DOCSLIB.ORG

Non-Collider Projekte

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Non-Collider Projekte KET Jahrestreffen Bad Honnef, 19.11.2016 Christoph Rembser (CERN) This alk is mainly based on the “Physics beyond colliders kick-off workshop” (PBC) at CERN, September 2016, see https://indico.cern.ch/event/523655/ Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 1 New physics, experimentally Precision Frontier* Figure by Mikhail Shaposhnikov “New Physics below the Fermi Scale” at the Physics Beyond Colliders Kickoff workshop *added by CR 19.11.2016 Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 2 Active fundamental particle physics programme next to LHC Approved Experiments, reviewed by the CERN SPS and PS Experiments Committee (SPSC), Status Nov. 2016 Experiment Description Comment Example: CERN AD2 (ATRAP) Precise laser or microwave spectroscopy of trapped antihydrogen AD3 (ASACUSA) Atomic Spectroscopy And Collisions Using Slow Antiprotons non-collider AD4 (ACE) Relative Biological Effectiveness of Antiproton Annihilation finished data taking AD5 (ALPHA) AD Antihydrogen spectroscopy experiments/ AD6 (AEGIS) Testing gravity with antimatter AD7 (GBAR) Testing gravity with antimatter AD8 (BASE) Comparisons of the fundamental properties of antiprotons and protons proposals, PS212 (DIRAC) Observation of mesonic atoms and tests of low energy QCD finished data taking PS PS215 (CLOUD) Influence of galactic cosmic rays (GCRs) on aerosols and clouds status Nov.2016 NA58 (COMPASS) Study of hadron structure and hadron spectroscopy NA61 (SHINE) Strong interactions, neutrinos and cosmic rays NA62 Measuring rare kaon decays NA63 SPS Electromagnetic Processes in strong Crystalline Fields NA64 Search for dark sectors in missing energy events UA9 (CRYSTAL) Crystal Channeling AWAKE Advanced Proton-Driven Plasma Wakefield Acceleration Experiment WA104 (NP01) Refurbishment of the ICARUS Detector ProtoDUNE-DP (NP02) Neutrino Prototype of a Double-Phase Liquid Argon TPC for DUNE ProtoDUNE-SP (NP04) Facility Prototype of a Single-Phase Liquid Argon TPC for DUNE Baby MIND (NP05) Prototype of a Magnetized Iron Neutrino Detector CAST non-accel. Search for Axions and Axion-like particles OSQAR Experiments Search for QED vacuum magnetic birefringence, Axions and photon Regeneration CNGS1 (OPERA) Neutrino oscillation experiment at LNGS finished data taking CNGS CNGS2 (ICARUS) Neutrino oscillation experiment at LNGS finished data taking Proposed Experiments, LoI, EoI, Proposal, TDR to the SPSC, Status Nov. 2016 ALPHA-g (P) AD Testing gravity with antimatter IAXO (I) non-accel. Search for axions or axion-like particles (ALPs) originating in the Sun via the Primakoff conversion SHIP (P) SPS General purpose fixed target facility at the CERN SPS accelerator exploring the domain of hidden particles P349 PS Search for polarization effects in the antiproton production process ENUBET (EOI) SPS/PS New methods for precise measurements of flux in accelerator neutrino beams SHIP/NA61 (EOI) SPS μ-flux measurements for SHiP using NA61/SHINE I245 (LOI) SPS Study of nu_tau production by measuring Ds ->tau: test of lepton universality in neutrino CC interactions EOI012 SPS Measurement of Short Living Baryon Magnetic Moment using bent crystals at SPS and LHC CR, Nov 2016 Scientific programmes of CERN non-collider experiments approved/reviewed by the SPSC up to LS2 Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 3 Neutrino masses - Fundamental Current strongest mass limit for lightest neutrino: electron anti-neutrino < 2.2 eV, future goals: 200meV Direct neutrino mass measurements: kinematic approach by measuring Beta decay of 3H or electron capture in 163HO; • Ho3H-based experiments: KATRIN, Project8, PTOLEMY; • 163Ho-based experiments ECHo, HOLMES, NuMECS; Some experiments need very sensitive temperature sensors, e.g. low temperature micro-calorimeters: → very small volume; → Working temperature below 100 mK, thus small specific heat and small thermal noise. E.G. HOLMES: Transition Edge Sensors HOLMES 4✕16 linear sub-array Technology interesting Absorber for other detectors! Sensor ΔE≈1eV and τ≈1μs Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 4 Dark Matter searches • Wide field of searches, many experiments, among for direct and indirect detection: Annual modulation with NAI Scintillators (ANAIS), Argon Dark Matter experiment (ArDM), Axion Dark Matter Experiment (ADMX), Chicagoland Observatory for Underground Particle Physics (COUPP), CDEX (China Dark matter Experiment), PANDA-X (Particle AND Astroparticle with Xenon), and TEXONO (Taiwan EXperiment On NeutrinO) Experiments, CoGeNT, Cryogenic Dark Matter Search (CDMS/SuperCDMS), Cryogenic Rare Event Search with Superconducting Thermometers (CRESST), DAMA/LIBRA, Dark Matter