1. 17 November 2003EUSO meeting: R. Mirzoyan The MAGIC Telescope Project Razmick Mirzoyan Max-Planck-Institute for Physics Munich, Germany EUSO meeting

2. 17 November 2003EUSO meeting: R. Mirzoyan MAGIC-I: inaugurated recently, on October 10 Location: Canary island La Palma

3. 17 November 2003EUSO meeting: R. Mirzoyan We hope to take the 1 st gamma ray data from the Crab Nebula in the coming 2 months

4. 17 November 2003EUSO meeting: R. Mirzoyan Dense fog (or a cloud) helps to visualize the Active Mirror Control laser pointer beams Photo by R. Wagner

5. 17 November 2003EUSO meeting: R. Mirzoyan Outline The MAGIC Collaboration –Aiming for low threshold –Physics goals The Telescope –Design overview –MAGIC Key elements for low threshold –Status of commissioning of the telescope elements Plans & Conclusions

6. 17 November 2003EUSO meeting: R. Mirzoyan The MAGIC project First presentation in 95 at the ICRC, Rome, (Bradbury et al) Approval of funding only late 2000 Start of construction in 2001 Now commissioning Inauguration October 10th

7. 17 November 2003EUSO meeting: R. Mirzoyan Barcelona IFAE, Barcelona UAB, Crimean Observatory, U.C. Davis, U. Lodz, UCM Madrid, INR Moscow, MPI Munich, INFN/ U. Padua, INFN/ U. Siena U. Siegen, Tuorla Observatory, Yerevan Phys. Institute, INFN/U. Udine, U. Wuerzburg, ETH Zurich The MAGIC Collaboration Major Major Atmospheric Atmospheric Gamma-Ray Gamma-Ray Imaging Imaging Cherenkov Cherenkov Telescope n MAGIC is an international collaboration operating a 17 m Cherenkov Telescope for observation of HE cosmic  –rays. n Main aim: to detect  –ray sources in the unexplored energy range: 30 (10)-> 250 GeV MAGIC is a challenging design to decrease the energy threshold, by 1) increasing the mirror size 2) using improved optics, light sensors and electronics 3) using advanced trigger MAGIC is a challenging design to decrease the energy threshold, by 1) increasing the mirror size 2) using improved optics, light sensors and electronics 3) using advanced trigger � MAGIC shall provide the lowest threshold ever obtained with a Cherenkov telescope !!!

8. 17 November 2003EUSO meeting: R. Mirzoyan The MAGIC PHYSICS Goals n AGNs n SNRs n Cold Dark Matter n Pulsars n GRBs n Tests on Quantum Gravity effects Cosmological  ray horizon Cosmological  ray horizon Origin of Cosmic Rays

9. 17 November 2003EUSO meeting: R. Mirzoyan Key elements of the MAGIC telescope 577 pixels enhanced QE, ~4° deg FOV camera + advanced calibration system 3-level advanced trigger system Analog optical signal transport via 162m long fibres Light weight carbon fibre frameLight weight carbon fibre frame 17 m diameter reflecting surface (240 m 2 ) Active mirror control

10. 17 November 2003EUSO meeting: R. Mirzoyan Any  that crosses cosmological distances through the universe interacts with the EBL Absorption of extragalactic  - rays Attenuated flux function of  -energy and redshift z. For the energy range of IACTs (10 GeV-10 TeV), the interaction takes place with the infrared (0.01 eV-3 eV, 100  m-0.4  m). Star formation, Radiation of stars, Absorption and reemission by ISM MAGIC By measuring the cutoffs in the spectra of AGNs, MAGIC can help in determining the IR background EBL

11. 17 November 2003EUSO meeting: R. Mirzoyan This produces a reduction factor e -  in the  ray flux. The GRH is defined as the “z” for the observed energy “E” that fulfils: Optical Depth The probability of being absorbed for HE gamma crossing the universe is the integration of the cross-section over the incident angle and along the path from its origin to the observation. Gamma Ray Horizon (GRH) i.e. a reduction 1/e of the flux of the extragalactic source. Optical Depth & GRH MAGIC phase I MAGIC phase II

12. 17 November 2003EUSO meeting: R. Mirzoyan MAGIC Expected sources MAGIC is just starting to operate, therefore it is still a mystery how many extragalactic sources we would detect. One can use the EGRET catalogue to pick the probable source candidates. By using 50 hours of observation time for each of these candidates, because of high sensitivity we expect to be able to measure the GRH at different redshifts with MAGIC.

13. 17 November 2003EUSO meeting: R. Mirzoyan Pulsars Where do  -rays come from? Outer gap or polar cap? nMany of the ~170 EGRET unidentified sources may be pulsars. 7  -ray pulsars seen by EGRET. Only upper limits from present IACTs (spectral cut-off) 7  -ray pulsars seen by EGRET. Only upper limits from present IACTs (spectral cut-off) 4-fold nn-logic

14. 17 November 2003EUSO meeting: R. Mirzoyan Gamma Ray Bursts Mechanism not yet fully resolved. MAGIC can take advantage of: –Huge collection area –Fast repositioning. Low energy threshold Under the assumption that it is possible to extrapolate the GRB energy spectrum in the GeV region, MAGIC can observe 2-3 GRB/year MAGIC is designed to observe the prompt emission of a GRB!

15. 17 November 2003EUSO meeting: R. Mirzoyan Other Physics targets for MAGIC n Search for neutralino annihilation gamma-rays (galactic center, neighboring galaxies, globular clusters) n Tests of possible Lorentz invariance violation: search for delay of HE gamma rays in rapidly varying phenomena at large distances (AGN flares, GRBs)

16. 17 November 2003EUSO meeting: R. Mirzoyan Given the huge sensitivity, MAGIC can observe fast transient phenomena like GRB and/or flare of AGN. Test of invariance of speed of light Quantum Gravity models predict energy dispersion of c. Non trivial dispersion relation where E QG appears! (10 16 -10 19 ) Photon delay depending on energy over distance 10 s delay Lorenz Invariance Violation S.D. Biller et al. PhRev Let 83, 2108 (1999) E QG > 6  10 16 GeV

17. 17 November 2003EUSO meeting: R. Mirzoyan The frame The 17m diameter f/1 telescope frame is a lightweight carbon fiber structure (tube and knot system) The foundation started in September 2001 and the telescope frame was completed in Dec. 2001. The assembly of the frame took ~2 months

18. 17 November 2003EUSO meeting: R. Mirzoyan The reflector Tessellated surface: –~950 mirror elements –49.5 x 49.5 cm 2 (~240 m 2 ) –All-aluminium, quartz coated, diamond milled, internal heating –>85% reflectivity in 300-650nm The overall reflector shape is parabolic (f/1), isochronous, to maintain the time structure of Cherenkov light flashes in the camera plane –Better light of night sky rejection (less pile-up)

19. 17 November 2003EUSO meeting: R. Mirzoyan Optical alignment 4 mirrors spots after the pre-alignment close to the virtual center of the MAGIC camera Final spot of a panel after The precise alignment of the mirrors

20. 17 November 2003EUSO meeting: R. Mirzoyan The Active Mirror Control The panels can be oriented during the telescope operation through an Active Mirror Control system (AMC) to correct for possible deformation of the telescope structure

21. 17 November 2003EUSO meeting: R. Mirzoyan The alignment of the mirrors The alignment of the first 103 mirrors in the telescope structure has been done by using a 20 W light source at a distance of 920m The camera plane was moved 29 cm backward to focus the lamp light 103 spots before and after the alignment ~1 pixel

22. 17 November 2003EUSO meeting: R. Mirzoyan The camera Two sections: –Inner part: 0.10 0 PMTs –Outer part: 0.20 0 PMTs Plate of Winston cones  Active camera area  95 % Plate of Winston cones  Active camera area  95 % n includes 577 PMTs

23. 17 November 2003EUSO meeting: R. Mirzoyan The camera Pixels: The photocatode QE is enhanced up to 30 % and extended to UV by a special coating of PM surface with milky wavelength shifter The photocatode QE is enhanced up to 30 % and extended to UV by a special coating of PM surface with milky wavelength shifter Each PM is connected to an ultrafast low-noise transimpedance preamp.Each PM is connected to an ultrafast low-noise transimpedance preamp. 6-dynode HV system zener stabilized with an active load6-dynode HV system zener stabilized with an active load 240 m 2 -> 312 m 2 !!!

