Very-high-energy astrophysics with the Major Atmospheric Gamma-ray Imaging Cherenk

(MAGIC) telescope

Alessandro De AngelisBrera, June 2006

Outline

• Introduction• VHE-γ instruments, techniques• Scientific highlights and

observations (in particular from MAGIC)

• Outlook

Motivations for the study of gammas

• Probe the most energetic phenomena occurring in nature

– Nonthermal• Nuclear de-excitation/disintegration

• Electron interactions w/ matter, magnetic & photon fields

• Matter/antimatter annihilations

• Decay of unstable particles

⇒ Clear signatures from new physics

Motivations for the study of gammas - II

Penetrating

• No deflection from magnetic fields, point ~ to the sources– Magnetic field in the galaxy: ~ 1μG

R (pc) = 0.01p (TeV) / B (μG)=> for p of 300 PeV @ GC the directional information is lost

• Large mean free path

• Regions otherwise opaque can be transparent to X/γ

• We know how to detect them with a reasonable efficiency

Large mean free path…Transparency of the Universe

4.5 pc

450 kpc

150 Mpc

Nearest Stars

Nearest Galaxies

Nearest Galaxy Clusters

Milky Way

Detection of a high E photon

• Above the UV and below “50 GeV”, shielding from the atmosphere – Above “10 MeV”, pair

production

• Above “50 GeV”, atmospheric showers– Pair <-> Brem

Problem: opacity of the atmosphere

Consequences on the techniques

• The fluxes of h.e. γ are low and decrease rapidly with energy– a perfect 1m2 detector would detect only 1 photon/2h above 10 GeV from

the strongest sources

=> with the present space technology, VHE and UHE gammas can be detected only from atmospheric showers– Earth-based detectors, atmospheric shower satellites

• The flux from high energy charged cosmic rays is much larger

• The earth atmosphere (28 X0 at sea level) is opaque to γ => only sat-based detectors can detect primary γ

Satellite-based and atmospheric: complementary, w/ moving boundaries

• Flux of diffuse extra-galactic photons

Atmospheric

Sat

• Cosmic gamma-ray observation:- directly from satellites (HE) < O(10 GeV) and - indirectly from ground-based installations (VHE) > O(10 GeV)

• Satellites: EGRET ⇒ HE-γ-ray astronomy to maturity

Ground-based vs Satellite

• Satellite :– primary detection– small effective area ~1m2

• lower sensitivity– large angular opening

• search– large duty-cycle– large cost– low energy– low bkg

• Ground based– secondary detection– huge effective area ~104 m2

• Higher sensitivity– small angular opening (IACT)– small duty-cycle– low cost– higher energy– high bkg

The Experimental VHE World (in progress)

STACEECACTUS

MILAGRO

TIBETARGO-YBJ

PACT

GRAPES

TACTIC

VERITAS

MAGIC

HESS CANGAROO

TIBETMILAGROSTACEE

TACTIC

High galactic latitudes(Φb=2 10-5 γ cm-2 s-1 sr -1 (100 MeV/E)1.1). Cerenkov telescopes sensitivities (Veritas, MAGIC, Whipple, Hess, Celeste, Stacee, Hegra) are for 50 hours of observations.Large field of view detectors sensitivities (AGILE, GLAST, Milagro, ARGO) are for 1 year of observation.

Sensitivity of γ-ray detectors

Ground detectors: EAS vs. IACT

• EAS (Extensive Air Shower): detection of the charged particles in the shower

• Cherenkov detectors: (IACT): detection of the Cherenkov light from charged particles in the atmospheric showers

Extensive Air Shower Particle Detector Arrays

• Built to detect UHE gammas small flux => need for large surfaces, ~ 104 m2

– But: 100 TeV => 50,000 electrons & 250,000 photons at mountain altitudes, and sampling is possible

• Typical detectors are arrays of 50-1000 scintillators of ~1m2/each (fraction of sensitive area < 1%)– Possibly a μ detector for hadron rejection

