DOCSLIB.ORG

Introduction to Class and Dark Matter

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Introduction 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 Outline 1 Introduction to Class 2 Introduction to Dark Matter Evidence for Dark Matter Searching for Dark Matter 3 Reminders L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 2 / 22 Introduction to Class You're not Prof. Corwin! Correct, I am not any of the 3 professors named Corwin (Luke, Edward, or Kelly) at Mines Prof. Luke Corwin is in Japan on a research-related trip I have agreed to take over this class for Jan. 14, 16, and 21. Barring unforeseen problems, Prof. L. Corwin will be back for Jan. 23 and most or all of the remainder of the semester. L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 3 / 22 Introduction to Class Available on the Class Webpage http://odessa.phy.sdsmt.edu/~lcorwin/PHYS792DM_ Spring2014/ClassWebpage.html The syllabus Past lecture notes (and recordings if possible) All out-of-class homework L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 4 / 22 Introduction to Class Mid-term Presentation 20 min. length Select one candidate for dark matter and explain it to the class Your presentation will need to help your fellow students understand the theoretical nature of this candidate and how well (or poorly) it is supported by current experimental data You may choose any candidate except for WIMPs Presentations will be during Week 7 Choose your candidate before or in class on Jan. 30. L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 5 / 22 Introduction to Class Dark Matter Candidates Massive Compact Halo Objects (MaCHOs) Axions Particles interacting only via gravity Sterile neutrinos superWIMPs Modified Newtonian Dynamics (MOND) If you know of another candidate, let Prof. Corwin know. L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 6 / 22 Introduction to Class Final Project Presentation 20 min. length Select one dark matter detection experiment and explain it to the class. You presentation will need to help your fellow students understand the type of dark matter being sought, the methods used, possible backgrounds, and expected sensitivities or results. You may choose an experiment that has been concluded, is in operation, is under construction, or is planned. We will have the presentations during finals week; exact times will be determined by the class. Choose your experiment before or in class on Feb. 20 Each student will present on a different experiment L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 7 / 22 Introduction to Class Possible Experiments Direct Searches ADMX, ArDM, CDMS, COUPP, Cogent, CRESST, CUORE, DAMA, DAMIC, DarkSide, DEAP/CLEAN, DM-TPC, DM-ice, Drift, Edelweiss, Eureca, IGEX, LIBRA, MIMAC, NAIAD, NEWAGE, ORPHEUS, PandaX, Picasso, ROSEBUD, SIMPLE, TEXONO, UKDMC, XENON, XMASS, WARP, Zeplin Indirect Searches AMANDA, AMS, ANTARES, BAIKAL, BESS, CAPRICE, CTA, Fermi, GAPS, HEAT, HESS, IceCube, IMAX, MACRO, Nestor, NINA, Pamela, Super-K L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 8 / 22 Introduction to Class Independent Study PaperI Students taking the Independent Study Dark Matter course for 1 additional credit are required to write a paper 4-5 pages using LATEX with header including \documentclass[11pt]{article} \geometry{verbose,letterpaper,lmargin=1in, rmargin=1in,tmargin=1in,bmargin=1in} Due May 1, 2014 L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 9 / 22 Introduction to Class Independent Study PaperII Topic Choices 1 Status and Methods of dark matter searches at particle colliders 2 What theoretical models of dark matter could explain the positive results of DAMA/LIBRA and CoGeNT as well as the negative results of LUX, etc? 3 What possibilities exist for WIMP detection beyond the \neutrino floor"? 4 How could WIMPs affect stellar or planetary evolution? 5 If you have a different idea for a topic, please let me know and we will discuss it. L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 10 / 22 Introduction to Dark Matter What do you know about dark matter? L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 11 / 22 Introduction to Dark Matter The Great Misnomer \Dark" matter is not really dark. If it were, we could detect it absorbing light. It has no electromagnetic interactions, so it is actually transparent, but \transparent matter" doesn't have quite the same ring to it Some theorists speculate that the effects we see are not actually from matter but from misunderstood gravity. We shall cover this in a later session. In the next few slides, we will briefly