The HighUnive

R A ORene A. On

SLAC 50th Anniversary Cele

-Energyerse

(UCLA)ng (UCLA)

ebration, 24 September 2012

Cosmic Messenger

We learn about the universt ) f fsystem) from four messen

Messenger SPhotons γ ne

Cosmic Rays p He++ coCosmic Rays p, He++, … coNeutrinos ν ne

Gravitational Waves neGravitational Waves ne

This talk will summarize ourThis talk will summarize our of messengers 1-3 at high en

rs

se (outside the solar ngers:

Strength Weaknesseutral absorbed

opious deflectedopious deflectedeutral hard to detect

eutral very hard to detecteutral very hard to detect

understanding and goalsunderstanding and goalsnergies (E > 1 GeV).

New wavebands = N

Infrared

Milky Way Galactic Center region

• Jim Buckley

TeV γ-rGhez et al 2012 TeV γ-r

G V & T V i i i

Ghez et al., 20121” x 1”

GeV & TeV emission is:

• Intense & non-thermal• totally unexpected

t d t d• not understood

New insight

GeV γ-raysFermi-LAT

S. Murgia, “Dark Attack 2012”15o x 15o15o x 15o

raysrays

M. Beilicke et al.“Gamma 2012”1o x 3o

Outline

IntroductionThe study of high eneThe study of high-eneDetection techniques, Main scientific motivat

Present LandscapeSurvey of existing expSurvey of existing exp(A few) recent scientifi

FutureFutureKey science goals for New instruments & neScience results presen

Summary, Acknowledgemy, g

rgy particles in the cosmosrgy particles in the cosmosfirst detectors

tions

periments, SLAC programperiments, SLAC programic highlights: γ’s, CR’s, ν’s

futureew ideasnted at SLAC’s 75th Anniversary !

ments

We celebrate two great an

50th Anniversary of SLA

W Panofsky SLAC BL May 1983

50

W. Panofsky, SLAC BL, May 1983

100th Anniversary of Cos100 Anniversary of Cos

100 yea

Victor Hess in 1912 P. Carlson, Phys. Today, Feb. 2012

100 yea

nniversaries in 2012:

AC

years

smic Rayssmic RaysCTA

arsDetector

Neutrino

Muon

ars

Cosmic Rays: Firs

1912 V. Hess discovery

1920-40 Identification as protons

1930-55 New Particles (e+,μ,π, etc.)Birth of “high-energy physics”

1939 Extensive air showers 1949 E. Fdiscovered by P. Auger “shoEcr > 1015 eVcr

P. Auger & R. Maze, Comptes Rendus, 1938

t 50 Years

C.D. Anderson, 1933 B. Rossi, “Cosmic Rays”, 1964

Fermi proposes 1962 J. Linsley discoveryock” accelerator of UHECRs

E > 1020 eV !

J. Linsley looking for rattlesnakesat Volcano Ranch (NM)

At Founding of SLABy 1962, we knew that cosmic rays were and that they covered a very large dynam

S. Swordy, 1993

Energy: GeV TeV PeV EeV Z

ACmostly charged protons & nuclei

mic range > 1012.

Cosmic rays:cover an enormous energy rangecover an enormous energy rangehave energy density ~ 1 eV/cm3

have mysterious origin(s) – bent by galactic B fieldby galactic B field

Photons, Neutrinos:are un deflected by B fieldsare un-deflected by B fieldscan be used to directly imageastrophysical sources

1962: Ideas for γ-ray and ν astronomyexisted but it took another 25 years

ZeV

existed – but it took another 25 yearsto bear fruit … skipping forward ...

γ−ray and Neutrino The few years following 1987 were critica

198Crab Neb

1987SN 1987A

IMB D t t 30 M V

Crab NebTeV γ ray

Whipple 10IMB Detector: 30 MeV ν

Detection of ν’sfrom SN 1987A TeV γ-rayfrom SN 1987A

Astronomyl ones for γ-ray and ν astronomy:

89bula

1991

HE γ-ray sky seen by EGRET

C t Ob t

bula: Firsty source

0m Telescope

Launch of Comptonγ ray Observatory

Compton γ-ray Observatory

y source γ-ray Observatory

Multi-Messenger Sc

Black HoleHole

eπ

p

Active Galactic

Jete

γNucleus (AGN)

Gγ

cience

EeVp Cosmic Rays

P Vν

PeVNeutrinos

eV/TeVγ−rays

γ-ray & Cosmic RayIntergalactic radiation fields limit the ra

γ γEBL e+ e-

Spectral DistoSpectral Disto

y Horizonange of γ-rays and cosmic rays:

P γCMB Δ+ Νπ

S i E 6 1019 V

“GZK Effect”

Suppression Ep > 6 x1019eV

ortion Li it th di t tortion Limits the distance to sourcesto < ~150 Mpc.