• Direction from the arrival times, δθ can be ~ 1 deg• Thresholds rather large, and dependent on the point

of first interaction

EAS Particle Detector ArraysPrinciple

• Each module reports:– Time of hit (10 ns accuracy)– Number of particles crossing

detector module– Time sequence of hit

detectors -> shower direction

• Radial distribution of particles -> distance L

• Total number of particles -> energy

First Generation EAS ArraysTi

bet I

IIM

ilagr

o

ARGO

Milagro

• Resolution 0.5o

• Sensitivity ~1 Crab/year, threshold ~ 400 GeV– Not appropriate for the detection of most

astrophysical sources

Cherenkov (Č) detectorsCherenkov light from γ showers

• Č light is produced by particles faster than light in air• Limiting angle cos θc ~ 1/n

– θc ~ 1º at sea level, 1.3º at 8 km asl– Threshold @ sea level : 21 MeV for e, 44 GeV for μ

Maximum of a 1 TeV γ shower ~ 8 Km asl200 photons/m2 in the visibleDuration ~ a few nsAngular spread ~ 0.5º

Ground-based detectors: Cherenkov telescopes

• Breakthrough in high-energy astrophysics:IACTs established as astronomical tools

⇒ transition from ‘VHE-γ experiments’ to ‘VHE-γ telescopes’exploding interest in the astronomical community

• Big step within last year: - quantitative (tripling number of detected sources) - qualitative (unprecedented high quality)

COMING OFCOMING OF (GOLDEN?) AGE FOR CHERENKOV TELESCOPES !AGE FOR CHERENKOV TELESCOPES !

Incoming γ-ray

~ 10 kmParticleshower Detecting

TeV-γ-rayswith IACTs~ 1o

Chere

nkov

light

~ 120 m

Observational Technique−+→+ eepγ

γ→+ −+ ee

Image intensityShower energy

Image orientationShower direction

Image shapePrimary particle

Better bkgd reduction Better angular resolutionBetter energy resolution

Systems of Cherenkov telescopes

Gamma / hadron separation

Proton shower( wide, points anywhere )

Gamma shower( narrow, points to source )

m

h (m)

100 GeV proton

leng

thle

ngth

width

alpha

45 GeV gamma

μ

CAT (1996-2003)

HEGRA (1993-2002)

Whipple (1969-)

CANGAROO (1992-2001)

Crab nebula (Weeks+ 1989)Mk 421 (Punch+ 1992)

Prototype IACTs

New (first)-generation IACTs

• Reduce threshold larger fluxes (e.g., PL spectra) larger Cherenkov light collector larger telescopes

• Improve sensitivity higher discovery potential better γ/hseparation telescope arrays

ANDAND……- wide-field camera: survey capability, serendipitous discoveries, source morphology studies (HESS: 5-deg FoV)

- isochronous mirror and fast digitization : possibility of using Cherenkov photon arrival time for γ/h separation (MAGIC: sub-ns timing)

- light structure: fast GRB follow-up (MAGIC: ~20s repositioning)

Present IACTs: the “Big Four”

Roque delos Muchachos, Canary Islands

VERITAS (USA,UK1…)1: Oct ’03

2: 2006100 m2

(→7)

MontosaCanyon,Arizona

Windhoek, Namibia

HESS (Germany & France)2: Sum ’02

4: Early ’04100 m2

(→16)

Woomera, Australia

CANGAROO III(Japan & Australia)2: Dec. ’02, 3: Early ’0457 m2 (→4)

MAGIC MAGIC (Germany, Italy & Spain)(Germany, Italy & Spain)1: Autumn 1: Autumn ‘‘0303236 m236 m22

((→→2)2)

In progress: MoU to balance between competition and cooperationIn progress: MoU to balance between competition and cooperation

Overlap of the ‘Big4’ allows for ~continuous observations Overlap of the ‘Big4’ allows for ~continuous observations

MACE 2010?

