DOCSLIB.ORG

Direct Dark Matter Searches: the Experimental Context

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read 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 • In case of positive signature, additional evidence of its nature is needed Rate and spectra in Directionality Annual modulation different target materials Mainly forward scatters larger <v> smaller <v> 100 GeV/c2 WIMP CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 5 Detectors for direct WIMP search Direct detection techniques Detector requirements : PHONONS/ • Large mass HEAT • Low energy threshold Bolometers : Al O : CRESST-I • Background suppression 2 3 * = French ü deep underground contribution ü passive/active shielding Bolometers : Bolometers : * ü low intrinsic radioactivity Ge: EDELWEISS CaWO : CRESST Ge+Si : SuPerCDMS 4 ü ER/NR discrimination Solid-state ü or sPecific signature CCDs : Si : DAMIC* scintillators (directionality, annual mod.) NaI : DAMA CsI : KIMS Light gases : News-G* , MIMAC* Noble element DP-TPC Noble liquids Xe : PandaX, LUX, Ge bolometers LXe : XMASS XENON* Bubble chambers LAr : DEAP Ar : DarkSide* IONISATION/ SCINTILLATION/ multiPle signals à ER/NR discrimination CHARGE LIGHT CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 6 Direct search for WIMPs : status and strategies ���������� ��������� -�� -� �� ����-� �� - ] ��� ] � ����� -�� -� �� �� �� [ �� Threshold [ ������ ������ �� �� σ σ -�� -��� -� �� ����� �� - -�� �� �������� � �� -���� ��� ���� -�� - �������� ������� -�� � -� ������� �� �� - - Mass + discrimination ��� ��-�� ������� ��-�� Bolometers (Si, Ge, CaWO4) CCDs (Si) ���� ������ ���� ������ ��-�� Light gases ��-�� ���� ����� ������� ������� �� Liquefied ����� ����� ���������� �� ������� ��� �������� ��������� ������������NEW ! ���������� noble elements (Xe, Ar) ������� ��������� �� ��������� ��-�� � �� ��� ���� ���� ������ ���� [���/��] CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 7 Cryogenic bolometers + low E threshold, excellent E resolution + good ER/NR discrimination from light or ionization yield - need to operate in a cryostat - limited crystal mass HEAT + LIGHT HEAT + CHARGE à CRESST (CaWO4 @LNGS) EDELWEISS (Ge @LSM) talk by J. Gascon SuPerCDMS (Ge/Si @Soudan) ER NR CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 8 Cryogenic bolometers : recent results CRESST-III (2018,prel.) -�� � small size è • mdet~ 24 g x5 �� �� lower threshold • exPosure = 5.7 kg*day ��������� • threshold = 30 eV ] ] � -�� � �� �� �� [ �� [ �� ��������� �� EDELWEISS-III (2016) �� σ fiducialisationè • m ~ 870 g x24 σ det ��-�� ��-� surface bkg • FID detectors ����-� • exPosure = 582 kg*day - suppression ��� • threshold = 900 eV ����� -�� -� ������� ������� à talk by J. Gascon �� �� - - ���������� ������ ������ SuPerCDMS (2017) -��� ��-�� ��-� • - ����� mdet~ 600 g x15 �� ��������-�� � • exPosure = 1690 kg*day �� ��� • threshold = 8 keV ���� ������ ���� ������ - ��-�� � ��-� ���� ����� ������� ������� �� ����� ����� ���������� �� ������� ��� CDMSlite-Run3 (2018) �������� ��������� ������������ ���������� high bias-V è • m ~ 600 g ������� ��������� �� ��������� det ��-�� coherent ν scattering on Ge lower threshold • large bias V (Luke-Neganov boost) ��� ��� � � �� • exPosure = 36(60) kg*day (degraded PID) � • threshold = 70 eV ���� ������ ���� [���/� ] CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 9 Cryogenic bolometers : future strategies ��������� ��-�� ��-� ����-� - ��� -�� �� -� �� �� �� �� ] ���� ] Lower E threshold � ����� -�� -� �� [ �� �� �� 2 [ �� à �� 1-5 GeV/c Higher bias-voltage ���������� σ σ ��-�� ��-� (Luke-Neganov boost) ������ ������ - ���� ������ ��� ��-�� ��� ��-� ������� ������� - -�� ����� - SuPerCDMS-HV @SNOLAB - �� �������� � -�� �� -� �� ��� �� - EDELWEISS-LT 500/100 kg*d � 2 ��-�� ��-� [NEW!] à ���� ������ 0.1-1 GeV/c Smaller-mass crystals ���� ������ -�� -� �� ���� ����� ������� ������� �� �� ����� ����� ���������� �� ������� ��� (above-ground operation so far) �������� ��������� ������������ ���������� ������� ��������� �� ��������� ��-�� ��� � � �� CRESST-above ground 0.5g Al2O3 ���� ������ ���� [���/��] EDELWEISS-Surf 32g Ge ImProved background discrimination à better ionization resolution EDELWEISS-DMB8, 200 kg @SNOLAB à surface background rejection SuPerCDMS-iZIP @SNOLAB à talk by J. Gascon CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 10 Other DM candidates Electron recoil signal from scattering of very low-mass DM (Axions or Axion-Like Particles) or from absorPtion of Dark Photons EDELWEISS with imProved ionisation will extend reach to lower masses à talk by J. Gascon CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 11 Silicon detectors Dark WIMPs (NR) Photons Si-CCDs DAMIC (ER) à talk by A. Letessier-Selvon 40 g @SNOLAB Proj : 1 kg @LSM 3D position reco PID from cluster pattern ��������� ��-�� ��-� ����-� - ��� -�� �� -� �� �� �� �� �� ���� ] �� ���� ] � ����� �� -�� -� �� [ �� �� �� [ �� �� ���������� σ Si-bolometers SuPerCDMS σ ��-�� ��-� ������ ������ - ���� ������ ��� ��-�� ��� ��-� ������� ������� - -�� ����� - - �� �������� � + Lower energy threshold for WIMP searches -�� �� -� �� ��� �� - � + Single-charge resolution achieved in HV mode (ER) ��-�� ��-� ���� ������ ���� ������ CDMS-HVeV, 0.49 g*day (2018) -�� -� �� ���� ����� ������� ������� �� �� ����� ����� ���������� �� ������� ��� Projection 50 kg*y �������� ��������� ������������ ���������� ������� ��������� �� ��������� ��-�� ��� � � �� ���� ������ ���� [���/��] CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 12 Gaseous detectors NEWS-G à talk by P. Lautridou MIMAC è DIRECTIONAL DETECTION à talk by D. Santos Light gases è low mas WIMPs ��-�� ��� ���������� ���� ��������� Results (@LSM) : -�� - -� � ] �� �� ] � - �� [ • �� 60cm diam ��� [ �� �� -�� -� recoil event �� �� σ • Ne-CH4mix σ ˜34 keVee ������ • exP. 9,7 kg*d ������ ��-�� ��-� - ������� ������� �� � - - �� ��� - � ProsPects (@SNOLAB): ��-�� ��-� • 140cm diam ���� ������ ���� ������ ��-�� ��-�� • H / He ���� ����� ������� ������� �� ����� ����� ���������� �� ������� ��� Other techniques for directional detection : �������� ��������� ������������ ���������� 2 ������� ��������� �� ��������� à down to 0.1 GeV/c ��-�� ��� ��� � � �� emulsions, anisotroPic crystals, LAr ���� ������ ���� [���/��] CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 13 Noble liquid detectors (LXe, LAr) • Non segmented, homogeneous, comPact detectors • Easily scalable to very large masses • accurate position reconstruction -> background rejection • ER/NR discrimination from light + charge • in LAr, ER/NR discrimination also from scintillation Pulse shaPe (PSD) • in LAr, intrinsic contamination from 39Ar à Underground Ar, DePleted Ar Single-phase LIGHT ONLY Dual-phase LIGHT(S1) + CHARGE(S2) LXe : XMASS (832 kg @ Kamioka ) LXe : XENON-1t (1.3t @LNGS), LUX (118 kg@SURF), Panda-X (500kg @CJPL) LAr : DEAP-3600 (3600 kg @SNOLab ) LAr : DarkSide-50 (38kg @LNGS), ArDM (800 kg @CANFRANC) CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 14 Noble liquid detectors : recent results Xe XENON-1t (2018) 1 t*y current best limit Ar in high-mass region (2018) DakSide-50 PSD Parameter 16660 kg*d UAr WIMP region background-free result (using PSD) Ar DakSide-50 (2018) 6786 kg*d UAr current best limit 1.8-6 GeV/c2 (ionisation only) à talk by D. Thers à talk by D. Franco CS IN2P3, 25/10/2018 A. Tonazzo - World context for direct dark matter searches 15 Noble liquid detectors : future perspectives -�� -� High-mass WIMPs �� �� -�� -� �� ������ �� Muli-ton (2020-2025) ������ - ] ��� ] • Lux-ZePlin (LZ) � ��-�� ��-� - ����� -�� �� 10t LXe @SURF �� [ �� �������� � • XENON-nT [ -�� �� -� �� �� �� ��� �� -���� 8t LXe @LNGS ���� σ σ - � -�� • DarkSide-20k ��-�� �������� ��-� 20t DAr @LNGS ��-�� ��-� ��� ������� ������� global efforts (>2025) - - • DARWIN 50t LXe ��-�� ������� ��-�� • GADMC 300t DAr �� -�� ����� -�� �� ��������������� �� -�� ������ -�� �� �� ����
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]
  • 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]
  • 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]
  • 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]
  • Direct Detection of Dark Matter
    Bernard Sadoulet Dept. of Physics /LBNL UC Berkeley UC Institute for Nuclear and Particle Astrophysics and Cosmology (INPAC) Direct Detection of Dark Matter Four broad classes of models Situation May 2017 Low mass, DAMA High WIMP Mass Noble liquids PICO Low WIMP Mass Low temperature detectors Super CDMS Gas Further in the future at very low mass PATRAS May 17, 2017 1 B.Sadoulet The Emerging Mystery of Dark Matter From Zwicky (1933), Vera Rubin (1970), Faber-Gallagher (1979) =>Convincing evidence for dark matter http://physics.ucsc.edu/~joel/Ay/214/Jan12-Primack-DM-History.pdf Clusters 26 % 69.1 % The Ultimate Copernican Revolution ≠ Not made of ordinary matter! (Big Bang Nucleothesis, CMB) Somewhat eclipsed by the discovery of Dark Energy 1998 Standard Cosmological model Lambda CDM! Not light neutrinos! “Cold”=non relativistic at time of galaxy formation. Extremely successful. No unambiguous sign of special properties Dwarf galaxies: core, too big to fail? Likely “gastrophysics" PATRAS May 17, 2017 2 B.Sadoulet 4 Complementary Approaches LHC Cosmological Observations Planck Dark Matter Keck telescopes Galactic Halo (simulation) WIMP production on Earth VERITAS, also HESS, Magic + IceCube (v) CDMS WIMP annihilation in the cosmos GLAS Fermi/GLAST T WIMP scattering on Earth:e.g. Super CDMS,LUX etc. PATRAS May 17, 2017 33 B.Sadoulet Four Classes of Particle Dark Matter Could detect these by scattering of Particles in thermal equilibrium + decoupling when non- galactic dark matter on a suitable target in laboratory relativistic Freeze out when annihilation rate ≈ expansion rate 3⋅10-27 cm3 / s α 2 ⇒ Ω h2 = Ω ≈ 25% ⇒ σ ≈ DM v DM A M 2 σ A EW Cosmology points to W&Z scale Inversely standard particle model requires new physics at this scale => significant amount of dark matter Weakly Interacting Massive Particles Problem: not (yet?) seen yet at the LHC A dark sector which could be as complex as matter sector Self interacting dark matter, dark photon etc.
    [Show full text]
  • Dark Matter 1 25
    25. Dark matter 1 25. DARK MATTER Revised September 2015 by M. Drees (Bonn University) and G. Gerbier (Queen’s University, Canada). 25.1. Theory 25.1.1. Evidence for Dark Matter : The existence of Dark (i.e., non-luminous and non-absorbing) Matter (DM) is by now well established [1,2]. The earliest, and perhaps still most convincing, evidence for DM came from the observation that various luminous objects (stars, gas clouds, globular clusters, or entire galaxies) move faster than one would expect if they only felt the gravitational attraction of other visible objects. An important example is the measurement of galactic rotation curves. The rotational velocity v of an object on a stable Keplerian orbit with radius r around a galaxy scales like v(r) M(r)/r, where p M(r) is the mass inside the orbit. If r lies outside the visible part of the∝ galaxy and mass tracks light, one would expect v(r) 1/√r. Instead, in most galaxies one finds that v becomes approximately constant out∝ to the largest values of r where the rotation curve can be measured; in our own galaxy, v 240 km/s at the location of our solar system, with little change out to the largest observable≃ radius. This implies the existence of a dark halo, with mass density ρ(r) 1/r2, i.e., M(r) r; at some point ρ will have to fall off faster (in order to keep the∝ total mass of the galaxy∝ finite), but we do not know at what radius this will happen.
    [Show full text]
  • Arxiv:2012.02436V5 [Physics.Ins-Det] 18 May 2021
    Prepared for submission to JINST Design and Commissioning of the PandaX-4T Cryogenic Distillation System for Krypton and Radon Removal Xiangyi Cui,0,2 Zhou Wang,1,2,1 Yonglin Ju3,1 Xiuli Wang,3 Huaxuan Liu,3 Wenbo Ma,1 Jianglai Liu,0,1,2 Li Zhao,1,2 Xiangdong Ji0,1,4 Shuaijie Li,0 Rui Yan,3 Haidong Sha,3 Peiyao Huang,3 Jifang Zhou, 5 Changsong Shang, 5 Liqiang Liu 5 0Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai 200240, China 1INPAC and School of Physics and Astronomy, Shanghai Jiao Tong University, Shanghai Laboratory for Particle Physics and Cosmology, Shanghai 200240, China 2Shanghai Jiao Tong University Sichuan Research Institute, Chengdu 610000, China 3Institute of Refrigeration and Cryogenics, Shanghai Jiao Tong University Shanghai 200240, China 4Department of Physics, University of Maryland, College Park, Maryland 20742, USA 5 Yalong River Hydropower Development Company, Ltd., Chengdu 610051, China E-mail: [email protected], [email protected] Abstract: An online cryogenic distillation system for the removal of krypton and radon from xenon was designed and constructed for PandaX-4T, a highly sensitive dark matter detection experiment. The krypton content in a commercial xenon product is expected to be reduced by 7 orders of magnitude with 99% xenon collection efficiency at a flow rate of 10 kg/h by design. The same system can reduce radon content in xenon by reversed operation, with an expected radon reduction factor of about 1.8 in PandaX-4T under a flow rate of 56.5 kg/h. The commissioning of this system was completed, with krypton and radon operations tested under respective working conditions.
    [Show full text]
  • Recent Results from XMASS
    Recent results from XMASS Katsuki Hiraide (ICRR, the University of Tokyo) June 19-23, 2017 WIN2017@Irvine 1 Outline • The XMASS experiment • Recent dark matter results – Annual modulation search [Phys. Lett. B759 (2016)272-276] – WIMPs search by fiducialization New results !! • Supernova neutrino detection via coherent scattering [Astropart. Phys. 89 (2017) 51-59] • Summary 2 KamLAND The XMASS project Super-Kamiokande XMASS: a multi purpose experiment with liquid xenon CANDLES XMASS E-GADS Located 1,000 m underground (2,700 m.w.e.) at the Kamioka Observatory in Japan NEWAGE CLIO Aiming for Direct detection of dark matter Observation of low energy solar neutrinos (pp/7Be) Search for neutrino-less double beta decay Features Low energy threshold (~0.5keVee) Sensitive to e/g events as well as nuclear recoil Large target mass and its scalability 3 Single-phase liquid Xenon detector: XMASS-I Liquid xenon detector 832 kg of liquid xenon (-100 oC) 642 2-inch PMTs (Photocathode coverage >62%) Each PMT signal is recorded by 10-bit 1GS/s waveform digitizers 80cm Water Cherenkov detector 10m diameter, 11m high 11m 72 20-inch PMTs Active shield for cosmic-ray muons Passive shield for n/g 10m 4 Diversity of physics target with XMASS Dark matter searches Solar axion search Possibility of supernova Low mass WIMP search WIMP-129Xe inelastic scattering Phys. Lett. B724 (2013) 46 neutrino detection Phys. Lett. B719 (2013) 78 PTEP (2014) 063C01 Astropart. Phys. 89 (2017) 51 XMASS (90%CL) DAMA LXe (90%CL) Supernova at 10kpc (Livermore model) XMASS XMASS Expected signal Background Bosonic super-WIMPs search Annual modulation search Search for 2n double electron capture on 124Xe, 126Xe Phys.
    [Show full text]
  • How Zwicky Already Ruled out Modified Gravity Theories Without Dark Matter
    How Zwicky already ruled out modified gravity theories without dark matter Theodorus Maria Nieuwenhuizen1,2 1Institute for Theoretical Physics, University of Amsterdam, Science Park 904, 1090 GL Amsterdam, The Netherlands 2International Institute of Physics, UFRG, Lagoa Nova, Natal - RN, 59064-741, Brazil Various theories, such as MOND, MOG, Emergent Gravity and f(R) theories avoid dark matter by assuming a change in General Relativity and/or in Newton’s law. Galactic rotation curves are typically described well. Here the application to galaxy clusters is considered, focussed on the good lensing and X-ray data for A1689. As a start, the no-dark-matter case is confirmed to work badly: the need for dark matter starts near the cluster centre, where Newton’s law is still supposed to be valid. This leads to the conundrum discovered by Zwicky, which is likely only solvable in his way, namely by assuming additional (dark) matter. Neutrinos with eV masses serve well without altering the successes in (dwarf) galaxies. Keywords: MOND, MOG, f(R), Emergent Gravity, galaxy cluster, Abell 1689, dark matter, neutrinos I. INTRODUCTION Niets is gewichtiger dan donkere materie52 Dark matter enters the light in 1922 when Jacobus Kapteyn employs this term in his First Attempt at a Theory of the Arrangement and Motion of the Sidereal System1. It took a decade for his student Jan Oort to work out the stellar motion perpendicular to the Galactic plane, and to conclude that invisible mass should exist to keep the stars bound to the plane2. Next year, in 1933, Fritz Zwicky applied the idea to the Coma galaxy cluster and concluded that it is held together by dark matter.
    [Show full text]