review some of the evidence for dark matter and the methods for searching for it. These will all be covered in detail throughout the semester. L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 12 / 22 Introduction to Dark Matter Evidence for Dark Matter Figure : On scales from galaxies to the cosmos, we see more gravity than can be accounted for by visible matter. http://cheezburger.com/2510042880 L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 13 / 22 Introduction to Dark Matter Evidence for Dark Matter Galactic Rotation Curves One of the iconic galactic rotation curves from Mon. Not. Roy. Astron. Soc. 249 (1991) 523. \. the dashed curves are for the visible components, the dotted curves for the gas, and the dash-dot curves for the dark halo." L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 14 / 22 Introduction to Dark Matter Evidence for Dark Matter Figure : The \Bullet Cluster": Hot gas detected in X-rays (pink), visible matter (white and orange), and gravitational lensing (blue) indicate most of the matter in these clusters is \dark". http://chandra.harvard.edu/photo/2006/1e0657/ L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 15 / 22 Introduction to Dark Matter Evidence for Dark Matter What We Know Something is causing the appearance of more gravity than can be explained with visible matter. Excess matter could also help explain the large-scale structure of the Universe and present abundances of light elements in the Universe. If this \something" is matter and is in particle form, that particle is nothing we have encountered in the lab or at accelerators. We have bounds on this particle's behavior from stellar behavior and astrophysics. It must have mass and be even more weakly interacting than neutrinos; therefore, the most favored candidates are called Weakly Interactive Massive Particles L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 16 / 22 Introduction to Dark Matter Evidence for Dark Matter What We Don't Know We don't know for certain that dark matter particles exist, as opposed to new physics of gravity. Most physicist are confident, but it would be better to actually find the particles Are dark matter particles WIMPs? Does more than one dark matter particle exist? What is it's mass? What are its spin-independent and spin-dependent nuclear cross-sections? Is the dark matter particle its own antiparticle? L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 17 / 22 Introduction to Dark Matter Searching for Dark Matter How We Find Out: Two Search Methods Direct Detection Cryogenic liquid or solid detectors are used to search for the small energy deposited by a WIMP on the rare occasion in collides with a nucleus. At Sanford, LUX and the planned LZ experiment use this approach with cryogenic liquid xenon. Indirect Detection If dark matter and anti-dark matter particles exist in sufficient densities and have sufficient annihilation cross-sections, they will produce detectable amounts of annihilation produces (e.g. positrons or neutrinos) that would be indirect evidence of particle dark matter. L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 18 / 22 Introduction to Dark Matter Searching for Dark Matter Direct Detection Example: LUX L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 19 / 22 Introduction to Dark Matter Searching for Dark Matter Direct Detection Example: LUX First Results LUX 90% CL ) (blue) compared 2 with the limits from several −44 10 previous direct DM searches. The inset 6 8 10 12 (same axis units) also shows the −40 10 nucleon cross section (cm regions claimed as − −45 evidence or 10 −42 WIMP 10 measurement from other experiments.a −44 10 1 2 3 a 10 10 10 arXiv:1108.3384 m (GeV/c2) WIMP L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 20 / 22 Introduction to Dark Matter Searching for Dark Matter Indirect Detection Example: Super-Kamiokande -12 ) 10 AMANDA -1 s Soft channel ICECUBE -2 SK-I -13 10 SK-I+II+III -14 10 -15 10 Expected flux region (E > 1 GeV ) Limit on WIMP-induced upmu (cm -16 µ 10 2 3 4 10 10 10 WIMP mass(GeV/c2) Figure : Upper limit of the flux of ν-induced upward going muons resulting from dark matter particles trapped in the sun annihilating into bb. The shaded region represents a particular dark matter model (Astrophysical J. 742 (2011) 78). L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 21 / 22 Reminders Reminders First Homework Due Jan. 21 Choose your topic for mid-term presentation before Jan. 30 Choose your topic for final presentation on or before Feb. 20 L. Corwin, PHYS 792 (SDSM&T) Introduction Jan. 14, 2014 (W1-1) 22 / 22.