MAGIC

Grantecan

MAGIC and its Control House

Telescopio Nazionale Galileo

MAGIC

La Palma, IAC28° North, 18° West

MAGIC

The MAGIC site

MAGIC

17 m

17 m

ReflRefl. . surfacesurface::236 m236 m22, F/1, 17 m , F/1, 17 m ∅∅

–– 964 heated mirrors on 247 panels964 heated mirrors on 247 panels–– Lasers+mechanisms for AMCLasers+mechanisms for AMC

CameraCamera::~ 1 m ~ 1 m ∅∅, 3.5, 3.5°°FoVFoV576 PMT (QE576 PMT (QEMAXMAX ~ 30%)~ 30%)

AnalogicalAnalogicalTransmissionTransmission((opticaloptical fiberfiber))

22--level Trigger:level Trigger:11ºº levellevel: : coincidencecoincidence22ºº level: pattern recognitionlevel: pattern recognition300 300 MHzMHz DAQDAQ

RapidRapid pointingpointing–– Carbon fiber structureCarbon fiber structure–– Active Mirror ControlActive Mirror Control

⇒⇒ 2020÷÷30 30 secondsseconds

After upgrade of theoptics in July 2004

the telescope is in itsfinal shape

~300Hz shower ratesEth ~40GeV

the Active Mirror Control laser beams

Photo by R. Wagner

Photograph of the 576-pixel imaging camera of MAGIC-I.In the central part one can see the 396 high resolution pixelsof 0.1° size. Those are surrounded by 180 pixels of 0.2°.

The Major Atmospheric Gamma-ray ImagingCherenkov (MAGIC) telescope: parameters

956 0.5m x 0.5m aluminum mirrorsParabolic shapeDiameter: 17m – area: 240 m2f/D = 1Al mirrors + C fiber low weightSlew time ~ 20 sHexagonal camera: FOV: 3.8°

E(threshold) ~ 50 GeVSensitivity: 0.05 Crab in 50 hrsAngular resol.: 0.1 degEnergy resol.: 30%

World’s largest IACT => lowest threshold

SNRsSNRs

Cold Dark Cold Dark MatterMatter

PulsarsPulsarsGRBsGRBs

Quantum Gravity Quantum Gravity effectseffects

cosmologicalcosmologicalγγ--Ray HorizonRay Horizon

AGNsAGNs

The Physics Program and the first results

Origin of Origin of Cosmic RaysCosmic Rays

CrabStable γ source GeV/TeV (Whipple ‘89).Standard candle for gamma astronomy

Crab Nebula

HESS:~ 30 Time(h)

MAGIC :~ 20 Time(h)

σ

σ

×

×

MAGIC: Significant signalstarts at 50GeV (2h of observation).

3% Crab @ 5 in 25-50 hrsσ

Crab: reaching theinverse Compton peak

Synchrotron

I.C.

X-Ray I.R.

Measured on 20 decades

γ (MAGIC)

Preliminary

MAGIC

MAGIC scientific papers in 2006I: AGNs

1. “Observation of VHE γemission from the AGN 1ES1959+650 with MAGIC”, ApJ 639 (2006) 761.

2. “Discovery of VHE γ -ray emission from 1ES1218+30.4”, ApJ Lett. 642 (2006) 119.

3. “Observations of Mkn 421 with MAGIC”, astro-ph/0603478, accepted for publication in ApJ.

4. Detection of VHE radiation from the BL Lac PG 1553+113 with the MAGIC telescope, subm. to ApJ-L.

PG1553:source at z~0.3detected at 9σ

1ES1218 (z=0.18)New Source

PG 1553 (New source )

MAGIC scientific papers in 2006 II: SNRs and μQSR5. “MAGIC observations of

VHE γ -rays from HESS J1813-178”, ApJ Lett. 637 (2006) 41.

6. “Observation of VHE γradiation from HESS J1834-087/W41 with MAGIC”, ApJ Lett. 643 (2006) 53.

