F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

Florian GoebelFlorian GoebelMax-Planck-Institut für PhysikMax-Planck-Institut für Physik(Werner-Heisenberg-Institut)(Werner-Heisenberg-Institut)

MünchenMünchen

for the for the

MAGIC collaborationMAGIC collaboration

International School of Cosmic Ray Astrophysics

Erice, 2-13. July 2004

The The MAGICMAGIC Telescope Telescope

MAGIC - talks in this session -

•Overview - F.Goebel

Selected physics topics•Pulsars - R. de los Reyes•AGNs - R. Firpo•Microquasars - N. Sidro•GRBs - S. Mizobuchi

First Analysis•Analysis method - D. Mazin•First results - E. Aliu

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

The The MAGICMAGIC telescope telescope

Largest Imaging Air Largest Imaging Air Cherenkov TelescopeCherenkov Telescope (17 m mirror dish)(17 m mirror dish)

Located on Canary Island Located on Canary Island La PalmaLa Palma (@ 2200 m asl) (@ 2200 m asl)

LowestLowest energy thresholdenergy threshold ever obtained with a ever obtained with a Cherenkov telescopeCherenkov telescope

Aim: detect Aim: detect –ray –ray sourcessources in the unexplored in the unexplored energy range: energy range: 30 30 (10)-> (10)-> 300 GeV300 GeV

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

The unexplored spectrum gapThe unexplored spectrum gap

Satellites give nice Satellites give nice crowded crowded picture of picture of –ray –ray energies up to 10 GeV.energies up to 10 GeV.

Effective area < 1 m2

Ground-based Ground-based experiments show very experiments show very few sourcesfew sources with energies with energies > ~300 GeV.> ~300 GeV.

Effective area > 104 m2

Close gap with MAGICexpect discovery of many new sources

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

AGNsAGNs

SNRsSNRs Cold Dark MatterCold Dark Matter

PulsarsPulsars

GRBsGRBs

Tests of Tests of Quantum Quantum Gravity effectsGravity effects

Cosmological Cosmological

-Ray -Ray HorizonHorizon

The The MAGICMAGIC Physics Program Physics Program

Origin of Origin of Cosmic Cosmic RaysRays

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

-rays-rays travelling cosmological distances travelling cosmological distances interact interact with the Extragalactic Background Light (EBL) Extragalactic Background Light (EBL)

Absorption of extragalactic Absorption of extragalactic - - raysrays

eeEBLHE 222 cmE e

Attenuated flux is function of Attenuated flux is function of -energy-energy and and source distance source distance (redshift z).(redshift z).

For IACTs energies (10 GeV-10 TeV), the For IACTs energies (10 GeV-10 TeV), the interaction takes place with interaction takes place with infrared infrared ’s (0.01 eV-3 eV, 100 (0.01 eV-3 eV, 100 m-0.5 m-0.5 m).m).

MAGIC

EBL

),()()(

zEeEE unabsorbedobserved

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

MAGIC phase I

MAGIC phase II

Gamma Ray HorizonGamma Ray Horizon

The EBL absorption limits the maximum observable distance of -ray sources.

A lower energy thresholds allows a deeper look into the universe

Gamma Ray Horizon

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

)()(4

)( 2

2dll

M

vNDM

Search for Dark Matter Particles Search for Dark Matter Particles

Neutralino Neutralino (lightest SUSY particle) is (lightest SUSY particle) is attractiveattractive Cold Dark Matter candidate Cold Dark Matter candidate

-flux from -flux from annihilations: annihilations:

)1100( TeVmGeV

qq

Z

-line E-line E = m = m

--line Eline E = m = mmm22mm

continuumcontinuum

Particle physics:

-continuum dominates-continuum dominates

--lines suppressed

CDM density:

-ray flux ~ -ray flux ~ 22 => => search for CDM clumpssearch for CDM clumps

observe: galactic center (high diffuse galactic center (high diffuse background),background), dwarf spheroidal and nearby galaxies,dwarf spheroidal and nearby galaxies, globular clusters globular clusters

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

Key Elements of the Key Elements of the MAGICMAGIC TelescopeTelescope

17 m diameter reflecting surface (240 m17 m diameter reflecting surface (240 m2 2 ))

Analog signal transport via Analog signal transport via optical fibers optical fibers

2-level trigger system2-level trigger system& 300 MHz FADC system& 300 MHz FADC system IPE