WIMP Search in Noble Liquids (DARWIN), Dark Matter Search Experiment with Liquid Argon Pulse Shape Discrimination (DEAP), DarkSide, Experiment for Direct Detection of WIMP Dark Matter (EDELWEISS), European Underground Rare Event Calorimeter Array (EURECA), Finding U(1)s of a Novel Kind (FUNK), Korea Invisible Mass Search (KIMS), Large Hadron Collider (LHC), LUX-ZEPLIN (LZ), Project In Canada to Search for Supersymmetric Objects (PICASSO), Superheated Instrument for Massive Particle Experiments (SIMPLE), XENON 100, XMASS, Alpha Magnetic Spectrometer (AMS), Any Light Particle Search (ALPS I and ALPS II), Astronomy with a Neutrino Telescope and Abyss environmental RESearch (ANTARES), BAIKAL Neutrino Telescope, The Cherenkov Telescope Array (CTA), Fermi Gamma-ray Space Telescope-Large Area Telescope (FGST-LAT), General Antiparticle Spectrometer (GAPS), Heavy Photon Search (HPS), High Energy Stereoscopic System (HESS), IceCube Neutrino Observatory, The Isotope Matter Antimatter Experiment (IMAX), The Major Atmospheric Gamma-ray Imaging Cherenkov Telescopes (MAGIC), Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA), Super-Kamiokande (SK), Very Energetic Radiation Imaging Telescope Array System (VERITAS). interactions.org Dark Matter Hub, …very nice overview at see http://www.interactions.org/cms/?pid=1034004 Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 5 Facilities at the CERN PS: the Antiproton Decelerator AD AD: low-energy antiprotons (5.3MeV/c, 3 107 per cycle) for studies of antimatter. Upgrade: additional ELENA (Extra Low ENergy Antiproton) ring providing 100 keV antiprotons. Experiments: ~100 times more particles per unit time. AD Experiments: ATRAP (spectroscopy and p_bar magnetic moment), ALPHA (spectroscopy), ASACUSA (spectroscopy, atomic and nuclear collision cross sections), BASE (p_bar magnetic moment), AeGIS, GBAR and (t.b.appr.) ALPHA-g (antimatter gravity experiments) Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 6 @AD: the BASE experiment Precise comparisons of the fundamental properties of pbar and p by measuring the cyclotron and Larmor frequencies of single trapped (anti)protons (optionally H-). Goal until 2018 : measurement of magnetic moment of the (anti)proton with precision of δg/g 10−9 (~factor1000 w.r.t. ATRAP measurement, Phys. Rev. Lett. 110, 130801 – March 2013); ➡ Letter of Intent to SPS and PS Experiments Committee (SPSC) June 2012, Technical Design Report to SPSC January 2013; ➡ Recommended by SPSC and approved by the CERN Research Board: June 2013 Example on how fast things can move forward! ➡ Operation and first results: 2014. N.B.: currently BASE is still running with pbars caught in November 2015. C. Smorra et al., A reservoir trap for antiprotons, Int. Journ. Mass. Spec. 389, 10 (2015). Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 7 @AD: BASE (2) All measured antiproton-to-H- cyclotron frequency ratios as a function of time. 6,521 ratios were measured in 35days. single H- ion single antiproton • FIRST measurement with the new apparatus: high precision comparison of the antiproton-to-proton charge-to mass ratio by comparing cyclotron frequencies of antiproton an hydrogen ions in a Penning trap, Nature. 2015;524:196–199; • 69ppt comparison of the proton/antiproton Q/M ratio ➡ succeeding Gabrielse, G. et al. “Precisionmass spectroscopy of the antiproton and proton using simultaneously trapped particles. Phys. Rev. Lett. 82, 3198–3201 (1999); ➡ currently most precise test of CPT invariance with baryons. Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 8 Precise measurement of electric dipole moment EDM describes the positive and negative charge distribution inside a particle. Aligns along the spin axis of the particle, and violates both Parity and Time Reversal. • EDM measurement requires trapping the particle/atom for a long time, e.g. in storage rings; • EDM of neutron is measured - direct measurement of charged ion EDM not yet been performed; Idea presented at PBC: Pure Electrostatic Storage Ring for proton EDM -29 • 10 e cm sensitivity would correspond to 100 TeV for new physics energy scale, pure electrostatic ring applicable to proton only. talks by Themis at PBC Bowcock workshop and ➣ Mei Bai Non-Collider Projekte - KET Jahrestreffen, 19 November 2016 Christoph Rembser 9 Mu3E Experiment at PSI • Search for lepton flavour violating decay (A.Blondel et al., arXiv:1301.6113) ➡ BR(μ+ → e+ e+ e- ) < 10-12 (SINDRUM 1986) ➡ BR(μ+ → e+ e+ e- ) < 10-15 (phase I, PiE5 beamline) ➡ BR(μ+ → e+ e+ e- ) < 10-16 (phase II, High Intensity Muon beamline) ➣ see http://www.physi.uni-heidelberg.de/Forschung/he/mu3e/ Main technological Challenges:
Recommended publications
  • A Spectrometer for Proton Driven Plasma Accelerated Electrons at Awake - Recent Developments∗

