The MAGIC Project:
1 / 11

The MAGIC Project: Performance of the 1st telescope - PowerPoint PPT Presentation

  • Uploaded on

The MAGIC Project: Performance of the 1st telescope. Razmick Mirzoyan On behalf of the MAGIC Collaboration Max-Planck-Institute for Physics Munich, Germany. MAGIC-I at ORM in La Palma. First presentation s in 19 95 , for example, 24th ICRC, Rome , ( Bradbury et al . )

I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
Download Presentation

PowerPoint Slideshow about 'The MAGIC Project: Performance of the 1st telescope' - abiba

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.

- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
The magic project performance of the 1st telescope

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

Magic i at orm in la palma
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

Imaging camera

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

Trigger architecture
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


  • 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

Active mirror control

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

Angular resolution
Angular Resolution

  • angular resolution: 0.1o

  • DISP method

R.Mirzoyan: CTA meeting, Berlin

Energy resolution
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



  • 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

The magic project performance of the 1st telescope

The2nd improved telescope is being build

  • to double the sensitivity and

  • to help to lower the energy threshold further down




R.Mirzoyan: CTA meeting, Berlin


  • 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