IPEIPE

CENET

Active mirror controlActive mirror control

Diamond milled aluminum mirrorsDiamond milled aluminum mirrors

Light weightCarbon fiberStructurefor fast repositioning 3.53.5oo FOV camera FOV camera

577 high QE PMTs577 high QE PMTs

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

The ReflectorThe Reflector

~950 spherical mirror elements ~950 spherical mirror elements 49.5 x 49.5 cm49.5 x 49.5 cm2 2

All-aluminumAll-aluminum, quartz coated, , quartz coated, diamond milleddiamond milled, internal heating, internal heating

>85% reflectivity>85% reflectivity (300- (300-650nm)650nm)

4 mirrors mounted on 1 panel4 mirrors mounted on 1 panel mirror spot (after pre-alignment): mirror spot (after pre-alignment):

d90%~1cm (pixelinner d=3cm)

overall reflector: overall reflector: parabolicparabolic (f/1), (f/1), isochronousisochronous,,

maintain time structure of maintain time structure of Cherenkov light flashes (~2 Cherenkov light flashes (~2 nsec)nsec)

better bkg light rejectionbetter bkg light rejection

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

The FrameThe Frame

carbon fiber carbon fiber structurestructure

lightweight lightweight dish & mirrors: 20 dish & mirrors: 20 tonstonstelescope: 65 tonstelescope: 65 tons

StiffStiff allows allows fast slewing fast slewing

time (time (180º in both axes 180º in both axes in 22sin 22s))

Fast follow-up of a Fast follow-up of a Gamma Ray BurstGamma Ray Burst

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

The Active Mirror Control The Active Mirror Control

PC controlled motors allow PC controlled motors allow remote refocusingremote refocusing of all of all mirror panels anytimemirror panels anytime

Correct for small Correct for small deformations of telescope deformations of telescope structurestructure

Achievable Point Spread Achievable Point Spread Function: Function: RR80 80 ~ 15mm ~ 15mm 0.05 0.05°° 0.9 0.9 mradmrad

Panel orientation measured Panel orientation measured with with laserlaser beam beam

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

The CameraThe Camera

Matrix of 577 PMTs Field of View: 3.50

Inner part: 0.10 pixel Outer part: 0.20 pixel

Plate of Plate of Winston conesWinston cones

Active camera area Active camera area 98%98%

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

High QE PMTsHigh QE PMTs

Pixels:Pixels: 6 stage PMTs6 stage PMTs

ET 9116A (1”)ET 9116A (1”) ET 9117A (1,5”) ET 9117A (1,5”)

Quantum Efficiency Quantum Efficiency increased up to increased up to 30 %30 % with with diffuse scattering coatingdiffuse scattering coating

extended UV sensitivity byextended UV sensitivity by withwith wavelength shifterwavelength shifter coatingcoating

239 m2 -> 284 m2 !!!

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

The Signal ProcessingThe Signal Processing

Stretch pulse to 6 nsecStretch pulse to 6 nsec Split to high & low gain Split to high & low gain

(dynamic range > 1000) (dynamic range > 1000) Digitize with Digitize with 300 MSamples/s300 MSamples/s

8 bit FlashADCs8 bit FlashADCs (testing 2GS/s)

Analog signalsAnalog signals transmitted transmitted over over 162 m162 m long long optical fiberoptical fiber::

Signal still Signal still shortshort Cable Cable weightweight, , noisenoise immune. immune.

Max trig rate ~ 1 kHz data rate => 20 MB/s => 800 GB/night

2 level trigger2 level trigger Fast (5 nsec) Fast (5 nsec) next neighbor next neighbor

logiclogic Slower (150 nsec) Slower (150 nsec) topological

pattern recognition

TWO FOLD KINDS (86) THREE FOLD KINDS (51)

FOUR FOLD KINDS (67) FIVE FOLD KINDS (106)

F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

Future of MAGIC observatoryFuture of MAGIC observatory

Second MAGIC type Second MAGIC type telescope under telescope under constructionconstruction(more observation (more observation time, background time, background rejection & better rejection & better event reconstruction in event reconstruction in coincidence mode)coincidence mode)

MAGIC I

Plans for 34 m telescope Plans for 34 m telescope for gamma astronomy for gamma astronomy down to down to E = 5 GeVE = 5 GeV ECO100

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