7. “Variable Very High Energy Gamma-Ray Emission from the μQSR LS I+61 303”, Science, May 2006.

Index –2.5 ± 0.2

90 cm VLA (green) + MAGIC (bck) + 12CO (black)

Source is Extended!

First μQSR at VHE (up to 5 TeV)Hint of periodicity over 6T

MAGIC scientific papers in 2006 - III

8. “Flux upper limit of γ-ray emission by GRB050713a from MAGIC”, ApJ Lett. 641 (2006)

9. “Observation of γ rays from the Galactic Center with MAGIC”, ApJ Lett. 638 (2006) 101.

+ 8 additional publications in the pipeline (including 3-4 new sources)

GRB050713aGRB050904 (in prompt phase)

And response timeIMPROVING!

Galactic Center

2min resolutionLight curve

Mkn501 giant flareBins of 2 min

Cycle1 (Feb 2005-Apr 2006)• Statistics of physics runs for Cycle1:

– 1070 hours dark time out of 1714, plus 150 h “good technical runs”, and 212 hours moon

• Moon time increasing to an asymptotical value ~1/3– ~100 hours ToO (with some important results)

• will increase with the increased number of collaborations– Suzaku, Swift, GLAST, AGILE, …

• All data analyzed– Papers published or submitted for all positive

signals, but 6 (Crab, Mkn501, x, y, z, t)• 2 GRB observations during the primary burst• MAGIC Catalog opened (MAGIC Jxxx-yyy)

Cycle2• From period 42, starting on May 14, 2006, to period

54, ending on May 29, 2007• 840 dark time hours recommended for observation

time in Class A, plus a maximum (?) of 236h for ToO– 46% to AGN– 28% to Galactic Sources– 9% to Pulsars– 14% to DM, including M87+ Special projects (τ neutrinos, …)

GRB fully accepted (36h ToO) – going towards a further improvement of the response time

Realistic goal for the performance of MAGIC in 2006 (single telescope)

10-14

10-13

10-12

10-11

10 100 1000 104 105

E x

F(>

E) [

TeV

/cm

2 s]

E [GeV]

Crab

10% Crab

1% Crab

GLAST

MAGIC

HESS

E.F(>E) [TeV/cm2s]

ExtragalacticSource Redshift Spectral Index Type Detection (>5σ) ConfimationM87 0.004 2.9 FR I HESSMkn 421 0.031 2.2 BL Lac Whipple ManyMkn 501 0.034 2.4 BL Lac Whipple Many1ES 2344+514 0.044 2.9 BL Lac Whipple HEGRA,MAGIC1ES 1959+650 0.047 2.4 BL Lac Tel. Array ManyPKS 2005-489 0.071 4.0 BL Lac HESSPKS 2155-304 0.116 3.3 BL Lac Mark VI HESSH1426+428 0.129 3.3 BL Lac Whipple ManyH2356-309 0.165 3.1 BL Lac HESS1ES 1218+304 0.182 3.0 BL Lac MAGIC1ES 1101-232 0.186 2.9 BL Lac HESSPG 1553 >0.25 4.0 BL Lac MAGIC

At least a handle on EBL, but also the possibility of accessing cosmological constants (Martinez et al.) could become reality soon (maybe including X-ray obs.)

‘Correlation’ of spectral slope vs redshift

Given IC peak, MAGIC bandpass will see range of spectral slopesHigh-z sources: only steep spectrum

Pian+1998

BL Lac objects

1.5

2.0

2.5

3.0

3.5

4.0

4.5

0 0.1 0.2 0.3 0.4Redshift Parameter z

Spec

tral

Inde

x

PKS2005 PG1553

New Sources

Pian+ 1998

Meas.t of EBL(z) from blazar spectra !

ForFor givengiven sourcesource, at , at redshiftredshift zz::• synchro (X-ray) ⊕ assumption IC (VHE-γ-ray)• intrinsic VHE-γ-ray spectra available• intrinsic vs observed spectrum ⇒⇒ EBLEBL

RepeatRepeat forfor severalseveral sourcessources, a , a variousvarious z:z:⇒⇒ EBL(EBL(zz))

need for coupled hard-X / VHE-γ obs’s(e.g., INTEGRAL / MAGIC)

need to lower energy threshold of IACTs(IC peak at <50-100 GeV)

GRH measurement is constraining the EBL density (and paving the way to a measurement of

cosmological parameters)Blanch & Martinez 2004

Simulatedmeasurements

Different EBL models

Mkn 421Mkn 501

1ES1959+650

PKS 2155-304H1426+428

PKS2005-489

1ES1218+3041ES1101-232H2356-309

Simulatedmeasurements

Mkn 421Mkn 501

1ES1959+650PKS2005-489 1ES1218+304

1ES1101-232

H2356-309PKS 2155-304H1426+428

• From a phenomenological point of view, the effect can be studied with a perturbative expansion. In first order, the arrival delay of γ−rays emitted simultaneously from a distant source should be proportional to their energy difference and the path L to the source:

• The expected delay is very small and to make it measurable one needs to observe very high energy γ-rays coming from sources at cosmological distances.

cL

EEtQG

Δ∼Δ

Tests of Quantum Gravity effects

GRB Observation

• MAGIC is the right instruments, due toits fast movement & low threshold– MAGIC is in the GCN Network– GRB alert active since Apr 2005– 8 useful triggers since

• For the first time with a usefulsensitivity MAGIC observed a GRB at high-energy symultaneously with the primary burst (for 30s)– GRB050713a (threshold of 120 GeV)– GRB050904 (threshold of 60 GeV)

High time-resolution study of AGN flare

• Huge Mkn 501 flare on 1st July 2005 -> 4 Crab intensity.

• Intensity variation in 2 minute bins -> new, much stronger, constraints on emission mechanism and light-speed dispersion relations (effective quantum gravity scale).

Preliminary

Preliminary 2 minutes time bins

Crab

Dark Matter

• meV candidates: non-directional, indirect (and subtle)– Might have implications on gamma rays [Bignami et al. 2005]

• GeV/TeV candidates: – direct (nondirectional) if we live in a sea of DM– indirect (directional) mostly through photons: where to look for?

• Photons are the main character of this story– Interaction between astrophysicists and experimentalists is the

key

The main field of research:Heavy WIMPs, indirect: self-annihilation

annihilation

into γγ or γZ:Eγ = mχ / mχ− mZ

2/4 mχ

=> clear signature at high energiesbut: loop suppressed

χ

χ

γ,Zγ

χ±,W

χ

χ q

qannihilation into qq -> jets -> n γ’s=> continuum of low energy gammasdifficult signature but large flux

Good energy resolution in the few % range is needed

But also: antimatter (positrons), neutrinos

γ-Flux from χ-Annihilation2

2

( , )( ) ( )DM

dN El dl

dtdAdEd Mγ

χ

α ρΩ

= ⋅ ΩΩ ∫

Astrophysics:γ-ray flux ~ ρ2

=> search for CDM clumps

Particle physics:SUSY modelsfragmentation functions

Prada, Flix, et al: astro-ph/0401512

pMSSM

DM density profiles: Cusp, Core, Clumps…

Navarro,Frenk & White (1996):αNFW = 1Moore (1998):αMoore = 1.5Stoehr (2004)α < 1

ρ(r) = ρ ors

rα 1 +rrs

⎛

⎝ ⎜

⎞

⎠ ⎟

3−α

gamma-flux dependence ρ2 => inner, high ρDM region dominatingCDM simulations:uncertainties

experimental data for GC (rotation curves, microlensing data, ..)

no evidence for cuspy profilecusp not unambiguously ruled out

predictions for ∫ρχ2(l)dl

differ by orders of magnitude

Galactic Center

Distance (7.5 kpc) GC best candidate for indirect DM searches ?

- other γ-ray sources in the FOV, i.e. SNR Sgr A East

- competing plausible scenarios

BUT:

- central halo DM density vs L relation: ρ0∝L-1

- halo core radius: extended vs point-like

Highest DM density candidate Close byNot extendedNot associated with known astrophysical object

Targets for DM search

1 degree

Subtracted Image

The Galactic Center

Contours of CS emission (molecular tracer)

– Source coincident with supermassiveblack hole Sgr A*

• Diffuse Emission– Emission along the

plane is revealed by subtraction of strong sources...

– Correlation with molecular material

• Cosmic rays interacting with molecular clouds

HESS

GC observed in VHE gamma by Cangaroo, HESS, MAGIC• HESS+MAGIC and Cangaroo results don’t match

Cangaroo spectral indexΓ=-4.6±0.5HESS spectral indexΓ=-2.63±0.04MAGIC 2005: Γ=-2.3±0.4flux: ~10% of Crabno apparent variability

10-9

10-8

10-7

0,1 1 10Energy [TeV]

E2dN

/dE

15 TeVWIMP6 TeV

WIMP

HESS, astro-ph/0408145

The Galactic Center MAGIC

>1 TeV

VLA

Gal. Eq.

Preliminary

Unbroken PL, index 2.3

Good agreement between HESS andMAGIC (large zenith angle observation)

⇒ strong γ-ray source to outshine DM signal ?⇒ most SUSY scenarios: cutoff in DM spectrum at a few TeV ??

Galactic Center: MAGIC MAGIC

DRACO dSph : Motivations- Milky Way surrounded by small, faint companion galaxies

- dSph’s very DM-dominated objects.

- detection most likely?

- Distances, M/L ratios 16<D/kpc<250, 30<M/L<300

DRACOhighest M/L

dwarf

Northern source

Mrk421

Mrk501

Crab

R.A.OngAug 2005

Pulsar Nebula

SNR

AGN

Other, UNID

The VHE Sky - 1995

Mrk421 H1426

Mrk5011ES1959

1ES 2344

PKS 2155

Cas ARXJ 1713

CrabTeV 2032

M87

GC

R.A.OngAug 2005

Pulsar Nebula

SNR

AGN

Other, UNID

The VHE Sky - 2003

+ 8-15 additional sourcesin galactic plane.

Nadia Tonello

Cherenkov TelescopesCherenkov Telescopes

HESS-II• New 28m telescope.• 2048 pixel camera.• Lower energy threshold (30 GeV?)• First light in 2008.

MAGIC-II• Improved 17m telescope.• Faster FADCs and a high-QE

camera.• First light in 2007.

MAGICMAGIC--II MAGICMAGIC--IIII

85m

Outlook: What next ? 1.

VERITAS• 4x 12m telescopes at Kitt-Peak in

2007 (2 now)

Veritas on Sept 4, 2005

The second MAGIC telescope

Mirrors: 1m2 layout

• Very similar to the small mirrors

Central hole for the laser housing

Mirror box + honeycomb

Front plate

Layout comparison

50 cm mirrors

1 m mirror

AMC motors

Layout comparison

Production steps

1.Raw blank assemblingFront plate glued with Al box and

honeycombAlready spherical shape

2. Diamond milling

3. Quartz layer surfacing

4. Ready! (7 mirrors already done in Padova, 2 in Munich)

Test on the mirror spot

• Results:

The rigidity of the new mirrors and the tune-up of the milling machine are delivering very good results

Spot is comparable to the one we had for

0.5m mirrors!0.5 cm

3 large mirrors already installed in Oct 05

winter has passed… and we manage the technique!

Outlook: What next ? 2.The Cherenkov

Telescope Array facility CTA

aims to explore the sky in the 10 GeV to 100 TeV energy range

builds on demonstrated technologies

combines guaranteed science with significant discovery potential

is a cornerstone towards a multi-messenger exploration of the nonthermal universe

Unifying European efforts

VERITAS

MAGIC

H.E.S.S.

… and maintaining European lead

CTA involves scientists fromCzech RepublicGermanyFranceItalyIrelandUKPolandSpainSwitzerlandArmeniaSouth AfricaNamibia

from several communitiesastronomy & astrophysicsparticle physicsnuclear physics

about 250-300 scientists workingcurrently in the field will bedirectly involved,user community significantly larger

few 1000 m

High-energy section~0.05% area coverage

Eth ~ 1-2 TeV

250 m

Medium-energy section~1% area coverage

Eth ~ 50-100 GeV

70 m

Low-energy section~10% area coverage

Eth ~ 10-20 GeV

Array layout: 2-3 Zones

FoV increasingto 8-10 degr.

in outer sections

Not to scale !

Option “off the shelf”: Mix of telescope types

Modes of operation• Deep wide-band mode: all

telescopes track the same source

• Survey mode: staggered fields of view survey sky

• Search & monitoring mode:subclusters track different sources

• Narrow-band mode: halo telescopes accumulate high-energy data, core telescopes hunt pulsars

Telescope structure “off the shelf” (but new ideas for large-field are welcome)

Proven:H.E.S.S. 12 m dish

Proven:MAGIC rapid-slewing 17 m dish(and new MAGIC, started)

Construction started:H.E.S.S. II 28 m dish0 10 m 20 m 30 m

Dish size

Cost /Dish Area

Cameracost dominates

Dish costdominates

(Very optimistic) Schedule

Telescope prototypes

Site exploration

Full operation

Partial operation

Array construction

Component prototypes

Array design

1312111009080706

GLAST

FP 7 Design Study

“Letter of Intent”(100 pages, physics + conceptual design)

Technicalproposal

• Working groups start meeting in June– Physics: A. De Angelis and L. Drury (convenors), G. Lamanna, F.

Aharonian, M. Teshima, K. Mannheim, D. Torres, G.F. Bertone, M. Punch, B. Giebels, …

– MC: K. Bernloher and E. Carmona (conv.), G. Hermann, G. Lamanna, S. Nolan, C. Bigongiari, A. Moralejo, W. Rhode, …

– Photon detector: T. Schweizer and P. Vincent (conv.), P. Goret, M. Punch, M. Teshima, E. Lorenz, N. Turini, …

– Choice of the site: B.K. and M. Teshima (conv.), G. Vasiliades, J. Cortina, …

– Mechanics and mirrors: M. Mariotti and M. Panter (conv.), E. Lorenz, A. Biland, P. Chadwick, O. de Jager, …

– DAQ and computing: A. Biland and U. Schwanke (conv.), F. Goebel, L. Drury, T. Brez, G. Cabras, …

Steering committee meeting on July 11th – 1st physics meet’ in July (Venezia or London) People interested please contact the convenors.

~3000 sourcesby GLAST, AGILE

~1000 sourcesby CTA

GLASTAGILE

RadioKAT,…

X-rays

HardX-rays

Gamma raysGLAST

CherenkovTelescopes

Multiwavelength / multimessenger astronomy

Multi-Messengers observationAll sky observatory (N,S stations)

Gamma Rays

Neutrinos

Gamma Ray &X-Ray Satellites

IceCube 2010: Completion of the construction

CTA North

CTA South

Conclusion• Breakthrough in VHE γ-ray astronomy: outstanding results from present

IACTs

• VHE γ-ray installations: observatories, no longer experiments VHE γ-ray astronomy established

– New VHE sources: more discovered last year than in the previous 20 years! ... more are coming

– SNRs, μQSO, pulsars particle acceleration – Blazars, EBL SSC model of jets, measure EBL, cosmological parameters– GRBs prompt emission detectable ( exotica: QG?)– Clusters structure formation– Indirect DM searches OK if WIMP parameters (density <- astrophysics; X-

section <- particle physics, SUSY) favorable (also GLAST)

• A further breakthrough NEEDS partnership with astronomers– Science (immediate)– Telescope design (the environment should be very receptive towards new ideas)