    A Spectrometer for Proton Driven Plasma Accelerated Electrons at Awake - Recent Developments∗

    Proceedings of IPAC2016, Busan, Korea WEPMY024 A SPECTROMETER FOR PROTON DRIVEN PLASMA ACCELERATED ELECTRONS AT AWAKE - RECENT DEVELOPMENTS∗ Lawrence Charles Deacon, Simon Jolly, Fearghus Keeble, UCL, London Aurélie Goldblatt, Stefano Mazzoni, Alexey Petrenko, CERN, Geneva Bartolomej Biskup, CERN, Geneva; Czech Technical University, Prague 6 Matthew Wing, UCL, London; DESY, Hamburg; University of Hamburg, Hamburg Abstract SPECTROMETER DESIGN The AWAKE experiment is to be constructed at the CERN Neutrinos to Gran Sasso facility (CNGS). This will be the first experiment to demonstrate proton-driven plasma wake- field acceleration. The 400 GeV proton beam from the CERN SPS will excite a wakefield in a plasma cell several meters in length. To probe the plasma wakefield, electrons of 10–20 MeV will be injected into the wakefield follow- ing the head of the proton beam. Simulations indicate that electrons will be accelerated to GeV energies by the plasma wakefield. The AWAKE spectrometer is intended to measure both the peak energy and energy spread of these accelerated electrons. Results of beam tests of the scintillator screen Figure 1: A 3D CAD image of the spectrometer system output are presented, along with tests of the resolution of annotated with distances along the z direction from the exit the proposed optical system. The results are used together of the plasma cell to the magnetic centers of magnets, and with a BDSIM simulation of the spectrometer system to pre- the center of the scintillator screen. dict the spectrometer performance for a range of possible accelerated electron distributions. INTRODUCTION RESOLUTION Proton bunches are the most promising drivers of wake- Optical System fields to accelerate electrons to the TeV energy scale in a The resolution of the energy spectrometer will ultimateley single stage.
  • European Astroparticle Physics Strategy 2017-2026 Astroparticle Physics European Consortium

    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.
  • Proton Driven Plasma Wakefield Acceleration in AWAKE