24. 17 November 2003EUSO meeting: R. Mirzoyan The readout Cherenkov light pulses from air showers are typically ~ 2-5 ns long Pixel signals are modulating the VCSEL lasers @850 nm and thus transported over 162 m multimode optical fibres to the counting house: –Very low dispersion –Low weight, noise inmune. Sampling using 300 Msample/s FlashADCs: –  /h discrimination through signal shape –LONS pick-up reduction –Event buffering, telescope system synchronization...

25. 17 November 2003EUSO meeting: R. Mirzoyan Trigger Two level trigger system The level 1 (L1) is a fast coincidence device (2-5 ns) with simple patterns (N-next-neighbour logic) on single trigger cells. Level 2 (L2) is slower (50-150 ns), and can perform a global sophisticated pattern recognition Two level trigger system The level 1 (L1) is a fast coincidence device (2-5 ns) with simple patterns (N-next-neighbour logic) on single trigger cells. Level 2 (L2) is slower (50-150 ns), and can perform a global sophisticated pattern recognition Discriminators L0 Discriminators L0 Set the minimum number of photoelectrons per pixel to be used in the trigger Level 2 L2 Level 2 L2 Perform an advanced pattern recognition to use topological constraint: pixel counting in a given region of the detector mask hot spots like bright stars rough image reconstruction, etc…. On-line event selection To FADC Level 1 L1 Level 1 L1 Make a tight time coincidence on simple pattern of compact images and enable L2

26. 17 November 2003EUSO meeting: R. Mirzoyan Trigger  - 44 GeV Trigger display L2 pattern recognition Off-line On-line On-line image analysis on the trigger event Off-line analysis

27. 17 November 2003EUSO meeting: R. Mirzoyan The Data Acquisition System Needs: –577 PMT x 1 Byte x 30 samples x 1 kHz  ~ 20 MByte/s (x 11 hours )  ~ 800 GB/night (longest nights in December) Cheap PC based solution: –Multiprocessor threaded system. –PCI FPGA based readout card & RAID0 disks system.

28. 17 November 2003EUSO meeting: R. Mirzoyan GRB alert from satellites: prompt follow-up The light weight structure and the low inertia of the structure allows a fast slewing time in such a way that the telescope will be able to perform an early follow-up of a Gamma Ray Burst With the motors running at 70% of full power, the telescope is able to turn 180º in both axes in less than 22s

29. 17 November 2003EUSO meeting: R. Mirzoyan Near Future Plans: MAGIC-I Winter 2003- spring 2004: System debugging & Start regular observations Step-by-step lowering of the threshold setting towards few 10’s of GeV

30. 17 November 2003EUSO meeting: R. Mirzoyan Near Future Plans: MAGIC-II Just now ordering the frame structure for the MAGIC-II telescope. The frame with understructure shall be ready in La Palma in May 2005, the 2nd Telescope to be completed near the end of 2005. The 2 nd telescope will essentially be the clone of the 1 st telescope, only a few improvements will be implemented. This will save us time and finances.

31. 17 November 2003EUSO meeting: R. Mirzoyan Conclusions So far all the new technical and technological novelties implemented in MAGIC behave as expected In the next few month we will make extensive tests of the apparatus with engineering and physics runs We are considering MAGIC as the first element of an international observatory to study the deep universe with high energy gamma rays. Construction of the 2 nd telescope has already been started. Our proposal is to transform the MAGIC site, Roque de los Muchachos, in the “European Cherenkov Observatory” ECO