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International LEPTON-PHOTON Symposium 2005, Uppsala organized by IUPAP

International LEPTON-PHOTON Symposium 2005, Uppsala organized by IUPAP bi-annual conference, alternating with ICHEP in US special format: only invited review talks, including review of submitted papers, plus poster session attended by ~400 people, including 4 lab directors

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International LEPTON-PHOTON Symposium 2005, Uppsala organized by IUPAP

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  1. International LEPTON-PHOTON Symposium 2005, Uppsala organized by IUPAP bi-annual conference, alternating with ICHEP in US special format: only invited review talks, including review of submitted papers, plus poster session attended by ~400 people, including 4 lab directors (SLAC, FNAL, DESY, IHEP) my own presentation was on “R&D for future accelerators” and covered LHC upgrade, super-factories (VEPP-2000, DAFNE-2, SuperKEKB), CLIC including Uppsala contribution, ATF, ATF-2, polarized e+ source, n factory, b beams, m collider, plasma acceleration, laser acceleration I noticed substantial interest in CLIC and some in b beams Frank Zimmermann, ABP-RLC 08.07.2005

  2. direct neutrino mass measurements – KATRIN Tritium Experiment in Karlsruhe Weinheimer

  3. many experiments look for neutrino-less double-beta decay Cremonesi

  4. Srubabati

  5. Dark Matter Searches Motivation from Particle Physics Laura Baudis • Standard Model extremely successful … but incomplete! • Neutrinos oscillate -> are massive! • Hierarchy problem: 103 GeV << 1019 GeV -> we expect new physics at the weak scale! • Popular extensions: • Supersymmetry (bosons - fermions) • LSP (neutralino) • Extra dimensions (3 + d +1) • LKP (first KK excitation of the photon) Generic: WIMPs, M ~ 10 GeV - 1 TeV

  6. WIMPs: 106 per second through your thumb without being noticed! 1015 through a human body each day: only < 10 will interact, the rest is passing through unaffected! If their interaction is so weak, how can we detect them?

  7. We can make them in accelerators… FERMILAB CERN

  8. We can look at the Sun or go into space…

  9. Or we can go to Minnesota… … to get rid of COSMIC RAYS deep down an old iron mine…

  10. DAMA 3s ZEPLIN I EDELWEISS CDMS II (2004) Where do we stand? ~ 0.2 events/kg/day Most advanced experiments start to test the predicted SUSY parameter space One evidence for a positive WIMP signal (DAMA NaI) Not confirmed by other experiments Predictions: Ellis & Olive, Baltz & Gondolo, Mandic & all

  11. The Cosmic Mystery-Pie ‘The constitution of the universe may be set in first place among all natural things that can be known’ Galileo Galilei, Dialogue

  12. WEAK LENSING – A POWERFUL PROBE FOR THE FUTURE Distortion of background images by foreground matter Hannestad Unlensed Lensed

  13. CONCLUSIONS WE ARE NOW FIRMLY INTO THE ERA OF PRECISION COSMOLOGY COSMOLOGICAL CONSTRAINTS ARE NOW IMPORTANT FOR PARTICLE PHYSICS EXPERIMENTS SOME PARAMETERS (LIKE NEUTRINO MASSES) ARE MORE CONSTRAINED BY COSMOLOGY THAN BY EXPERIMENTS THE FUTURE IS LOOKING VERY BRIGHT!

  14. Cosmic Ray Physics - Westerhoff

  15. Pierre Auger Observatory • Hybrid detector, combining surface detector array (SD) and fluorescence detector (FD) • 1600 surface detector stations with 1500 m distance • 4 fluorescence sites overlooking the surface detector array • 3000 km2 area • 1 Auger year = 30 AGASA years (SD) www.auger.org

  16. combine two succesful techniques • fluorescence eye with • active photodetectors • (HiRes) • ground array of particle detectors • (AGASA) Halzen

  17. Auger LHC Tevatron HERA

  18. The Future • We should be optimistic ! • New York Times, December 29, 1932 Robert A. Millikan Westerhoff

  19. Techniques Satellite: CMB, O/IR, g-ray Balloon: CMB, n Ground: CMB, O/IR Air Shower: g-ray, CR, n Underground: Dark matter Underground: n R. Ong A myriad of techniques !

  20. “Top Hits” since LP 2003 • Existence of Dark Energy is confirmed by measurements in CMB and X-rays. • Initial measurements of CMB polarization made. • TeV g-rays discovered from Galactic Center. • Detailed survey of galactic plane – many sources found ! • Particles E > 1020 eV confirmed – what are they? • Limits on Dark Matter improved by factor of five to s < 10-42 cm2 . • Limits on UHE neutrino sources significantly improved by AMANDA.

  21. Dorfan Formal organization begun at LCWS 05 The Global Design Effort Technically Driven Schedule

  22. GDE – Near Term Plan • Staff the GDE • Administrative, Communications, Web staff • Regional Directors (one per region) • Engineering/Costing Engineer (one per region) • Civil Engineer (one per region) • Key Experts for the GDE design staff from the world community • Fill in missing skills (later) Total staff size about 20 FTE (2005-2006)

  23. GDE – Near Term Plan • Organize the ILC effort globally • First Step --- Appoint Regional Directors within the GDE who will serve as single points of contact for each region to coordinate the program in that region. • Gerry Dugan (North America), Fumihiko Takasaki (Asia), Brian Foster (Europe) • Make Website, coordinate meetings, coordinate R&D programs, Weekly “Director’s Corner”, etc • http://www.interactions.org/linearcollider/ • R&D Program • Coordinate worldwide R & D efforts, in order to demonstrate and improve the performance, reduce the costs, attain the required reliability, etc. (Proposal Driven to GDE)

  24. GDE – Near Term Plan • Schedule • Begin to define Configuration (Aug 05) • Baseline Configuration Document by end of 2005 ----------------------------------------------------------------------- • Put Baseline under Configuration Control (Jan 06) • Develop Reference Design Report by end of 2006 • Three volumes -- 1) Reference Design Report; 2) Shorter glossy version for non-experts and policy makers ; 3) Detector Concept Report

  25. Some of the key Near-Term Design Choices • Accelerating Gradient • Positron Production mechanism • Design of Damping ring • Site-specific considerations: One or two tunnels? Shallow or deep?, etc • Total cost will be a key determining factor in our ability to get the ILC built. Therefore cost optimization of all systems is of primary importance

  26. new high energy effects with scale L must control the higgs mass d scale of new physics from the requirement that the radiative corrections to the higgs mass are small : unless (Veltman condition) : tension with accuracy of the Standard Model Halzen

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