May 4th 2006R.Mirzoyan: CTA meeting, Berlin The MAGIC Project: Performance of the 1st telescope Razmick Mirzoyan On behalf of the MAGIC Collaboration Max-Planck-Institute for Physics Munich, Germany

May 4th 2006R.Mirzoyan: CTA meeting, Berlin 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

May 4th 2006R.Mirzoyan: CTA meeting, Berlin Imaging Camera Field of View: dynode PMTs (low gain) from Electron Tubes, England central 0.1° PMTs: 397 edge 0.2° PMTs: 180 Quantum Efficiency is up to 30 % by using milky diffuse scattering coating enhanced UV sensitivity using wavelength shifter coating 240 m 2 -> 312 m 2 !!! Temperature stabilisation by cooled-down water flow through the skin of camera

May 4th 2006R.Mirzoyan: CTA meeting, Berlin Trigger architecture L0 => L0 => Computer controlled discriminators + Single pixel rate online monitor L1 => fast coincidence simple topology trigger ( NN logic) 4-6ns gate L2 => 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 => Prescaler => Final combination of different trigger tables with a prescale factor

May 4th 2006R.Mirzoyan: CTA meeting, Berlin Rates During observations the trigger rate is about Hz. Standard trigger condition is „any ≥ 4NN pixels above a threshold of ~ 8-10 ph.e.“ Depending on the analyses cuts the  rate from Crab Nebula is about 8-10 events in one minute. An up-time of % for observations has been achieved in good weather months.

May 4th 2006R.Mirzoyan: CTA meeting, Berlin Active Mirror Control Light-weight structure requires zenith angle dependent corrections of deformations of the reflector shape achieved PSF: 90% of light contained in 0.1° size inner pixel Tracking of Jupiter With AMC Without AMC

May 4th 2006R.Mirzoyan: CTA meeting, Berlin Angular Resolution DISP method angular resolution: 0.1 o

May 4th 2006R.Mirzoyan: CTA meeting, Berlin Energy resolution Image SIZE  ph.e.  together with several other parameters is used for energy estimation optimized estimator using Random Forest technique 20% 1 TeV (100 GeV)

May 4th 2006R.Mirzoyan: CTA meeting, Berlin Sensitivity Trigger threshold ~ 50GeV –Sensitivity: 2.5% Crab for – E > 100GeV (5 , 50h) –or 22  h ~ 15 galactic and extragalactic sources are detected or discovered (see the talk by Masahiro), interesting publications already appeared/are queing MAGIC-I 1 h ON Z.A.: 15°-25° Size > 360 ph.e. (E > 200 GeV)  cut < 6° Excess ev.: 648 Significance: 41  Mkn  July 1 st 2005

May 4th 2006R.Mirzoyan: CTA meeting, Berlin MAGIC-I MAGIC-II The 2nd improved telescope is being build –to double the sensitivity and –to help to lower the energy threshold further down MAGIC - II

May 4th 2006R.Mirzoyan: CTA meeting, Berlin 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.