    Proton Driven Plasma Wakefield Acceleration in AWAKE

    Proton Driven Plasma Article submitted to journal Wakefield Acceleration in Subject Areas: AWAKE Plasma Wakefield Acceleration, 1 1 Proton Driven, Electron Acceleration E. Gschwendtner , M. Turner , **Author List Continues Next Page** Keywords: AWAKE, Plasma Wakefield Acceleration, Seeded Self Modulation In this article, we briefly summarize the experiments Author for correspondence: performed during the first Run of the Advanced Insert corresponding author name Wakefield Experiment, AWAKE, at CERN (European e-mail: [email protected] Organization for Nuclear Research). The final goal of AWAKE Run 1 (2013 - 2018) was to demonstrate that 10-20 MeV electrons can be accelerated to GeV- energies in a plasma wakefield driven by a highly- relativistic self-modulated proton bunch. We describe the experiment, outline the measurement concept and present first results. Last, we outline our plans for the future. 1 Continued Author List 2 E. Adli2,A. Ahuja1,O. Apsimon3;4,R. Apsimon3;4, A.-M. Bachmann1;5;6,F. Batsch1;5;6 C. Bracco1,F. Braunmüller5,S. Burger1,G. Burt7;4, B. Buttenschön8,A. Caldwell5,J. Chappell9, E. Chevallay1,M. Chung10,D. Cooke9,H. Damerau1, L.H. Deubner11,A. Dexter7;4,S. Doebert1, J. Farmer12, V.N. Fedosseev1,R. Fiorito13;4,R.A. Fonseca14,L. Garolfi1,S. Gessner1, B. Goddard1, I. Gorgisyan1,A.A. Gorn15;16,E. Granados1,O. Grulke8;17, A. Hartin9,A. Helm18, J.R. Henderson7;4,M. Hüther5, M. Ibison13;4,S. Jolly9,F. Keeble9,M.D. Kelisani1, S.-Y. Kim10, F. Kraus11,M. Krupa1, T. Lefevre1,Y. Li3;4,S. Liu19,N. Lopes18,K.V. Lotov15;16, M. Martyanov5, S.
  • Light Dark Matter in a Minimal Extension with Two Additional Real Singlets

    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.
  • Dark Matter Direct Detection with Edelweiss-II

    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
  • The AWAKE Acceleration Scheme for New Particle Physics Experiments at CERN

    The AWAKE Acceleration Scheme for New Particle Physics Experiments at CERN

    AWAKE++: the AWAKE Acceleration Scheme for New Particle Physics Experiments at CERN W. Bartmann1, A. Caldwell2, M. Calviani1, J. Chappell3, P. Crivelli4, H. Damerau1, E. Depero4, S. Doebert1, J. Gall1, S. Gninenko5, B. Goddard1, D. Grenier1, E. Gschwendtner*1, Ch. Hessler1, A. Hartin3, F. Keeble3, J. Osborne1, A. Pardons1, A. Petrenko1, A. Scaachi3, and M. Wing3 1CERN, Geneva, Switzerland 2Max Planck Institute for Physics, Munich, Germany 3University College London, London, UK 4ETH Zürich, Switzerland 5INR Moscow, Russia 1 Abstract The AWAKE experiment reached all planned milestones during Run 1 (2016-18), notably the demon- stration of strong plasma wakes generated by proton beams and the acceleration of externally injected electrons to multi-GeV energy levels in the proton driven plasma wakefields. During Run 2 (2021 - 2024) AWAKE aims to demonstrate the scalability and the acceleration of elec- trons to high energies while maintaining the beam quality. Within the Physics Beyond Colliders (PBC) study AWAKE++ has explored the feasibility of the AWAKE acceleration scheme for new particle physics experiments at CERN. Assuming continued success of the AWAKE program, AWAKE will be in the position to use the AWAKE scheme for particle physics ap- plications such as fixed target experiments for dark photon searches and also for future electron-proton or electron-ion colliders. With strong support from the accelerator and high energy physics community, these experiments could be installed during CERN LS3; the integration and beam line design show the feasibility of a fixed target experiment in the AWAKE facility, downstream of the AWAKE experiment in the former CNGS area. The expected electrons on target for fixed target experiments exceeds the electrons on target by three to four orders of magnitude with respect to the current NA64 experiment, making it a very promising experiment in the search for new physics.
  • AWAKE! Allen Caldwell Even Larger Accelerators ?

    AWAKE! Allen Caldwell Even Larger Accelerators ?