Diffuse “GZK” neutrinos.

Main Scientific Mot1. A New Window on the Cosm

Discovery of new astrophy(e.g. GRBs, Fermi bubbles

Understanding the sourcesTevatrons/Pevatrons involvTevatrons/Pevatrons involv

Multi-messenger astronomproviding complementary v

“You can observe a lot by

2. Connection of “Inner-Spac2. Connection of Inner SpacNew physics/new particles (e.g. dark matter, primordia

HE beams over long distannature of space-time.

“The universe is an elemThe universe is … an elemlaboratory.” (David Schr

tivationsmossical phenomena

s, Galactic center …).

s of high-energy particles:ving “extreme astrophysics”.ving extreme astrophysics .

my: cosmic rays, γ-rays and ν’sviews.

just watching.” (Yogi Berra)

ce” “Outer-Space”ce Outer Spacedetectable HE signatures

al black holes, etc.).

nces tests of cosmology and the

mentary particle physicsmentary particle physics ramm)

A New Window on

Key points on “extreme astrophKey points on extreme astroph

The universe is filled with luW j t t ti t dWe are just starting to unde

The energy supply for thesegravitational/EM potentialsgravitational/EM potentials astrophysical situations.

Charged particles are acceleCharged particles are acceleenergies with diverse mech

the Cosmos

hysics”:hysics”:

uminousTevatrons/Pevatrons.t d h th kerstand how they work.

e sources harnesses in a wide variety ofin a wide variety of

erated to ultra relativisticerated to ultra-relativistic anisms/parameters.

The Many Faces of

Pulsars

AGN

NS dynamo

Jets powered by accretion or unipolarInduction UHECR’sNS dynamo Induction. UHECR s

Gamma-RayBursts Unide

Star collapserelativistic jets

??

Particle AccelerationStar Forming Regions

SupernovaRemnantsRemnants

?

SNRs, cosmic rays,molecular clouds.

F i A l ti? Fermi Acceleration

Binary Systemsentifieds

VERITAS

Accretion jetsor stellar winds??

Outline

IntroductionThe study of high eneThe study of high-eneDetection techniques, Main scientific motivat

Present LandscapeSurvey of existing expSurvey of existing exp(A few) recent scientifi

FutureFutureKey science goals for New instruments & neScience results presen

Summary, Acknowledgemy, g

rgy particles in the cosmosrgy particles in the cosmosfirst detectors

tions

periments, SLAC programperiments, SLAC programic highlights, : γ’s, CR’s, ν’s

futureew ideasnted at SLAC’s 75th Anniversary

ments

CR, γ-ray, & NeutrinCRCR, γ-ray

BalloonBalloonInstruments

AtmosphericCherenkovCherenkovTelescopes

ν

no Detectors

Satellite

y

Instruments

Air Shower Arrays

(particle andN2 fluoresence)

Ice/WaterCherenkovDetectors

CR, γ-ray, & NeutrinCRCR, γ-ray

BalloonBalloonInstrumentsANITA

AtmosphericCherenkovCherenkovTelescopesHESS

ν

MAGIC VERITAS

no Detectors (2012)

Satellite

y

InstrumentsFermi SpaceTelescopeTelescope

Air Shower Arrays

(particle andN2 fluoresence)Auger

Ice/Water

gTelescope Array(HAWC)

CherenkovDetectorsSuper-K

IceCube

Fermi Large Area T

Particle detector in spaceγ-rays by pair conversionE range: 20 MeV to >300 GeVL fi ld f iLarge field of viewLaunched 11 June 2008

SLAC’SLACLABOCHH

Completed LAT tracker before integrationwith spacecraft

Telescope (LAT)

Fermi-LAT Conceptual Picture

’s Key Roles Key RoleAT electronics, flight software

Beam tests & integration of LATOperations and data processing Central in LAT analysis & scienceHost laboratory for collaborationHost laboratory for collaboration

