Post on 18-Aug-2018
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 )
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.
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 !