P5 Report in 2008, There Have Been Large International Science Projects Successfully
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3.00Pm CET = 7.00 Am Pacific Time GRAVITATIONAL
PRESS RELEASE IN OCCASION OF THE START OF O3 Embargoed until March 26 – 3.00pm CET = 7.00 am Pacific time GRAVITATIONAL WAVE DETECTORS JOIN FORCES FOR A NEW YEAR-LONG SIGNAL HUNT Cascina (Pisa, Italy) - The Virgo and LIGO detectors are ready to start the new Observing run called O3, lasting a whole year. The hunt for gravitational waves is set to start on April 1st when the European Virgo detector, based in Italy at the European Gravitational Observatory (EGO), and the LIGO twin detectors, located in the state of Washington and Louisiana (USA), will start to take data becoming together the most sensitive gravitational wave observatory to date. During a one-year period the LIGO and Virgo Collaborations will register science data continuously, and the three detectors will operate as a global observatory. Since August 2017, the end of the second observation run O2, the two collaborations have intensively worked on their interferometers to improve the sensitivity and reliability. Scientists have also improved their offline and online data analysis and developed further the procedures for releasing Open Public Alerts: these will within minutes notify the physics and astronomy community when a potential gravitational-wave event is observed. “With our three detectors now operational at a significantly improved sensitivity, the global LIGO-Virgo detector network is expected to make several new detections. Moreover it will allow precise triangulation of the sources of gravitational waves. This will be an important step towards our quest of multi-messenger astronomy”, says Jo van den Brand of Nikhef (the Dutch National Institute for Subatomic Physics) and VU University Amsterdam, who is the spokesperson for the Virgo collaboration. -
New Aspera Roadmap
Astroparticle Physics for Europe ASPERA (& ApPEC) Roadmap Antonio Ferrer IFIC/MINECO Aspera-Spain Coordinator Benasque IMFP 1 June 2012 Astroparticle Physics for Europe > What is ApPEC ? > ApPEC is an European Consortium of funding agencies for Astroparticle Physics Coordination. Astroparticle Physics for Europe ApPEC created in 2001 by the national funding agencies of France, Germany, Italy, the Netherlands and UK. Since then Spain, Belgium, Portugal, Greece, Switzerland and Poland have joined ApPEC aims to Promote and facilitate co-operation within the European Particle Astrophysics (PA) community Develop and promulgate long term strategies for European PA, offering advice to national funding agencies and EU Assist in improving links and co-ordination between European PA and the scientific programmes of organisations such as CERN, ESA, and ESO Express their collective views on AP in appropriate international forums, such as OECD, UNESCO etc. Astroparticle Physics for Europe > What is ASPERA ? > ASPERA is an ERANET, a European network of national government agencies responsible for coordinating and funding research in astroparticle physics. > ASPERA is funded by the European Commission (FP 6) at the level of 2.5 Million € over a three years period. It started in July 2006. > ASPERA arises from the existence of ApPEC (Astroparticle Physics European Coordination). What is ASPERA ? Astroparticle Physics for Europe ‘per aspera ad astra’ www.aspera-eu.org ASPERA-I FP6 ERANET (July2006-July2009, 2.5 M€) Study APP personnel and funding -
Benefits to the U.S. from Physicists Working at Accelerators Overseas
SLAC{PUB{15859 December, 2013 Benefits to the U.S. from Physicists Working at Accelerators Overseas Jacob Anderson, Raymond Brock, Yuri Gershtein, Nicholas Hadley, Michael Harrison, Meenakshi Narain, Jason Nielsen, Fred Olness, Bjoern Penning, Michael Peskin, Eric Prebys, Marc Ross, Salvatore Rappoccio, Abraham Seiden, Ryszard Stroynowski ABSTRACT We illustrate benefits to the U.S. economy and technological infrastructure of U.S. participation in accelerators overseas. We discuss contributions to exper- imental hardware and analysis and to accelerator technology and components, and benefits stemming from the involvement of U.S. students and postdoctoral fellows in global scientific collaborations. CONTRIBUTED TO Snowmass 2013 Electronic Proceedings Community Summer Study, Minneapolis, MN July 29 { August 6, 20123 SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025 Work supported by US Department of Energy contract DE-AC02-76SF00515 and HEP. Contents 1 Introduction 2 2 U.S. Leadership in Fundamental Science 3 2.1 Today's Big Science Scale . 3 2.2 Sharing of effort in large science projects . 5 2.3 Sharing international responsibility for large projects . 7 3 Particle Physics Innovation-Transfer 7 3.1 Contributions to Detectors . 8 3.1.1 CMS endcap . 9 3.1.2 ATLAS pixel tracker . 9 3.2 Contributions to Accelerators . 11 3.2.1 Accelerator collaboration in overseas projects . 11 3.2.2 The LHC luminosity upgrade . 13 3.2.3 The ILC R&D program . 14 3.2.4 Accelerator innovation: conclusions . 15 4 Particle Physics Imagination-Transfer 16 4.1 Contributions to Experimental Analysis . 16 4.1.1 An analysis contributor { 1 . -
CERN Council Meeting – March 2020
The 2020 Update of the European Particle Physics Strategy CERN Council meeting – March 2020 Halina Abramowicz Tel Aviv University Secretary of the Strategy Update Presentation of the 2020 Strategy update • General Introduction • Preamble • Strategy Statements (20): introduction and formulation 19/06/2020 CERN Council Open Session 1 EPPSU2020 General Introduction 20 Strategy Statements unanimously adopted by the ESG in Jan.2020 • 2 statements on Major developments from the 2013 Strategy • 3 statements on General considerations for the 2020 update • 2 statements on High-priority future initiatives • 4 statements on Other essential scientific activities for particle physics • 2 statements on Synergies with neighbouring fields • 3 statements on Organisational issues • 4 statements on Environmental and societal impact Derived based on o Granada Symposium o National Inputs Two documents submitted : o Working Group 1: Social and career aspects for the next generation 1. Draft Update of the European Strategy for o Working Group 2:Issues related to Global Projects hosted by CERN or funded Particle Physics (with preamble, statements, conclusion) for feedback through CERN outside Europe CERN/SPC/1137/RA CERN/3486/C2 o Working Group 3: Relations with other groups and organisations 2. Deliberation Document (with in addition o Working Group 4: Knowledge and Technology Transfer rational behind the statements) for information o Working Group 5: Public engagement, Education and Communication CERN/SPC/1136/RA; CERN/3485/C o Working Group 6: Sustainability -
What Is Astroparticle Physics ?
What is AstroParticle Physics ? KEY QUESTIONS AND METHODS 9What is the Universe made of ? 9Nature of dark matter and energy 9Use rare processes (neutrino properties , proton decay) to probe the first instants of the Universe 9What is the origin of cosmic rays? What is the nature of violent cosmic phenomena ? 9Use new messengers beyond light and radio waves (high energy photons , neutrinos, charged particles, gravitational waves) to probe the « interior » of violent cosmic processes Observatories deployed 9In the desert (AUGER/Argentina, HESS/Namibia) 9In large planes (GW antenna Virgo/Pisa) 9Underground (Gran Sasso/Fréjus/Camfrance/Boulby) 9Underwater (Mediterannean ANTARES/NEMO/NESTOR) 9In space (FERMI,/PAMELA, AMS at the ISS) 9RICH INTERFACE WITH ENVIRONMENT AND GEOSCIENCE 9ASTROPARTICLE PHYSICS HAS A RICH ECSITE Conference – Stavros Katsanevas / ASPERA – June 2009 OUTREACH POTENTIAL Federating a community through a European outreach project 10-17 October 2009: European week of astroparticle physics Celebrating the 100th anniversary of first cosmic rays experiments •In the frame of IYA 2009, we are mobilising physicists, laboratories, sites of experiments to organize big or small events •Open days, talks for the general public, exhibitions… With events organized all over Europe, astroparticle physicists will meet the general public and explain the challenges they face •Science centres are very welcome to organize things in this frame, we are open to collaborations, providing for instance speakers for public talks… •More information to come on: www.astroparticle.org ECSITE Conference – Stavros Katsanevas / ASPERA – June 2009 Federating a community through a European outreach project 10-17 October 2009: European week of astroparticle physics: 2 large events as examples Roma: first large exhibition fully dedicated to astroparticle physics • Developped by the three major Italian institutes involved in astroparticle physics INFN, INAF & ASI, the 600 square-metres exhibition will be inaugurated during the week in an art Museum in Roma. -
Of European Astroparticle Physics Unveiled to the World 29 September 2008
The 'Magnificent 7' of European astroparticle physics unveiled to the world 29 September 2008 Today Europeans presented to the world their To insure the coordination of astroparticle physics at strategy for the future of astroparticle physics. the European level, research agencies from 13 What is dark matter? What is the origin of cosmic countries joined their efforts within the ASPERA* rays? What is the role of violent cosmic European network, an ERA-Net funded by the processes? Can we detect gravitational waves? European Commission. Thanks to the work achieved through ASPERA, European countries for With seven types of major large-scale projects the first time have a common tool to programme physicists want to find the answers to some of the jointly and share their efforts in astroparticle most exciting questions about the Universe: physics. -- CTA, a large array of Cherenkov Telescopes for This ambitious programme will gather European detection of cosmic high-energy gamma rays countries to open new exciting windows to the -- KM3NeT, a cubic kilometre-scale neutrino Universe, and the most advanced projects such as telescope in the Mediterranean Sea CTA (high-energy gamma rays) and KM3NeT (high- -- Ton-scale detectors for dark matter searches energy neutrinos) could start construction by 2012. -- A ton-scale detector for the determination of the The complete funding of this billion-scale fundamental nature and mass of neutrinos programme would need a smooth yearly increase -- A Megaton-scale detector for proton decay's of current investments for astroparticle physics, search, neutrino astrophysics & investigation of amounting to an integrated increase of about 50% neutrino properties in a ten-year period. -
Deliberation Document on the 2020 Update European Strategy
DELIBERATION DOCUMENT ON THE 2020 UPDATE OF THE EUROPEAN STRATEGY FOR PARTICLE PHYSICS The European Strategy Group _Preface The first European Strategy for Particle Physics (hereinafter referred to as “the Strategy”), consisting of seventeen Strategy statements, was adopted by the CERN Council at its special session in Lisbon in July 2006. A first update of the Strategy was adopted by the CERN Council at its special session in Brussels in May 2013. This second update of the Strategy was formulated by the European Strategy Group (ESG) (Annex 1) during its six-day meeting in Bad Honnef in January 2020. The resolution on the 2020 Update of the European Strategy for Particle Physics was adopted at the 199th Session of the CERN Council on 19 June 2020. The ESG was assisted by the Physics Preparatory Group (Annex 2), which had provided scientific input based on the material presented at a four-day Open Symposium held in Granada in May 2019, and on documents submitted by the community worldwide. In addition, six working groups (Annex 3) were set up within the ESG to address the following points: Social and career aspects for the next generation; Issues related to Global Projects hosted by CERN or funded through CERN outside Europe; Relations with other groups and organisations; Knowledge and Technology Transfer; Public engagement, Education and Communication; Sustainability and Environmental impact. Their conclusions were discussed at the Bad Honnef meeting. This Deliberation Document was prepared by the Strategy Secretariat. It provides background information underpinning the Strategy statements. Recommendations to the CERN Council made by the Working Groups for possible modifications to certain organisational matters are also given. -
Future Ground-Based Gravitational-Wave Observatories: Synergies with Other Scientific Communities
Future Ground-Based Gravitational-Wave Observatories: Synergies with Other Scientific Communities GWIC April 2021 COMMUNITY NETWORKING SUBCOMMTTEE Michele Punturo, INFN - Perugia, Italy (Co-chair) David Reitze, Caltech, USA (Co-chair) David Shoemaker, MIT, USA STEERING COMMITTEE Michele Punturo, INFN - Perugia, Italy (Co-chair) David Reitze, Caltech, USA (Co-chair) Peter Couvares, Caltech, USA Stavros Katsanevas, European Gravitational Observatory, Italy Takaaki Kajita, University of Tokyo, Japan Vicky Kalogera, Northwestern University, USA Harald Lueck, Albert Einstein Institute, Germany David McClelland, Australian National University, Australia Sheila Rowan, University of Glasgow, UK Gary Sanders, Caltech, USA B.S. Sathyaprakash, Penn State University, USA and Cardiff University, UK David Shoemaker, MIT, USA (Secretary) Jo van den Brand, Nikhef, Netherlands GRAVITATIONAL WAVE INTERNATIONAL COMMITTEE This document was produced by the GWIC 3G Subcommittee and the GWIC 3G Synergies with Scientific Communities Subcommittee Final release, April 2021 Cover: LIGO/Caltech/MIT/Sonoma State (Aurore Simonnet) Contents 1 Introduction ........................................................1 2 Constituencies & Affiliated Communities .......................2 3 Engaging with Constituencies & Communities .................7 4 Summary of Recommendations ................................ 11 1. Introduction Planning for the development of a 3rd generation global gravitational-wave detector array is a multifaceted and complex effort that will necessarily need a high level of community input. Interfacing to extant and new stakeholders in the broader scientific constituencies is absolutely necessary to, first, keep them aware of the activities taking place in the ground-based gravitational-wave community and, second, receive input to inform and evolve the planning. The Community Networking Subcommittee within the GWIC 3G Planning Committee is charged with organizing and facilitating communications between 3rd generation projects and the relevant scientific communities. -
Long Base-Line Neutrino Oscillation Beams and Experiments
481 LONG BASE-LINE NEUTRINO OSCILLATION BEAMS AND EXPERIMENTS Stavros Katsanevas University of Athens 104 Solonos, GR-106 80 Athens. Abstract Strong interest has recently been shown in very long base-line neutrino beams1 directed at existing or planned massivedetector facilities, in order to extend the search forneutrino oscil lations. There are currently proposed experiments in the U.S, Japan and Europe. Among such possibilities are beams from CERN pointing towards the Gran Sasso Underground Laboratory in Italy and the NESTOR Underwater Laboratory in the Ionian Sea off the west coast of the Peloponnese. After a brief review of the long baseline beam possibilities in the U.S and Japan, the basic parameters of a CERN beam are studied. A number of possible configurations cov ering a range of neutrino energy bands are studied and estimates of the neutrino fluxes, event rates and backgrounds at typical detectors are reported. A neutrino oscillation search down to limits of sin2 0.01 and could be made with currently proposed detectors. 20 � �m2 � O.OOleV2 482 1 Introduction The relatively old idea of a long baselineaccelerator beam pointing to a detector located tens to hundreds of kilometers away hasevolved from the phase of first estimations [l] to that of realistic designs and detailed proposals [2]. Further, results of the KAMIOKANDE, !MB, and SOUDAN [3] collaborations suggest that perhaps as much as 40 % of the atmospheric v" events in the energy range from 0.2-1.5 GeV have oscillated to some other type of neutrino. On then other hand, FREJUS [4] did not record any effect. -
Theory for Non-Accelerator Particle Physics