The GeV Sky (c 201

Extragalactic SourcesExtragalactic Sources(AGN, galaxy clusters, dwarf g

Galactic Plane (pulsars

E tExt

Three-year γ-ray sky see

12)

galaxies, local group,UnIDs)

Galactic Center

, SNRs, binaries, UnIDs)

t l ti Difftragalactic Diffuse

en by Fermi-LAT

VERITAS: Ground-BaT4

T2

T1T1

VERITAS at Mt. Hopkins, AR, USA

A premier TeV γ-ray instrumFour x 12m atmospheric ChereFour x 12m atmospheric ChereEnergy range: 50 GeV-100 TeVVery sensitive, but narrow field Completing (Sept 2012) camera

ased γ-ray Detector

T3T3

Atmospheric

mentenkov telescopes

Atmospheric CherenkovTechnique

enkov telescopesVof viewa upgrade

A VERITAS Telescope

The TeV Sky (c 201

T V k b HESS MTeV sky seen by HESS, M> 130 sources now (only 2

2)

tevcat.uchicago.edu

AGIC VERITASAGIC, VERITAS2 in 1992, 8 in 2002)

SNRs: Origin of Co

General PictureRR

, 201

1V

. Acc

iari

et a

l.

Standard paradigm for CR’sGives luminosity, spectral shape.Several SNRs now provide evidence for hadron acceleration.but … more evidence needed.

osmic Rays

Recent Data from Tycho’s SNR

Tycho, age = 440y, D = 2-5 kpc

Recent Data from Tycho’s SNRVERITAS Fermi-LAT

., 20

11 G

iord

ano

et a

l.F.

Morlino & Caprioli, 2011

Fermi Bubbles

Complete Surprise !Very extended (10 kpc) wRelated to earlier history

M. Su et al. 2010

!with hard spectrum.of Galactic center ?

Auger Project: 3000

Auger Project in Mendoza, Arge

World’s largest particle de3000 km2 area covered

g j g

Energy range: E > 1017 eVSurface array of 1600 detecto24 fluoresence detectors, 4 lo

0 km2 Detector

entina

Surface array & fluorescence detection

etector

orsocations

A surface detector & fluorescence station

The 1019 eV Sky (c 2

AGN position(3.1° circle)

Event position

EeV sky seen by Auger (EEeV sky seen by Auger (EAdditional 25 events from

2012)P. Abreu et al., 2010

E > 55 EeV), 69 events.E > 55 EeV), 69 events.m Telescope Array (E>57 EeV).

CR’s at the Highest

A

O i i i till k

S. Westerhoff, “COSPAR 2012”

Origin is still unknownAuger and Telescope Array agre

Unclear if GZK effect or souWeakly correlated with nearby A

t Energies

Auger Telescope Array

S. Westerhoff, “COSPAR 2012”

ee on spectrum – clear cutoff ~6x1019eVurce acceleration limitAGN/matter

IceCube: ν Detecto

Detect

Te

kmkm

Schematic of IceCube at South Pole

r at South Pole

orMuon

Neutrino

eV muon-neutrino detection

m3 Neutrino Detector

Installing an IceCube string

m Neutrino DetectorIce-Cherenkov techniqueEnergy range: 1011-1017 eV86 strings x 60 optical modulesIceTop for air showersD C f l iDeep Core for low energies

Latest Neutrino Res

C. Spiering, “Gamma 20

IceCube neutrino sky map (probability)

No ν’s detected from point sources.Limits now well below initial estimates.

Diffuse Search: 2 detected events0 14 expected from background0.14 expected from backgroundE > 1015 eV

sults

Event displays of one PeV diffuse neutrino event

012”

.

A. Ishihara, “NNeutrino 2012”

Number of photoelectrons detected by IceCubefor two shower events, with models/bkgfn.

Inner Space O

New Physics:• Dark matter annihilation/

• Exotic particle interaction( i lik ti l(e.g. axion-like particles,

• Neutrino properties.

p p cross section at UHE• p-p cross-section at UHE

• … your item here …

Passage of HE Beams through• Measurement of cosmic

• Lorentz invariance violat

• “GZK neutrinos” from UH

Outer Space

/decay γ-rays, ν’s.

ns/decay i di l BH’ )primordial BH’s).

EE.

h space:radiation fields (EBL, IGMF).

ion.

HECR interactions.

