The MAGIC Project: Performance of the 1st telescope

1. The MAGIC Project: Performance of the 1st telescope Razmick Mirzoyan On behalf of the MAGIC Collaboration Max-Planck-Institute for Physics Munich, Germany R.Mirzoyan: CTA meeting, Berlin

2. MAGIC-I at ORM in La Palma • First presentations in 1995, for example,24th ICRC, Rome, (Bradbury et al.) • Design study: spring 1998 • Approval of funding late 2000 • Start of construction 2001 • Inauguration October 2003 • Comissioning late summer 2004 • Regular observations: early fall 2004 R.Mirzoyan: CTA meeting, Berlin

3. 6 dynode PMTs (low gain) from Electron Tubes, England central 0.1° PMTs: 397 edge 0.2° PMTs: 180 Quantum Efficiency is up to30 %by using milkydiffuse scattering coating enhanced UV sensitivity usingwavelength shiftercoating Imaging Camera • Field of View: 3.50 Temperature stabilisation by cooled-down water flow through the skin of camera 240 m2 -> 312 m2 !!! R.Mirzoyan: CTA meeting, Berlin

4. Trigger architecture L0 =>Computer controlled discriminators + Single pixel rate online monitor L1 =>fast coincidence simple topology trigger (2-3-4-5 NN logic) 4-6ns gate L2 =>digital pattern selection made with tree structured lookup table system (20ns gate) pixel counitng in compact regions hot pixels mask higer topological constraint …. Prescaler => Final combination of different trigger tables with a prescale factor R.Mirzoyan: CTA meeting, Berlin

5. Rates • During observations the trigger rate is about 250-300 Hz. • Standard trigger condition is „any ≥ 4NN pixels above a threshold of ~ 8-10 ph.e.“ • Depending on the analyses cuts the g rate from Crab Nebula is about 8-10 events in one minute. • An up-time of 90-95 % for observations has been achieved in good weather months. R.Mirzoyan: CTA meeting, Berlin

6. Without AMC Tracking of Jupiter With AMC achieved PSF: 90% of light contained in 0.1° size inner pixel Active Mirror Control Light-weight structure requires zenith angle dependent corrections of deformations of the reflector shape R.Mirzoyan: CTA meeting, Berlin

7. Angular Resolution • angular resolution: 0.1o • DISP method R.Mirzoyan: CTA meeting, Berlin

8. Energy resolution • Image SIZE (S ph.e.) together with several other parameters is used for energy estimation • optimized estimator using Random Forest technique • 20% (30%) @ 1 TeV (100 GeV) R.Mirzoyan: CTA meeting, Berlin

9. Sensitivity MAGIC-I • Trigger threshold ~ 50GeV • Sensitivity: 2.5% Crab for • E>100GeV (5,50h) • or 22 s/h • ~ 15 galactic and extragalactic sources are detected or discovered(see the talk by Masahiro), interesting publications already appeared/are queing Mkn-501 July 1st 2005 1h ON Z.A.: 15°-25° Size > 360 ph.e. (E > 200 GeV) acut < 6° Excess ev.: 648 Significance: 41s R.Mirzoyan: CTA meeting, Berlin

10. The2nd improved telescope is being build • to double the sensitivity and • to help to lower the energy threshold further down MAGIC-II MAGIC - II MAGIC-I R.Mirzoyan: CTA meeting, Berlin

11. Conclusions • Since ~ 1.5 years we are observing with MAGIC-I. We have achieved smooth operational condition. • ~15 sources (new and known) have been detected, publications are queing. • For the time being we can analyse sorces down to ~ 80 GeV, we are working to lower the threshold further down. • New technologies, used in MAGIC-I, performe satisfactory. In the past we needed to improve the AMC system, especially by making the electronics water-tight. • MAGIC-II will include improvements that we learnt from MAGIC-I. • In 2007 we are going to opearte 2 telescopes in coincidence; that‘s going to double the sensitivity. R.Mirzoyan: CTA meeting, Berlin