Jianglai Liu Shanghai Jiao Tong University
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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 -
European Astroparticle Physics Strategy 2017-2026 Astroparticle Physics European Consortium
European Astroparticle Physics Strategy 2017-2026 Astroparticle Physics European Consortium August 2017 European Astroparticle Physics Strategy 2017-2026 www.appec.org Executive Summary Astroparticle physics is the fascinating field of research long-standing mysteries such as the true nature of Dark at the intersection of astronomy, particle physics and Matter and Dark Energy, the intricacies of neutrinos cosmology. It simultaneously addresses challenging and the occurrence (or non-occurrence) of proton questions relating to the micro-cosmos (the world decay. of elementary particles and their fundamental interactions) and the macro-cosmos (the world of The field of astroparticle physics has quickly celestial objects and their evolution) and, as a result, established itself as an extremely successful endeavour. is well-placed to advance our understanding of the Since 2001 four Nobel Prizes (2002, 2006, 2011 and Universe beyond the Standard Model of particle physics 2015) have been awarded to astroparticle physics and and the Big Bang Model of cosmology. the recent – revolutionary – first direct detections of gravitational waves is literally opening an entirely new One of its paths is targeted at a better understanding and exhilarating window onto our Universe. We look of cataclysmic events such as: supernovas – the titanic forward to an equally exciting and productive future. explosions marking the final evolutionary stage of massive stars; mergers of multi-solar-mass black-hole Many of the next generation of astroparticle physics or neutron-star binaries; and, most compelling of all, research infrastructures require substantial capital the violent birth and subsequent evolution of our infant investment and, for Europe to remain competitive Universe. -
Small Scale Problems of the CDM Model
galaxies Article Small Scale Problems of the LCDM Model: A Short Review Antonino Del Popolo 1,2,3,* and Morgan Le Delliou 4,5,6 1 Dipartimento di Fisica e Astronomia, University of Catania , Viale Andrea Doria 6, 95125 Catania, Italy 2 INFN Sezione di Catania, Via S. Sofia 64, I-95123 Catania, Italy 3 International Institute of Physics, Universidade Federal do Rio Grande do Norte, 59012-970 Natal, Brazil 4 Instituto de Física Teorica, Universidade Estadual de São Paulo (IFT-UNESP), Rua Dr. Bento Teobaldo Ferraz 271, Bloco 2 - Barra Funda, 01140-070 São Paulo, SP Brazil; [email protected] 5 Institute of Theoretical Physics Physics Department, Lanzhou University No. 222, South Tianshui Road, Lanzhou 730000, Gansu, China 6 Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa, Faculdade de Ciências, Ed. C8, Campo Grande, 1769-016 Lisboa, Portugal † [email protected] Academic Editors: Jose Gaite and Antonaldo Diaferio Received: 30 May 2016; Accepted: 9 December 2016; Published: 16 February 2017 Abstract: The LCDM model, or concordance cosmology, as it is often called, is a paradigm at its maturity. It is clearly able to describe the universe at large scale, even if some issues remain open, such as the cosmological constant problem, the small-scale problems in galaxy formation, or the unexplained anomalies in the CMB. LCDM clearly shows difficulty at small scales, which could be related to our scant understanding, from the nature of dark matter to that of gravity; or to the role of baryon physics, which is not well understood and implemented in simulation codes or in semi-analytic models. -
Light Dark Matter in a Minimal Extension with Two Additional Real Singlets
PHYSICAL REVIEW D 103, 015010 (2021) Light dark matter in a minimal extension with two additional real singlets Markos Maniatis * Centro de Ciencias Exactas and Departamento de Ciencias Básicas, UBB, Avenida Andres Bello 720, 3780000 Chillán, Chile (Received 24 August 2020; accepted 12 December 2020; published 8 January 2021) The direct searches for heavy scalar dark matter with a mass of order 100 GeV are much more sensitive than for light dark matter of order 1 GeV. The question arises whether dark matter could be light and has escaped detection so far. We study a simple extension of the Standard Model with two additional real singlets. We show that this simple extension may provide the observed relic dark matter density, does neither disturb big bang nucleosynthesis nor the cosmic microwave background radiation observations, and fulfills the conditions of clumping behavior for different sizes of Galaxies. The potential of one Standard Model–like Higgs-boson doublet and the two singlets gives rise to a changed Higgs phenomenology, in particular, an enhanced invisible Higgs-boson decay rate is expected, detectable by missing transversal momentum searches at the ATLAS and CMS experiments at CERN. DOI: 10.1103/PhysRevD.103.015010 I. INTRODUCTION collisions. In particular, in this way a DM candidate may enhance the invisible decay rate of a SM-like Higgs boson. Recently it has been reported [1] that the NGC1052–DF2 Note that in the SM the only invisible decay channel of galaxy with a stellar mass of approximately 2 × 108 solar the Higgs boson (h) is via two electroweak Z bosons masses has a rotational movement in accordance with its which subsequently decay into pairs of neutrinos (ν), that observed mass. -
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 • -
Dark Matter Direct Detection with Edelweiss-II
Dark matter direct detection with Edelweiss-II Eric Armengaud - CEA / IRFU Blois 2008 http://edelweiss2.in2p3.fr/ 1 Direct detection of dark matter : principles . A well-identified science goal: Detect the nuclear recoil of local WIMPs inside some material Target the electroweak interaction scale, m ~ GeV-TeV At least 3 strategies: Search for a global recoil spectrum V(Earth/Sun): Search for a - small - annual modulation V(Sun/Wimp gaz): Search for a - large - forward/backward asymetry Remove backgrounds!!! Go deep underground Use several passive shields Develop smart detectors to identify the remaining radioactivity interactions 2 Direct detection of dark matter . A well-identified science goal: Detect the nuclear recoil of local WIMPs inside some material Target the electroweak interaction scale, m ~ GeV-TeV At least 3 strategies: Search for a global recoil spectrum • Cryogenic bolometers: CDMS, CRESST, EDELWEISS… • Liquid noble elements: XENON, LUX, ZEPLIN, WARP, ArDM… • Superheated liquids: COUPP, PICASSO, SIMPLE… • Solid scintillator (DAMA, KIMS), low- threshold Ge (TEXONO), gaz detector (DRIFT)… A very active field with both R&D and large-scale setups 3 The XENON10 experiment • Quite easily scalable, « high » temperatures • First scintillation pulse (S1) + Second pulse due to e- extraction to the gaz (S2) ⇒ Nuclear recoil discrimination - especially @ low E • Position measurements ⇒ Fiducial cut (~5kg) • Low-energy threshold + Xe mass ⇒ sensitivity to low-mass Wimps Electronic recoils Nuclear recoil region But : not background-free -
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. -
Self-Interacting Inelastic Dark Matter: a Viable Solution to the Small Scale Structure Problems
Prepared for submission to JCAP ADP-16-48/T1004 Self-interacting inelastic dark matter: A viable solution to the small scale structure problems Mattias Blennow,a Stefan Clementz,a Juan Herrero-Garciaa; b aDepartment of physics, School of Engineering Sciences, KTH Royal Institute of Tech- nology, AlbaNova University Center, 106 91 Stockholm, Sweden bARC Center of Excellence for Particle Physics at the Terascale (CoEPP), University of Adelaide, Adelaide, SA 5005, Australia Abstract. Self-interacting dark matter has been proposed as a solution to the small- scale structure problems, such as the observed flat cores in dwarf and low surface brightness galaxies. If scattering takes place through light mediators, the scattering cross section relevant to solve these problems may fall into the non-perturbative regime leading to a non-trivial velocity dependence, which allows compatibility with limits stemming from cluster-size objects. However, these models are strongly constrained by different observations, in particular from the requirements that the decay of the light mediator is sufficiently rapid (before Big Bang Nucleosynthesis) and from direct detection. A natural solution to reconcile both requirements are inelastic endothermic interactions, such that scatterings in direct detection experiments are suppressed or even kinematically forbidden if the mass splitting between the two-states is sufficiently large. Using an exact solution when numerically solving the Schr¨odingerequation, we study such scenarios and find regions in the parameter space of dark matter and mediator masses, and the mass splitting of the states, where the small scale structure problems can be solved, the dark matter has the correct relic abundance and direct detection limits can be evaded. -
Prospects for Dark Matter Detection with Inelastic Transitions of Xenon
Prospects for dark matter detection with inelastic transitions of xenon Christopher McCabe GRAPPA Centre for Excellence, Institute for Theoretical Physics Amsterdam (ITFA), University of Amsterdam, Science Park 904, the Netherlands E-mail: [email protected] Abstract. Dark matter can scatter and excite a nucleus to a low-lying excitation in a direct detection experiment. This signature is distinct from the canonical elastic scattering signal because the inelastic signal also contains the energy deposited from the subsequent prompt de-excitation of the nucleus. A measurement of the elastic and inelastic signal will allow a single experiment to distinguish between a spin-independent and spin-dependent interaction. For the first time, we characterise the inelastic signal for two-phase xenon de- tectors in which dark matter inelastically scatters off the 129Xe or 131Xe isotope. We do this by implementing a realistic simulation of a typical tonne-scale two-phase xenon detector and by carefully estimating the relevant background signals. With our detector simulation, we explore whether the inelastic signal from the axial-vector interaction is detectable with upcoming tonne-scale detectors. We find that two-phase detectors allow for some discrim- ination between signal and background so that it is possible to detect dark matter that inelastically scatters off either the 129Xe or 131Xe isotope for dark matter particles that are heavier than approximately 100 GeV. If, after two years of data, the XENON1T search for elastic scattering nuclei finds no evidence for dark matter, the possibility of ever detecting arXiv:1512.00460v2 [hep-ph] 23 May 2016 an inelastic signal from the axial-vector interaction will be almost entirely excluded. -
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 -
Isospin Violating Dark Matter
Isospin Violating Dark Matter David Sanford Work with J.L. Feng, J. Kumar, and D. Marfatia UC Irvine Pheno 2011 - Tuesday May 10, 2011 Current State of Light Dark Matter I Great recent interest in CoGeNT light dark matter DAMA (Savage et. al.) CDMS-Si (shallow-site) I Major inconsistencies CDMS-Ge(shallow-site) CDMS-Ge (Soudan) between experimental XENON1 (! 11) XENON10 (! 11) results I DAMA and CoGeNT regions do not agree I XENON10/XENON100 rule out DAMA and CoGeNT I CDMS-Ge (Soudan) rules out much of CoGeNT and all of DAMA I Both DAMA and CoGeNT report annual modulation signals Possible Explanations of the Discrepancy Many theories have been put forward I Inelastic dark matter I Tucker-Smith and Weiner (2001) I Details of Leff in liquid xenon at low recoil energy I Collar and McKinsey (2010) I Channeling in NaI at DAMA I Bernabei et. al. [DAMA] (2007); Bozorgnia, Gelmini, Gondolo (2010) We propose to rescind the assumption of isospin conservation I Unfounded theoretical assumption I Simple resolution of several discrepancies I Also considered by Chang, Liu, Pierce, Weiner, Yavin (2010) I For fp 6= fn, this result must be altered Z I In fact, for fn=fp = − A−Z , σA vanishes from completely destructive interference Z I A−Z decreases for higher Z isotopes Isospin Conservation and Violation I DM-nucleus scattering is Dark Matter Compton Wavelength coherent I The single atom SI scattering cross-section is Nucleus 2 σA / [fpZ + fn(A − Z)] 2 2 / fp A (fp = fn) Z : atomic number A: number of nucleons 2 I Well-known A fp: coupling to protons -
Astrophysical Issues in Indirect DM Detection
Astrophysical issues in indirect DM detection Julien Lavalle CNRS Lab. Univers & Particules de Montpellier (LUPM), France Université Montpellier II – CNRS-IN2P3 (UMR 5299) Max-Planck-Institut für Kernphysik Heidelberg – 1st VII 2013 Outline * Introduction * Practical examples of astrophysical issues (at the Galactic scale) => size of the GCR diffusion zone: relevant to antiprotons, antideuterons, (diffuse gamma-rays) => positron fraction: clarifying the role of local astrophysical sources => impact of DM inhomogeneities: boost + reinterpreting current constraints => diffuse gamma-rays * Perspectives Julien Lavalle, MPIK, Heidelberg, 1st VII 2013 Indirect dark matter detection in the Milky Way Main arguments: But: ● Annihilation final states lead to: gamma-rays + antimatter ● Do we control the backgrounds? ● -rays : lines, spatial + spectral distribution of signals vs bg ● γ Antiprotons are secondaries, not necessarily positrons ● Antimatter cosmic rays: secondary, therefore low bg ● Do the natural DM particle models provide clean signatures? ● DM-induced antimatter has specific spectral properties Julien Lavalle, MPIK, Heidelberg, 1st VII 2013 Indirect dark matter detection in the Milky Way Main arguments: But: ● Annihilation final states lead to: gamma-rays + antimatter ● Do we control the backgrounds? ● -rays : lines, spatial + spectral distribution of signals vs bg ● γ Antiprotons are secondaries, not necessarily positrons ● Antimatter cosmic rays: secondary, therefore low bg ● Do the natural DM particle models provide clean signatures?