Dark Matter Detectiγ−ray Signals

S. Murgia, “Dark Attack 2012”

Galactic Center

Dark Attack 2012

Satellites

Halo

Extragalactic

DM simulation (Pieri et al., 20

ionNeutrino Signals

Also charged particles:

positronsanti protons

Line signalsanti-protonsanti-deuterons

011)

Current DM Limitsγ-ray DM limits

J. Conrad, “Gamma

No signal (yet)Limits at or approaching thermal recross section.

But …C. Weniger, “Gamma 2012”

Evidence for line at ~130 GeV2012”

lic

~3σ (post trials).seen by several authors.close to Galactic center.systematic effect ?can be confirmed or refuted.

Extragalactic BackgUse γ-ray beam to probe EBL –background from history of sta

Previously only upper limits on EB

2012 results by Fermi and HESS prfirst actual determinations of EBL

Density close to that predicted by resocounts impacts on the star formatio

ground Light (EBL)cosmic O/IR

ar formationM. Ajello, “Gamma 2012”

BL density.

rovide the

olved galaxy n history.

SLAC Program

Starting in early 1990’s:USA X-ray mission (E Bloom)USA X ray mission (E. Bloom).1992: Convergence of W. Atwood1994: GLAST existed (Stanford wThen SLAC developed a very stro

establishment of LASLAC Directors (Richter, Dorfan,( , ,Important connection to Stanford

Some of the significant impacts (so faSome of the significant impacts (so fa1. Origins of LAT and successful o2. Critical work to demonstrate Ask3. Theoretical work.4. Development of Cherenkov Tele5. (Large Synoptic Survey Telesco( g y p y

d, E. Bloom, & P. Michelson.workshop, Snowmass 94).ong program

AT Collaboration & Drell) gave invaluable support.) g pp (& establishment of KIPAC).

ar):ar):perations & science from Fermi.

karyan Effect ANITA ν Experiment.

escope Array (CTA).ope – important HEP expertise).p p p )

1992 Talk (Transparrencies!)

LAT Development

(ed. Elliott Bloom)

Askaryan Effect at LINAC beam tests

2000: Sand (silica)2004: Rock salt2004: Rock salt2007: Ice – ANITA calibration

Dawn Williams, Al Odian, , ,& Peter Gorham

Dieter Walz

SLAC

ANITA in ESA in 2007

Outline

IntroductionThe study of high eneThe study of high-eneDetection techniques, Main scientific motivat

Present LandscapeSurvey of existing expSurvey of existing exp(A few) recent scientifi

FutureFutureKey science goals for New instruments & neScience results presen

Summary, Acknowledgemy, g

rgy particles in the cosmosrgy particles in the cosmosfirst detectors

tions

periments, SLAC programperiments, SLAC programic highlights, : γ’s, CR’s, ν’s

futureew ideasnted at SLAC’s 75th Anniversary

ments

Big Science Questi(NB: subjective)

QuestionQuestionWhat is dark matter ? Can it be detected incosmos through its particle interactions ?M th ti d di t ib ti fMeasure the properties and distribution of What new physics/interactions can be idenby HE particles from space ?What is the origin of the cosmic rays, fromto 1020 eV scale ?What is the maximum energy of cosmic pagy pacceleration ?What are the intergalactic radiation fields (and IGMF) and how are they produced ?and IGMF) and how are they produced ?What is the source of the isotropic γ-ray fluIs there an isotropic neutrino flux ?How do cosmic accelerators (e g GRB’s aHow do cosmic accelerators (e.g. GRB s aSupernovae) work ?What is going on at the Galactic center ?

ons for Future

Particle RequirementParticle Requirementn the

DM

γ, ν Sensitivity(E resolution, E range)

DM.ntified γ, ν, CR Sensitivity, E resolution,

m TeV

article

γ, ν, CR

ν CR

Sensitivity, E resolution, ang. resolution, sky coverage, MWL dataν, CR g ,

(EBL γ Sensitivity, E range

ux ? γ, ν Sensitivity, E range

and γ ν CR Sensitivity E resolutionand γ, ν, CR Sensitivity, E resolution, angular resolution, sky coverage, MWL data

Big Science Questi(NB: subjective)

QuestionQuestionWhat is dark matter ? Can it be detected incosmos through its particle interactions ?M th ti d di t ib ti fMeasure the properties and distribution of What new physics/interactions can be idenby HE particles from space ?What is the origin of the cosmic rays, fromto 1020 eV scale ?What is the maximum energy of cosmic pagy pacceleration ?What are the intergalactic radiation fields (and IGMF) and how are they produced ?and IGMF) and how are they produced ?What is the source of the isotropic γ-ray fluIs there an isotropic neutrino flux ?How do cosmic accelerators (e g GRB’s aHow do cosmic accelerators (e.g. GRB s aSupernovae) work ?What is going on at the Galactic center ?

ons for Future

Particle RequirementParticle Requirementn the

DM

γ, ν(CR)

Sensitivity(E resolution, E range)

DM.ntified γ, ν, CR Sensitivity, E resolution,

m TeV

article

γ, ν, CR

ν CR

Sensitivity, E resolution, ang. resolution, sky coverage, MWL dataν, CR g ,

(EBL γ Sensitivity, E range

ux ? γ, ν Sensitivity, E range

and γ ν CR Sensitivity E resolutionand γ, ν, CR Sensitivity, E resolution, angular resolution, sky coverage, MWL data

Future Major (>10 yPresent Futu

Fermi

HESS

ChTelesγ SS

MAGICVERITAS

γSpace

Auger Expan

CR Tel Array JECR

IceCube ARA, A

Kν ANTARES K

P(*not necessarily complete)

ANITA

yr) Efforts*ure Key Features

herenkovcope Array

10x better sensitivityWider FOVHigher & lower E

e mission ?

nded Array ?

LEM-EUSO Larger apertureHigher E reach

ARIANNA, EVA Higher E coverage

KM3NET Greater sensitivityS kKM3NET S sky coverage

PINGU Lower E coverage

Future Major (>10 yPresent Futu

Fermi

HESS

ChTelesγ SS

MAGICVERITAS

γSpace

Auger Expan

CR Tel Array JECR

IceCube ARA, A

Kν ANTARES K

P(*not necessarily complete)

ANITA

yr) Efforts*ure Key Features

herenkovcope Array

10x better sensitivityWider FOVHigher & lower E

e mission ?

nded Array ?

LEM-EUSO Larger apertureHigher E reach

ARIANNA, EVA Higher E coverage

KM3NET Greater sensitivityS kKM3NET S sky coverage

PINGU Lower E coverage

Cherenkov Telesco

CTA: artist’s conception

Key features of CTA:Factor of 10 more sensitive, better σang and σE than HESS/VERITAS.Wide E range: 25 GeV – 100 TeV.Wide field-of-view (>6o).( )Two sites: S (10 km2), N (1 km2)40-80 Cherenkov telescopes/site.Open observatory.p yComplemented by HAWC (wide-field, high duty cycle) in N.

ope Array (CTA)

S. Funk, 2012

CTA and Fermi dark matter sensitivity

Proposed US ContrBoost core array by 36 telescopes.3x better sensitivity.Hi h l ti i iHigh resolution imaging.Wider field of view.Spatially resolve (arc-min) sources to

d k fil23Eutel

map dark matter profiles.

Potential sites for CTA in N. Arizona.

~

M

Proposed sites for CTA N in Arizona, USA

ributions to CTAGreatly improved effective area with CTA-US telescopes

CTA-US

3 midsized uropean lescopes

59 midsized telescopesp telescopes

# of telescopes in reconstruction

~ 0.07°~ 0.2°

CTA-US SC-MST.MSTImproved image resolution with CTA-US

CTA-US Telescope Innovative two-mirror telescope design

Corrects aberrations – wide FOV.Reduces place scale – compact camera.High channel count/density require HEP expPrototype telescope construction 2012-2015

Schwarzschild-Couder telescope design

& Cameran: Camera FOV

pertise.5.

8°

12,000 pixels

CameraDevelopment at SLACASIC designgNew photodetectortechnology (Si-PMs)Cost effectiveCost effective Compact (< 1m)

JEM-EUSO: UHECRJEM-EUSO:

N fluorescence detector on ISN2 fluorescence detector on ISExposure/year is x10 Auger.Proposed launch in 2017.p

JEM-EUSO effective area in nadir & tilt modes.

Rs in Space

SS.

JEM-EUSO concept

JEM-EUSO on ISS (nadir).

Askaryan Radio ArrARA:

Very large (~150 km2) radio neUses Askaryan effect to detectMain science goal: GZK neutrin

Possible layout for ARA at South P

ray (ARA)

eutrino detector at South Pole.t radio Cherenkov signal.nos, E > 1017 eV.

Pole

The Future Role for

SLAC has an important role

Very strong science base: fE ll t i t di i liExcellent interdisciplinary ain future with LSST impoU i HEP t h i lUnique HEP technical expecomputing.BEAMS till i tBEAMS – still very importaFacilities for construction ai t tinstruments.Managerial expertise for la

r

to play in this area:

faculty, students, researchers.h ( F i LAT dapproach (e.g. Fermi-LAT and

ortant for CTA follow-ups).ti h i l l t iertise: mechanical, electronic,

tnt.nd testing of large

rge projects.

And now …

Science Results at

Dark matter discovered in VHEfDiscovery followed by mapping o

through its γ-ray signature and declump.

Detection of 25,000 neutrinos fThe neutrinos from a supernova pprovide confirmation of the neutriunparalleled information about su

Three local sources of positronmystery of the excess positron flu

Measurement of the intergalacIGMF density and distribution argconfounding the cosmologistsconfounding the cosmologists.

SLAC’s 75th

E γ-rays!f Gof the Galactic DM distribution

etection of proper motion of nearby

from a Supernova in our Galaxy.in Cygnus at a distance of 7.5 kpcyg pino hierarchy, as well as upernova dynamics.

ns identified. This solves the ux at high energies.

ctic magnetic field (IGMF). The gues for a primordial B field,

Science Results at

GKZ effect and upper limit to coestablished So rces of UHECRestablished. Sources of UHECRof the UHE cosmic ray spectrum detection of GKZ neutrinos confir

18galaxies as the source of E>1018

Origin of cosmic rays solved. Ad t t d i d 40detected in γ-rays and 40 sourcesaccurate measurements of protonconjunction with the identificationof ~90% of the cosmic ray flux ha

Precise determination of extragM t f EBL tMeasurement of EBL spectrum veconstraint on star-formation rate d

N B th “k ” t i thN.B. these are “known” topics; there unexpected discoveries.

SLAC’s 75th

osmic particle acceleration Rs fo nd Precise meas rementsRs found. Precise measurements and anisotropy, combined with the med the identification of starburst eV particles.

A census of 300 Galactic sources d t t d i t i ids detected in neutrinos provide

n acceleration fraction. In of several local sources, the origin

as been established.

galactic background light (EBL). d hift id tersus redshift provides strong

density.

ill l t t i l b l t lwill almost certainly be completely

SLAC provides out

Pat Burchat with som

Mark II Detector at PEPMark II Vertex Chamber(group led by John Jaros)

standing training

Rene Ong, Nigel Lockyer, Mark Nelson, Larry Gladney

Dave Bennett, Robert Johnson

meone’s baby

Elliott Bloom, Harry Nelson

Summary• High energy (HE) particles probe

particle acceleration in the cosmother means.

• Equally important is using HE prbeyond the standard modelbeyond the standard model.

• The current suite of γ-ray, cosmiprovides an unparalleled view ofp pimportant questions remain !

• SLAC has developed a world-leaastrophysics. Development of th(CTA) and leadership in this projstrong program in particle astrop

“The real voyage of discovery landscapes but in having newlandscapes, but in having new

e astrophysics of TeV/PeV/EeVmos not tested or understood by

robes to search for new physics

c ray and neutrino detectors f the universe. However, many , y

ading program in HE particle he Cherenkov Telescope Array ject is an integral component of a physics at SLAC.

consists, not in seeking new w eyes ”w eyes.

Marcel Proust (1871-1922)

Acknowledgements

The following provided useful ad

• Jim Adams• Roger Blandford• Elliott Bloom

• Alb• Sp• Fra

• Markus Boettcher• Jan Conrad• Seth Digel

• Ma• Jim• PeSeth Digel

• Jonathan Feng• Stefan Funk• Peter Gorham

Pe• Sim• An• Da• Peter Gorham

• Francis Halzen• Werner Hofmann

K l H i K t

• Da• Pie• Ch

Ste• Karl-Heinz Kampert • Ste

Much thanks to John Jaros, Mic

s

dvice and/or information:

brecht Karlepencer Kleinank Krennrichanel Martinezm Matthewseter Michelsoneter Michelsonmona Murgiangela Olintoavid Saltzbergavid Saltzbergerre Sokolskyhristian Spieringefan Westerhoffefan Westerhoff

chael Peskin and the organizers !

CongCong

50th50th

Anniversary

gratulations SLAC !gratulations SLAC !