Theory for non-accelerator particle physics Subir Sarkar University of Oxford PPAP meeting, University of Birmingham, 15 July 2009 … significant overlap in physics priorities with the Particle Astrophysics Panel (PAAP) e.g. the following were the key questions addressed by ApPEC, the Astroparticle Physics European Coordination committee What is the universe made of? Do protons last for ever? What are the properties of neutrinos … and their role in cosmic evolution? What can neutrinos tell us about the interior of the Sun and Earth, and about supernova explosions? What is the origin of cosmic rays? How does the sky look at extreme energies? What is the nature of gravity? Can we detect gravitational waves? What can they tell us about violent cosmic processes? Since neutrino physics has been discussed already, I will focus on dark matter & nucleon decay courtesey: Stavros Katsanevas What are the fundamental conservation laws in Nature? “One is tempted to conclude that the only fundamental conservation laws left in physics are the gauge symmetries: Lorentz invariance and SU(3)✕ SU(2)✕ U(1). But then what about baryon and lepton conservation? They appear to be exact and unbroken, but they are surely not exact unbroken gauge symmetries, because we do not see the effects of a long-range vector field coupled to baryon or lepton number. The peculiar position of baryon and lepton conservation in today’s physics suggests that baryon and lepton conservation may go the way of the other non- gauge symmetries, and turn out to be only approximate consequences -
Energy Frontier Workshop
The 2020 Update of the European Particle Physics Strategy Snowmass – Energy Frontier Workshop Halina Abramowicz Tel Aviv University Secretary of the Strategy Update Outline • General Introduction • Preamble • Short guide to all 20 statements • Selected Strategy Statements: introduction and formulation 20/07/2020 Snowmass - High Energy Frontier 1 2020 Strategy Update Reminder - organisation of the Update Process • Decision making body – CERN Council as coordinating body of European Particle Physics (23 Member States) • Drafting of the Strategy Update document – responsibility of the European Strategy Group (ESG) (23 MS representatives, LDG - National Lab’s Directors Group, Strategy Secretariat; Invitees: Associate MS, Observer States,… - see backup slide) • Scientific Input to the Strategy Update – responsibility of the Physics Preparatory Group (PPG) (nominations 4 from ECFA, 4 from SPC, 4 from ICFA, 1 CERN, SUS – see backup slide) Ø Call for input and processing of the input Ø Open Symposium with outcome summarized in the Briefing Book • Coordinating body – the Strategy Update Secretariat (SUS) (Secretary elected by Council, chairs of SPC, ECFA, LDG) • Strategy implementation – purview of CERN DG, under scrutiny of CERN Council but also ECFA 20/07/2020 Snowmass - High Energy Frontier 2 2020 Strategy Update Timeline 2 Documents submitted to CERN Council - 2020 Update of the European Strategy for Particle Physics (with preamble, statements, conclusion) (brochure) - Deliberation Document (with in addition rational behind the statements) -
Di-Boson Production at Hadron Colliders
Di-Boson Production at Hadron Colliders Beate Heinemann, University of Liverpool . The Standard Model and Beyond . Tevatron and the LHC . γγ . Wγ and Zγ . WW, WZ, ZZ . Wh . Summary and Outlook Northwestern University - Seminar Oct. 4th 2004 Di-Boson Production: What’s that? Associated production of ≥ 2 gauge bosons of electroweak interaction pp-> γγ, Wγ, Zγ, WW, WZ, ZZ ? + X Something happens 10-04-2004 Beate Heinemann - Northwestern University 2 The Standard Model of Particle Physics -3 generations of quarks and leptons interact via exchange of gauge Gauge Bosons bosons: Particle Mass Force -Electroweak SU(2)xU(1): W, Z, γ (GeV/c2) -Strong SU(3): g Photon (γ) 0 Electroweak W± 80.450 Electroweak -Symmetry breaking caused by Higgs 0 field Z 91.187 Electroweak ⇒Generates Goldstone bosons Gluons (g) 0 Strong ⇒Longitudinal degrees of Higgs Boson freedom for W and Z ⇒ 3 massive and one massless -Vacuum quantum numbers (0++) gauge bosons -Couples to mass 10-04-2004 Beate Heinemann - Northwestern University 3 The Higgs boson: what do we know? . Precision measurements of mW depends on mt and mh 2 o MW =80.412 ± 0.042 GeV/c 2 o Mtop=178.0 +- 4.3 GeV/c . Prediction of higgs boson mass within SM due to loop corrections o Most likely value: 114 GeV . Direct limit (LEP): mh>114.4 GeV 10-04-2004 Beate Heinemann - Northwestern University 4 The Higgs boson: what do we know? . Precision measurements of 2 o MW =80.412 ± 0.042 GeV/c Better prediction with expected 2 o Mtop=178.0 +- 4.3 GeV/c .