Load more

Recommended publications
  • 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
    [Show full text]
  • A Statistical Framework for the Characterisation of WIMP Dark Matter with the LUX-ZEPLIN Experiment
    A statistical framework for the characterisation of WIMP dark matter with the LUX-ZEPLIN experiment Ibles Olcina Samblas Department of Physics A thesis submitted for the degree of Doctor of Philosophy November 2019 Abstract Several pieces of astrophysical evidence, from galactic to cosmological scales, indicate that most of the mass in the universe is composed of an invisible and essentially collisionless substance known as dark matter. A leading particle candidate that could provide the role of dark matter is the Weakly Interacting Massive Particle (WIMP), which can be searched for directly on Earth via its scattering off atomic nuclei. The LUX-ZEPLIN (LZ) experiment, currently under construction, employs a multi-tonne dual-phase xenon time projection chamber to search for WIMPs in the low background environment of the Davis Campus at the Sanford Underground Research Facility (South Dakota, USA). LZ will probe WIMP interactions with unprecedented sensitivity, starting to explore regions of the WIMP parameter space where new backgrounds are expected to arise from the elastic scattering of neutrinos off xenon nuclei. In this work the theoretical and computational framework underlying the calculation of the sensitivity of the LZ experiment to WIMP-nucleus scattering interactions is presented. After its planned 1000 live days of exposure, LZ will be able to achieve a 3σ discovery for spin independent cross sections above 3.0 10 48 cm2 at 40 GeV/c2 WIMP mass or exclude at × − 90% CL a cross section of 1.3 10 48 cm2 in the absence of signal. The sensitivity of LZ × − to spin-dependent WIMP-neutron and WIMP-proton interactions is also presented.
    [Show full text]
  • 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 •
    [Show full text]
  • 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.
    [Show full text]
  • Book of Abstracts Ii Contents
    DMSS: A Dark Matter Summer School Monday, 16 July 2018 - Friday, 20 July 2018 Other Institute Book of Abstracts ii Contents Introduction to Dark Matter .................................. 1 Supersymmetry ......................................... 1 Large Scale Structure Formation ................................ 1 Roundtable Discussions ..................................... 1 Dark Matter in the Milky Way ................................. 1 Neutrinos ............................................ 1 Direct Detection of Dark Matter ................................ 1 Roundtable Discussions ..................................... 1 Indirect Dark Matter Searches ................................. 2 Statistical Methods used in Dark Matter ............................ 2 Axions .............................................. 2 Cosmic Microwave Background ................................ 2 Non-SUSY Dark Matter ..................................... 2 Roundtable Discussions ..................................... 2 Dark Matter at the LHC ..................................... 2 Dark Energy ........................................... 2 Roundtable Discussions ..................................... 3 Roundtable Discussions ..................................... 3 Dark Matter search activity at the University of Montreal .................. 3 Extra Dimensions in High-Mass Diphoton Spectrum at 13 TeV ............... 3 The XENONnT Time Projection Chamber .......................... 4 Calibration of the XENON1T experiment at low energies using a Kr83m source . 4 Gravitational-wave
    [Show full text]
  • 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
    [Show full text]
  • LUX Detector
    LUX results and LZ sensitivity to dark matter WIMPs Vitaly A. Kudryavtsev University of Sheffield for the LUX and LZ Collaborations Outline n Dark matter direct detection with two-phase noble element instruments. n LUX detector. n LUX results: o WIMPs – spin-independent interactions; o WIMPs – spin-dependent interactions; o Axions and axion-like particles (ALPs). o Modulation search. n LZ detector. n Backgrounds n Sensitivity to WIMPs. n Conclusions. ICNFP2018, 6 July 2018 Vitaly Kudryavtsev 2 Principle of WIMP detection in LXe TPC n Liquid xenon time projection chamber – LXe TPC. n S1 – primary scintillation. n S2 –secondary scintillation, proportional to ionisation. n Position reconstruction based on the light pattern in the PMTs and delay between S2 and S1. ICNFP2018, 6 July 2018 Vitaly Kudryavtsev 3 Advantages of LXe n Good scintillator. n Two-phase -> TPC with good position resolution. n Self-shielding. n Good discrimination between electron recoils (ERs) and nuclear recoils (NRs). n High atomic mass: spin-independent cross- section ∝ A2 n Presence of even-odd isotopes (odd number of neutrons) for spin-dependent studies. n Other physics: o Axion search, o Neutrinoless double-beta decay. LZ Collaboration, LZ TDR, 1703.09144v1 [physics.ins-det] ICNFP2018, 6 July 2018 Vitaly Kudryavtsev 4 LUX Collaboration ² Brown University ² University at Albany, SUNY ² Imperial College London ² University College London ² LIP Coimbra, Portugal ² University of California, Berkeley ² Lawrence Berkley National Laboratory ² University of California, Davis
    [Show full text]
  • Dark Matter Vienna University of Technology V2.1
    Dark Matter Vienna University of Technology V2.1 Jochen Schieck and Holger Kluck Institut f¨urHochenergiephysik Nikolsdorfer Gasse 18 1050 Wien Atominstitut derTechnischen Universit¨atWien Stadionallee 2 1020 Wien Wintersemester 2017/18 18.12.2017 2 Contents 1 Introduction 7 1.1 What is "Dark Matter" . .7 1.1.1 Dark . .7 1.1.2 Matter . .7 1.1.3 Cosmology . .7 1.1.4 Massive particles as origin of "Dark Matter" . .7 1.1.5 "Dark Matter" as contribution to the energy density of the universe in Cosmology . .7 1.2 First Indication of observing "Dark Matter" . 13 1.3 Brief Introduction to Cosmology . 15 1.3.1 Special Relativity . 16 1.3.2 Differential geometry . 16 1.3.3 General Relativity . 16 1.3.4 Cosmology . 17 1.3.5 Decoupling of matter and radiation . 18 1.4 The Standard Model of Particle Physics . 19 1.4.1 The matter content of the Standard Model . 19 1.4.2 Forces within the Standard Model . 19 1.4.3 Shortcoming of the Standard Model . 20 1.4.4 Microscopic Behaviour of Gravity . 21 2 Evidence 23 2.1 Dynamics of Galaxies . 23 2.2 Gravitational Lensing . 24 2.2.1 Bullet Cluster . 31 2.3 Cosmic Microwave Background . 33 2.4 Primordial Nucleosynthesis (Big Bang Nucleosynthesis - BBN) . 35 3 Structure Evolution 39 3.1 Structure Formation . 39 3.1.1 The Classic Picture . 39 3.1.2 Structure Formation and Cosmology . 41 3.2 Model of the Dark Matter Halo in our Galaxy . 45 3 4 Unsolved Questions and Open Issues 49 4.1 Core-Cusp Problem .
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • The Why and How of Catching Wimps
    F EATURE Kavli IPMU Associate Professor Kai Martens Research Area： Experimental Physics The Why and How of Catching WIMPs catalogue of astronomical observations. This is the Introduction rst time in the history of humankind that such a The Kamioka Observatory is located under mount narrative is purely based on science. Ikeno between the cities of Toyama and Takayama Our narrative successfully tracks astronomical here in Japan. It is not the kind of observatory that observations through this history of the visible Dark Matter was discovered at, but it may be the Universe. We can watch this history unfold as our kind of observatory that the nature of Dark Matter telescopes zoom out from ever older objects at ever is revealed at. And XMASS is one of the experiments higher redshifts. Our narrative even reaches beyond that try to accomplish this. The why and the how the earliest moment of which electromagnetic are what we will be discussing over the next few radiation keeps a record when it explains the relative pages. You will have to forgive me though: It is a abundance of the chemical elements as well as the vast subject and I will take the liberty to cherry pick rich structure we see in the distribution of galaxies examples and feature choices that are designed to across the sky. motivate the path we took with XMASS. That is not to say that there are no more problems We are the Kavli Institute for the Physics and to be solved. There are mists: The abundance of Mathematics of the Universe.
    [Show full text]