international lepton-photon symposium 2005, uppsala organized by iupap bi-annual conference,...
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International LEPTON-PHOTON Symposium 2005, Uppsala
organized by IUPAPbi-annual conference, alternating with ICHEP in USspecial 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” andcovered LHC upgrade, super-factories (VEPP-2000, DAFNE-2,SuperKEKB), CLIC including Uppsala contribution, ATF, ATF-2, polarized e+ source, factory, beams, collider,plasma acceleration, laser acceleration
I noticed substantial interest in CLIC and some in beams
Frank Zimmermann, ABP-RLC 08.07.2005
direct neutrino mass measurements – KATRIN Tritium Experiment in Karlsruhe
Weinheimer
many experiments look for neutrino-less double-beta decay
Cremonesi
Srubabati
Motivation from Particle Physics
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 ++1)
LKP (first KK excitation of the photon)
Generic: WIMPs, M ~ 10 GeV - 1 TeV
Laura BaudisDark Matter Searches
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?
We can make them in accelerators…
FERMILAB
CERN
We can look at the Sun or go into space…
Or we can go to Minnesota…
deep down an old iron mine…
… to get rid of COSMIC RAYS
Where do we stand?
~ 0.2 events/kg/day
Most advanced experimentsstart 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
DAMA 3ZEPLIN I
CDMS II (2004)
EDELWEISS
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
Distortion of background images by foreground matter
Unlensed Lensed
WEAK LENSING – A POWERFUL PROBE FOR THE FUTURE
Hannestad
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!
Cosmic Ray Physics - Westerhoff
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
• fluorescence eye withactive photodetectors(HiRes)
• ground array of particle detectors(AGASA)
combine two succesful techniques
Halzen
LHCTevatron
HERA
Auger
The Future We should be optimistic !
New York Times, December 29, 1932
Robert A. Millikan
Westerhoff
TechniquesTechniques
A myriad ofA myriad oftechniques !techniques !
Satellite:Satellite:CMB, O/IR, CMB, O/IR, -ray-ray
Balloon:Balloon:CMB,CMB,
Ground:Ground:CMB, O/IRCMB, O/IR
Underground: Underground: Dark matterDark matter
Air Shower:Air Shower:-ray, CR,-ray, CR,
Underground: Underground:
R. Ong
““Top HitsTop Hits”” since LP 2003 since LP 2003
1.1. Existence of Existence of Dark EnergyDark Energy is confirmed by is confirmed by measurements in CMB and X-rays.measurements in CMB and X-rays.
Initial measurements of CMB polarization made.Initial measurements of CMB polarization made.
2.2. TeV TeV -rays discovered from Galactic Center.-rays discovered from Galactic Center. Detailed survey of galactic plane – many sources found !Detailed survey of galactic plane – many sources found !
3.3. Particles E > 10Particles E > 102020 eV confirmed – what are they? eV confirmed – what are they?
4.4. Limits on Limits on Dark MatterDark Matter improved by factor of five to improved by factor of five to < 10 < 10-42-42 cm cm22 . .
5.5. Limits on UHE neutrino sources significantly Limits on UHE neutrino sources significantly improved by AMANDA.improved by AMANDA.
The Global Design Effort
Formal organization begun at LCWS 05
Technically Driven Schedule
Dorfan
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)
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)
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
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
scale of new physics from the requirement that the radiative corrections to the higgs mass are small :
unless (Veltman condition) :
tension withaccuracy of theStandard Model
new high energy effects with scale must control the higgs
mass
Halzen
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