    Swapan Chattopadhyay Symposium April 30, 2021 AWAKE! Allen Caldwell Even larger Accelerators ? Energy limit of circular proton collider given by magnetic field strength. P B R / · Energy gain relies in large part on magnet development Linear Electron Collider or Muon Collider? proton P P Leptons preferred: Collide point particles rather than complex objects But, charged particles radiate energy when accelerated. Power α (E/m)4 Need linear electron accelerator or m large (muon 200 heavier than electron) A plasma: collection of free positive and negative charges (ions and electrons). Material is already broken down. A plasma can therefore sustain very high fields. C. Joshi, UCLA E. Adli, Oslo An intense particle beam, or intense laser beam, can be used to drive the plasma electrons. Plasma frequency depends only on density: Ideas of ~100 GV/m electric fields in plasma, using 1018 W/cm2 lasers: 1979 T.Tajima and J.M.Dawson (UCLA), Laser Electron Accelerator, Phys. Rev. Lett. 43, 267–270 (1979). Using partice beams as drivers: P. Chen et al. Phys. Rev. Lett. 54, 693–696 (1985) Energy Budget: Introduction Witness: Staging Concepts 1010 particles @ 1 TeV ≈ few kJ Drivers: PW lasers today, ~40 J/Pulse FACET (e beam, SLAC), 30J/bunch SPS@CERN 20kJ/bunch Leemans & Esarey, Phys. Today 62 #3 (2009) LHC@CERN 300 kJ/bunch Dephasing 1 LHC driven stage SPS: ~100m, LHC: ~few km E. Adli et al. arXiv:1308.1145,2013 FCC: ~ 1<latexit sha1_base64="TR2ZhSl5+Ed6CqWViBcx81dMBV0=">AAAB7XicbZBNS8NAEIYn9avWr6pHL4tF8FQSEeyx4MVjBfsBbSib7aZdu9mE3YkQQv+DFw+KePX/ePPfuG1z0NYXFh7emWFn3iCRwqDrfjuljc2t7Z3ybmVv/+DwqHp80jFxqhlvs1jGuhdQw6VQvI0CJe8lmtMokLwbTG/n9e4T10bE6gGzhPsRHSsRCkbRWp2BUCFmw2rNrbsLkXXwCqhBodaw+jUYxSyNuEImqTF9z03Qz6lGwSSfVQap4QllUzrmfYuKRtz4+WLbGbmwzoiEsbZPIVm4vydyGhmTRYHtjChOzGptbv5X66cYNvxcqCRFrtjyozCVBGMyP52MhOYMZWaBMi3sroRNqKYMbUAVG4K3evI6dK7qnuX761qzUcRRhjM4h0vw4AaacActaAODR3iGV3hzYufFeXc+lq0lp5g5hT9yPn8Avy+PMg==</latexit> A. Caldwell and K. V. Lotov, Phys.
  • Accelerator Programme Evaluation Report

    Accelerator Programme Evaluation Report

    OFFICIAL Accelerator Programme Evaluation Report ACCELERATOR PROGRAMME EVALUATION REPORT 1. Executive Summary 1.1. Accelerator science (i) enables advanced facilities that underpin fields as diverse as nuclear and particle physics, and physical and life sciences; and (ii) develops novel techniques that could revolutionise future research and lead to a wealth of applications. 1.2. Accelerator science within STFC is supported within the National Laboratories and by the Programmes Directorate (PD) programme. The PD programme funds accelerator R&D in universities via the UK’s two accelerator institutes (the Cockcroft and John Adams Institutes), and by fixed contribution to the Accelerator Science and Technology Centre (ASTeC) National Laboratory. 1.3. This review has evaluated the STFC PD funded Accelerators Programme under three financial scenarios (flat cash, and ±10%). The review includes a consideration of the breadth and balance of the programme and its sustainability. 1.4. We find that the UK performs world class accelerator science and is a valued and sought-after international partner. UK scientists lead international collaborations and working groups, develop innovative techniques, produce high impact papers, and leverage international investment in projects. UK accelerator institutes and universities provide world-class training and skilled graduates that move into industry and the public sector, 1.5. This world-leading expertise provides a basis to successfully leverage support and lead work in future projects. For example, the UK’s track record in cryomodules and targetry enabled the UK to successfully bid for BEIS funding and lead this work at Fermilab’s Long Baseline Neutrino Facility (LBNF). We note that this investment dwarfs PD’s total accelerator science budget, and that participation would not otherwise have been possible.
  • Jianglai Liu Shanghai Jiao Tong University

    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.
  • CERN and Astroparticle Physics

