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The MAGIC Telescope

The MAGIC Telescope. I nternational School of Cosmic Ray Astrophysics Erice, 2-13. July 2004. 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

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The MAGIC Telescope

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  1. The MAGIC Telescope International School of Cosmic Ray Astrophysics Erice, 2-13. July 2004 • 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 Florian Goebel Max-Planck-Institut für Physik(Werner-Heisenberg-Institut) München for the MAGIC collaboration F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  2. The MAGIC telescope • Largest Imaging Air Cherenkov Telescope(17 m mirror dish) • Located on Canary Island La Palma (@ 2200 m asl) • Lowestenergy threshold ever obtained with a Cherenkov telescope • Aim: detect –ray sources in the unexplored energy range: 30 (10)-> 300 GeV F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  3. Satellites give nice crowded picture of –ray energies up to 10 GeV. • Ground-based experiments show very few sources with energies > ~300 GeV. Effective area > 104 m2 Close gap with MAGIC expect discovery of many new sources The unexplored spectrum gap Effective area < 1 m2 F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  4. The MAGIC Physics Program • Cosmological g-Ray Horizon • AGNs • Pulsars • Origin of Cosmic Rays • Tests of Quantum Gravity effects • SNRs • Cold Dark Matter • GRBs F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  5. EBL MAGIC Absorption of extragalactic  - rays -rays travelling cosmological distances interact with the Extragalactic Background Light (EBL) For IACTs energies (10 GeV-10 TeV), the interaction takes place with infrared ’s (0.01 eV-3 eV, 100 m-0.5 m). Attenuated flux is function of g-energy and source distance (redshift z). F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  6. MAGIC phase I MAGIC phase II Gamma Ray Horizon The EBL absorption limits the maximum observable distance of g-ray sources. Gamma Ray Horizon A lower energy thresholds allows a deeper look into the universe F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  7. CDM density: Particle physics: g-ray flux ~ r2 => search for CDM clumps observe: galactic center (high diffuse g background),dwarf spheroidal and nearby galaxies,globular clusters g-line Eg = mc g-line Eg = mc- mZ2/4 mc g continuum g-linessuppressed g-continuum dominates Search for Dark Matter Particles • Neutralino (lightest SUSY particle) is attractive Cold Dark Matter candidate g-flux from c annihilations: F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  8. 17 m diameter reflecting surface (240 m2 ) • Diamond milled aluminum mirrors • Active mirror control IPE Light weight Carbon fiber Structure for fast repositioning IPE IPE • 3.5o FOV camera 577 high QE PMTs NET CE • Analog signal transport via optical fibers • 2-level trigger system& 300 MHz FADC system Key Elements of the MAGIC Telescope F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  9. ~950 spherical mirror elements 49.5 x 49.5 cm2 All-aluminum, quartz coated, diamond milled, internal heating >85% reflectivity (300-650nm) • 4 mirrors mounted on 1 panel • mirror spot (after pre-alignment): d90%~1cm(pixelinner d=3cm) overall reflector: • parabolic (f/1), isochronous, • maintain time structure of Cherenkov light flashes (~2 nsec) • better bkg light rejection The Reflector F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  10. The Frame • carbon fiber structure • lightweight dish & mirrors: 20 tonstelescope: 65 tons • Stiff • allows fast slewing time (180º in both axes in 22s) • Fast follow-up of a Gamma Ray Burst F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  11. PC controlled motors allow remote refocusing of all mirror panels anytime Correct for small deformations of telescope structure The Active Mirror Control • Panel orientation measured with laser beam • Achievable Point Spread Function: R80 ~ 15mm  0.05°  0.9 mrad F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  12. Matrix of 577 PMTs Field of View: 3.50 Inner part: 0.10 pixel Outer part: 0.20 pixel The Camera Plate of Winston cones  Active camera area 98% F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  13. Quantum Efficiency increased up to 30 % with diffuse scattering coating • extended UV sensitivity bywithwavelength shiftercoating High QE PMTs Pixels: • 6 stage PMTs • ET 9116A (1”) • ET 9117A (1,5”) 239 m2 -> 284 m2 !!! F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  14. Max trig rate ~ 1 kHz data rate => 20 MB/s => 800 GB/night • 2 level trigger • Fast (5 nsec) next neighbor logic • Slower (150 nsec) topological pattern recognition The Signal Processing • Analog signals transmitted over 162 m long optical fiber: • Signal still short • Cable weight, noise immune. • Stretch pulse to 6 nsec • Split to high & low gain (dynamic range > 1000) • Digitize with 300 MSamples/s8 bit FlashADCs(testing 2GS/s) F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

  15. MAGIC I • Plans for 34 m telescope for gamma astronomy down to E = 5 GeV ECO1000 Future of MAGIC observatory • Second MAGIC type telescope under construction(more observation time, background rejection & better event reconstruction in coincidence mode) F. Goebel, MPI München, 2-13 July 2004, ISCRA, Erice

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