alessandro de angelis brera, june 2006
TRANSCRIPT
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)