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