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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 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 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
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 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
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 ?
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
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 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 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 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. • 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: