new particle that only very weakly interacts with ordinary matter could form Cold Dark Matter - Formed in massive amounts in the Big Bang. - Non-relativistic freeze-out. -
Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search
Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2006 c 2006 Kaixuan Ni All rights reserved Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni Advisor: Professor Elena Aprile Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2006 c 2006 Kaixuan Ni All rights reserved ABSTRACT Development of a Liquid Xenon Time Projection Chamber for the XENON Dark Matter Search Kaixuan Ni This thesis describes the research conducted for the XENON dark matter direct detection experiment. The tiny energy and small cross-section, from the interaction of dark matter particle on the target, requires a low threshold and sufficient background rejection capability of the detector. The XENON experiment uses dual phase technology to detect scintillation and ionization simultaneously from an event in liquid xenon (LXe). The distinct ratio, be- tween scintillation and ionization, for nuclear recoil and electron recoil events provides excellent background rejection potential. The XENON detector is designed to have 3D position sensitivity down to mm scale, which provides additional event information for background rejection. Started in 2002, the XENON project made steady progress in the R&D phase during the past few years. Those include developing sensitive photon detectors in LXe, improving the energy resolution and LXe purity for detect- ing very low energy events. -
Direct Dark Matter Searches: the Experimental Context
Conseil Scientifique de l’IN2P3, 25-26 octobre 2018 Direct Dark Matter searches: the experimental context Alessandra Tonazzo (APC, Université Paris-Diderot) Direct search for WIMPs : current status ���������� ��������� -�� -� �� ����-� �� - ] ��� ] � ����� -�� -� �� �� �� [ �� [ ������ ������ �� �� σ σ -�� -��� -� �� ����� �� - -�� �� �������� � �� -���� ��� ���� -�� - �������� ������� -�� � -� ������� �� �� - - ��� ��-�� ������� ��-�� ���� ������ ���� ������ ��-�� ��-�� ���� ����� ������� ������� �� ����� ����� ���������� �� ������� ��� �������� ��������� ������������ ���������� ������� ��������� �� ��������� coherent ν scattering on Xe ��-�� � �� ��� ���� A personal selection ���� ������ ���� [���/��] CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 2 Direct detection of WIMPs WIMP <v>˜220 km/s Nuclear Recoil detectable signal ER < 100 keV Rate: ~1 evt/(ton*year) for σ~10-47cm2 in noble liquids CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 3 Backgrounds WIMP • Cosmic rays and cosmogenic neutron neutrons/isotopes neutrino • Radioactivity, natural (238U,232Th,235U,222Rn,...) or anthropogenic Nuclear Recoil (85Kr,137Cs,...), from detector elements e, γ • Neutrinos (solar, atmospheric, diffuse SN) scattering coherently off nuclei (”neutrino floor”) Electron Recoil Possibility for background discrimination CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 4 Direct detection of WIMPs : signatures • Anomalous rate of low-energy nuclear recoils • -
Using a Two-Phase Xenon Time Projection Chamber for Improved Background Rejection in Searches for Neutrinoless Double-Beta Decay
Using a two-phase xenon time projection chamber for improved background rejection in searches for neutrinoless double-beta decay by Callan Jessiman A thesis submitted to the Faculty of Graduate and Postdoctoral Affairs in partial fulfilment of the requirements for the degree of Master of Science in Physics Department of Physics Carleton University Ottawa, Ontario January 2020 c 2020 Callan⃝ Jessiman Abstract The nature of the neutrino masses is an important open question in particle physics; neutrinos were conceived and implemented into the Standard Model as massless, and their masses, now known to be nonzero, represent an area of new physics. Essential to the investigation of this area are mechanisms by which one might measure these masses, including the hypothetical neutrinoless double-beta decay, which has a lifetime related to the neutrino masses. Experiments searching for this rare decay, such as EXO, are impacted heavily by sources of background radiation. Here, a prototype two-phase time projection chamber is described, having superior temporal resolution to the existing EXO architecture. A machine- learning analysis of data from this prototype is used for pulse-shape discrimination, which has the potential to significantly increase EXO's sensitivity; the preliminary efforts described here are able to reduce backgrounds by 94%, while rejecting only 21% of the signal. ii Acknowledgements First, and foremost, I express my gratitude towards my supervisor, David Sinclair, and my colleague Braeden Veenstra. The entire project was of David's devising, as was the leadership that saw it through. Meanwhile, getting the thing to actually work, and extracting results from it, was Braeden's task as much as it was mine. -
1.1 the XMASS Project 1.2 XMASS-I
STATUS OF XMASS Y. KISIMOTO forXMASS collaboration Kamioka Observatory, Institute for Cosmic Ray Research, the University of To kyo, Higashi-Mozumi, Kamioka, Hida, Gifu 506-1205, JAPAN, Kavli Institute for Physics and Mathematics of the Universe (WPI) , the University of Tokyo, Kashiwa, Chiba 217-8582, JA PAN The XMASS experiment is a multi-purpose detector for rare events, such as direct detection of dark matter, using single-phase liquid xenon. The current phase of the XMASS(XMASS I) is focused on direct dark-matter detection with the largest target mass (835kg). In this paper, we report results of searches carried out with commissioning runs of the XMASS-I and current status of XMASS-I after hardware modification to reduce background followed by the commissioning runs. 1 The XMASS experiment 1.1 The XMASS project The XMASS project was proposed to observe rare events such as elastic scattering of electron by pp solar neutrinos, neutrinoless double beta decay, and elastic scattering of nuclei by dark matter particles with a large liquid-Xe detector 1. In the XMASS detector, scintillation lights from liquid xenon are observed by photo-multiplier tubes PMTs arranged around the liquid xenon volume. This simple configuration is very much suitable( for) observing the rare events because liquid xenon is an efficient scintillator and attenuation of scintillation light is quite small and also because liquid xenon has hight atomic number and high density and so it is worked as shield material against radiation from outside. We can, therefor, search for the rate events by extracting events in a low-background volume. -
The XMASS 800Kg Experiment
The XMASS 800kg Experiment XMASS collaboration: Kamioka Observatory, ICRR, Univ. of Tokyo: K. Abe, K. Hieda, K. Hiraide, Y. Kishimoto, K. Kobayashi, Y. Koshio, S. Moriyama, M. Nakahata, H. Ogawa, H. Sekiya, A. Shinozaki, Y. Suzuki, O. Takachio, A. Takeda, D. Umemoto, M. Yamashita, B. Yang IPMU, University of Tokyo: K. Martens, J.Liu Jing LIU Kobe University: K. Hosokawa, K. Miuchi, A. Murata, Y. Ohnishi, Y. Takeuchi Tokai University: F. Kusaba, K. Nishijima Gifu University: S. Tasaka Kavli IPMU, Univ. of Tokyo Yokohama National University: S. Nakamura, I. Murayama, K. Fujii Miyagi University of Education: Y. Fukuda NPB2012, Shenzhen STEL, Nagoya University: Y. Itow, K. Masuda, H. Uchida, H. Takiya Sejong University: Y.D. Kim Seoul National University: S. B. Kim KRISS: Y.H. Kim, M.K. Lee, K. B. Lee, J.S. Lee Xenon MASSive detector for Solar neutrino (pp/7Be) Xenon neutrino MASS detector (double beta decay) The XMASS Experiment Xenon detector for weakly interacting MASSive Particles PMT LXe inside ~100 kg LXe ~800 kg LXe multi ton scale prototype direct dark matter search Multi-purpose LXe (Liquid Xenon) surrounded by PMTs (Photomultiplier Tubes) recording scintillation lights generated by nuclear or electronic recoils in LXe XMASS 800kg Jing LIU @ NPB 2012 2 Xenon MASSive detector for Solar neutrino (pp/7Be) Xenon neutrino MASS detector (double beta decay) The XMASS Experiment Xenon detector for weakly interacting MASSive Particles PMT γ, n, α,… or χ? LXe LXe inside scintillation PMT ~100 kg LXe ~800 kg LXe ~26 ton LXe prototype direct -
Broader Impacts of XENON Research
XENON: A Liquid Xe Dark Matter Search Experiment at LNGS Columbia University: Elena Aprile, Karl-Ludwig Giboni, Pawel Majewski, Kaixuan Ni, Bhartendu Singh, Masaki Yamashita Brown University: Richard Gaitskell, Peter Sorensen, Luiz DeViveiros University of Florida: Laura Baudis, David Day Lawrence Livermore National Laboratory: William Craig, Adam Bernstein, Chris Hagmann Princeton University: Tom Shutt, John Kwong, Kirk McDonald Rice University: Uwe Oberlack, Omar Vargas Yale University: Daniel McKinsey, Richard Hasty, Hugh Lippincott Contact person Elena Aprile ([email protected]) Letter of Intent 1 1. The physics case The goal of the XENON experimental program is direct detection of dark matter in the form of weakly interacting massive particles (WIMPs) with an array of ten identical liquid Xe detector modules each with a 100 kg fiducial mass (XENON100).Current theoretical models indicate that WIMP interaction rates probably lie between the current sensitivity of existing experiments which is equivalent to ~0.25 evts/kg/day and ~2 evts/100 kg/yr normalized for a Xe target. The best prospects for the unambiguous identification of a WIMP nuclear recoil signal lie in detectors that have negligible radioactive background competing with the dark matter signal. This can be achieved principally by using nuclear recoil discrimination in order to veto competing electron recoil events (associated with gamma and beta backgrounds), effective neutron shielding, and through the operation of a large homogeneous detector volume with 3-D position resolution. The latter information can be used to select single hit events characteristic of a WIMP interaction while rejecting multiple hit events associated with backgrounds that propagate from the edge of the detector into the fiducial volume. -
Habilitationsschrift Zur Erlangung Der Venia Legendi Für Das
Habilitationsschrift zur Erlangung der Venia legendi f¨urdas Fach Physik der Ruprecht{Karls{Universit¨at Heidelberg vorgelegt von Teresa Marrod´anUndagoitia aus Eibar (Spanien) 2014 Revealing the nature of dark matter with XENON Habilitation summary by Teresa Marrod´anUndagoitia March 2014 Contents 1 Introduction 1 1.1 Indications for dark matter from Astronomy and Cosmology . 1 1.2 The nature of dark matter: possible candidates . 3 1.3 Searches for dark matter particles . 4 1.4 Principles of direct detection . 5 1.5 Current experimental results and possible interpretations . 7 2 The XENON experiment 9 2.1 Liquid xenon as detector material . 9 2.2 The XENON100 instrument . 10 2.3 Detector performance . 11 3 Searches for WIMPs in XENON100 13 3.1 Data selection and efficiency . 13 3.2 Nuclear recoil energy scale . 14 3.3 Background sources and experimental results . 15 3.4 Spin independent and dependent interpretations . 17 3.5 Other interpretations of the XENON100 data . 18 4 Light dark matter particles inducing electronic recoils 19 4.1 Motivation . 19 4.2 Low energy calibration sources . 20 4.3 Measurement of the electronic recoil scale using a Compton experiment . 22 4.4 Energy threshold of XENON100 . 22 5 Summary and outlook 25 Appendices 37 I Contents A Own contributions 39 B Main publications summarised in this work 41 C Complete list of publications 43 II Chapter 1 Introduction The existence of a new form of non-luminous matter is indicated by a variety of cosmo- logical and astronomical observations. It is commonly assumed that elementary particles could be the constituents of this 'dark' matter. -
Jianglai Liu Shanghai Jiao Tong University
Jianglai Liu Shanghai Jiao Tong University Jianglai Liu Pheno 2017 1 If DM particles have non-gravitational interaction with normal matter, can be detected in “laboratories”. DM DM Collider Search Indirect Search ? SM SM Direct Search Pheno 2017 Jianglai Liu Pheno 2017 2 Galactic halo . The solar system is cycling the center of galaxy with on average 220 km/s speed (annual modulation in earth movement) . DM local density around us: 0.3(0.1) GeV/cm3 Astrophys. J. 756:89 Inclusion of new LAMOST survey data: 0.32(0.02), arXiv:1604.01216 Jianglai Liu Pheno 2017 3 1973: discovery of neutral current Gargamelle detector in CERN neutrino beam Dieter Haidt, CERN Courier Oct 2004: “The searches for neutral currents in previous neutrino experiments resulted in discouragingly low limits (@1968), and it was somehow commonly concluded that no weak neutral currents existed.” leptonic NC hadronic NC v beam Jianglai Liu Pheno 2017 4 Direct detection A = m2/m1 . DM: velocity ~1/1500 c, mass ~100 GeV, KE ~ 20 keV . Nuclear recoil (NR, “hadronic”): recoiling energy ~10 keV . Electron recoil (ER, “leptonic”): 10-4 suppression in energy, very difficult to detect New ideas exist, e.g. Hochberg, Zhao, and Zurek, PRL 116, 011301 Jianglai Liu Pheno 2017 5 Elastic recoil spectrum . Energy threshold mass DM . SI: coherent scattering on all nucleons (A2 Ge Xe enhancement) . Note, spin-dependent Si effect can be viewed as scattering with outer unpaired nucleon. No luxury of A2 enhancement Gaitskell, Annu. Rev. Nucl. Part. Sci. 2004 Jianglai Liu Pheno 2017 6 Neutrino “floor” Goodman & Witten Ideas do exist Phys. -
Distillation Purification of Xenon for Krypton and Measurement of Radon Contamination in Liquid Xenon
DISTILLATION PURIFICATION OF XENON FOR KRYPTON AND MEASUREMENT OF RADON CONTAMINATION IN LIQUID XENON Y. Takeuchi for the XMASS collaboration Kamioka Observatory, ICRR, Univ. of Tokyo, Higashi-Mozumi, Gifu506-1205, Japan ABSTRACT: We succeeded to reduce the Kr contamination in liquid xenon by a factor of 1/1000 with a distillation system in Kamioka mine. Then, the remaining radioactivities in purified liquid xenon were measured with the XMASS prototype detector. In this report, the distillation system and the remaining internal radioactivity levels are described. 1. INTRODUCTION Liquid xenon is a good scintillator. It has a good photon yield (about 42photon/keV). Therefore, sensitivity against low energy events is good. The wave length (~175nm) is rather short, but it still can be observed by PMTs directly without a wave length shifter. The large atomic number provides a short radiation length for the low energy gamma rays. So, the external low-energy gamma rays would be absorbed in the outer region of the liquid xenon detector, and then the central region would become clean. The boiling point of liquid xenon is higher than other rare gas, like argon or neon, so it is relatively easy to handle. We can use liquid nitrogen to liquefy xenon. Because of rare gas and liquid, various purify methods can be applied. Xenon doesn't have long life radioactive isotopes. A possible problem of liquid xenon for the low background experiments is that there is a contamination of 85Kr during manufacture and refinement. Usual commercial “krypton-free” xenon still has ppb level krypton. It could become a serious background for the low background experiments.