    CERN and Astroparticle Physics

    CERN and Astroparticle Physics Fabiola Gianotti, APPEC, 7 April 2016 CERN scientific strategy: three main pillars Full exploitation of the LHC: ! Run 2 started last year ! building upgrades of injectors, collider and detectors (HL-LHC) Diversity programme serving a broad community: ! ongoing experiments and facilities at Booster, PS, SPS and their upgrades (ELENA, HIE-ISOLDE) ! participation in accelerator-based neutrino projects outside Europe (presently mainly LBNF in the US) through the CERN Neutrino Platform Preparation of CERN’s future: ! vibrant accelerator R&D programme exploiting CERN’s strengths and uniqueness (including superconducting high-field magnets, AWAKE, etc.) ! design studies for future accelerators: CLIC, FCC (includes HE-LHC*) ! future opportunities for scientific diversity programme (new) * HE-LHC:~16 T Nb3Sn magnets in LHC tunnel (" √s ~ 30 TeV) CERN scientific strategy: three main pillars Full exploitation of the LHC: ! Run 2 started last year ! building upgrades of injectors, collider and detectors (HL-LHC) Diversity programme serving a broad community: ! ongoing experiments and facilities at Booster, PS, SPS and their upgrades (ELENA, HIE-ISOLDE) ! participation in accelerator-based neutrino projects outside Europe (presently mainly LBNF in the US) through the CERN Neutrino Platform Preparation of CERN’s future: ! vibrant accelerator R&D programme exploiting CERN’s strengths and uniqueness (including superconducting high-field magnets, AWAKE, etc.) ! design studies for future accelerators: CLIC, FCC (includes
  • DARWIN: Dark Matter WIMP Search with Noble Liquids

    DARWIN: Dark Matter WIMP Search with Noble Liquids

    DARWIN: dark matter WIMP search with noble liquids Laura Baudis∗† Physik Institut, University of Zurich E-mail: [email protected] DARWIN (DARk matter WImp search with Noble liquids) is an R&D and design study towards the realization of a multi-ton scale dark matter search facility in Europe, based on the liquid argon and liquid xenon time projection chamber techniques. Approved by ASPERA in late 2009, DAR- WIN brings together several European and US groups working on the existing ArDM, XENON and WARP experiments with the goal of providing a technical design report for the facility by early 2013. DARWIN will be designed to probe the spin-independent WIMP-nucleon cross sec- tion region below 10−47cm2 and to provide a high-statistics measurement of WIMP interactions in case of a positive detection in the intervening years. After a brief introduction, the DARWIN goals, components, as well as its expected physics reach will be presented. arXiv:1012.4764v1 [astro-ph.IM] 21 Dec 2010 Identification of Dark Matter 2010-IDM2010 July 26-30, 2010 Montpellier France ∗Speaker. †DARWIN Project Coordinator; on behalf of the DARWIN consortium. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/ DARWIN: dark matter WIMP search with noble liquids Laura Baudis 1. Introduction One of the most exciting topics in physics today is the nature of Dark Matter in the Universe. Although indirect evidence for cold dark matter is well established, its true nature is not yet known. The most promising explanation is Weakly Interacting Massive Particles (WIMPs), for they would naturally lead to the observed abundance and they arise in many of the potential extensions of the Standard Model of particle physics.
  • First Results of the EDELWEISS-II Direct Dark Matter Search Experiment

    First Results of the EDELWEISS-II Direct Dark Matter Search Experiment

    First results of the EDELWEISS-II Direct Dark Matter search experiment. • Dark Matter enigma • EDELWEISS-II experiment • Ge-NTD Data analysis and interpretation Silvia SCORZA Radioactive background understanding Université Claude Bernard- Institut de Physique nucléaire de Lyon WIMP search • New ID-detectors First results CEA-Saclay IRFU + IRAMIS (FRANCE), CNRS/Neel Grenoble (FRANCE), • Perspectives CNRS/IN2P3/CSNSM Orsay (FRANCE), CNRS/IN2P3/IPNL Lyon (FRANCE), CNRS-CEA/Laboratoire Souterrain de Modane (FRANCE), JINR Dubna (RUSSIA), Karlsruhe Institute of Technology (GERMANY), OXFORD University (UK) DM search motivations CDM present at all scales in the Universe… ΩB=0.044±0.004 ΩM=0.27±0.04 Ωtot=1.02±0.02 Ω =0.22±0.02 Galaxy DM Clusters Cosmology DM searches justified : direct (DM elastic scattering off target nuclei) and indirect (DM annihilation signal in galactic halo) → not enough to identify DM nature … and soon, maybe also at LHC (natural candidates arise from New Physics scenarii, such as SUSY) → no direct cosmological test (relic abundance or stability)2 WIMP dark matter (particles) WEAKLY INTERACTING MASSIVE PARTICLE Neutral and weakly interactions: neither strong nor electromagnetic → DM does not collapse to the center of the galaxy Cold enough (non-relativistic) at decoupling era Stable at cosmological scale Relic present today → explanation of Ωm 3 SUSY naturally “predicts” WIMP DM R-parity conserved → LSP stable (particle : R=+1; sparticle : R=-1) NEUTRALINO Spin-Independent Diagrams -11 -5 Interaction cross section: