MAGIC (telescope)

This article is about the telescope. For other uses, see Magic (disambiguation).
MAGIC 1

The first MAGIC telescope
Organisation MAGIC collaboration
Location(s) La Palma, Canary Islands
Coordinates 28°45′43″N 17°53′24″W / 28.761944444444°N 17.89°W / 28.761944444444; -17.89Coordinates: 28°45′43″N 17°53′24″W / 28.761944444444°N 17.89°W / 28.761944444444; -17.89
Altitude 2200 m
Wavelength Gamma rays (indirectly)
Built 2004
Telescope style Reflector
Diameter 17 m
Collecting area 240 m2
Focal length f/D 1.03
Mounting metal structure
Website http://wwwmagic.mppmu.mpg.de/

MAGIC (Major Atmospheric Gamma Imaging Cherenkov Telescopes) is a system of two Imaging Atmospheric Cherenkov telescopes situated at the Roque de los Muchachos Observatory on La Palma, one of the Canary Islands, at about 2200 m above sea level. MAGIC detects particle showers released by gamma rays, using the Cherenkov radiation, i.e., faint light radiated by the charged particles in the showers. With a diameter of 17 meters for the reflecting surface, it was the largest in the world before the construction of H.E.S.S. II.

The first telescope was built in 2004 and operated for five years in standalone mode. A second MAGIC telescope (MAGIC-II), at a distance of 85 m from the first one, started taking data in July 2009. Together they integrate the MAGIC telescope stereoscopic system.[1]

MAGIC is sensitive to cosmic gamma rays with energies between 50 GeV (later lowered to 25 GeV) and 30 TeV due to its large mirror; other ground-based gamma-ray telescopes typically observe gamma energies above 200...300 GeV. Satellite-based detectors detect gamma-rays in the energy range from keV up to several GeV.

Aims

The goals of the telescope are to detect and study primarily photons coming from:

Observations

MAGIC has found pulsed gamma-rays at energies higher than 25 GeV coming from the Crab Pulsar.[4] The presence of such high energies indicates that the gamma-ray source is far out in the pulsar's magnetosphere, in contradiction with many models.

MAGIC detected[5] very high energy cosmic rays from the quasar 3C 279, which is 5 billion light years from Earth. This doubles the previous record distance from which very high energy cosmic rays have been detected. The signal indicated that the universe is more transparent than previously thought based on data from optical and infrared telescopes.

MAGIC did not observe cosmic rays resulting from dark matter decays in the dwarf galaxy Draco.[6] This strengthens the known constraints on dark matter models.

A much more controversial observation is an energy dependence in the speed of light of cosmic rays coming from a short burst of the blazar Markarian 501 on July 9, 2005. Photons with energies between 1.2 and 10 TeV arrived 4 minutes after those in a band between 0.25 and 0.6 TeV. The average delay was 30 ±12 ms per GeV of energy of the photon. If the relation between the space velocity of a photon and its energy is linear, then this translates into the fractional difference in the speed of light being equal to minus the photon's energy divided by 2×1017 GeV. The researchers have suggested that the delay could be explained by the presence of quantum foam, the irregular structure of which might slow down photons by minuscule amounts only detectable at cosmic distances such as in the case of the blazar.[7]

Technical specifications

MAGIC on a sunny day
Individual segments of a MAGIC telescope

Each telescope has the following specifications:

Each mirror of the reflector is a sandwich of an aluminum honeycomb, 5 mm plate of AlMgSi alloy, covered with a thin layer of quartz to protect the mirror surface from aging. The mirrors have spherical shape with a curvature corresponding to the position of the plate in the paraboloid reflector. The reflectivity of the mirrors is around 90%. The focal spot has a size of roughly half a pixel size (<0.05°).

Directing the telescope to different elevation angles causes the reflector to deviate from its ideal shape due to the gravity. To counteract this deformation, the telescope is equipped with Active Mirror Control system. Each four mirrors are mounted on a single panel, which equipped with actuators that can adjust its orientation in the frame.

The signal from the detector is transmitted over 162 m long optical fibers. The signal is digitized and stored in 32kB ring buffer. The readout of the ring buffer results in a dead time 20 µs, which corresponds to about 2% dead time at the design trigger rate of 1 kHz. The readout is controlled by an FPGA (Xilinx) chip on a PCI (MicroEnable) card. The data are saved to a RAID0 disk system at a rate up to 20 MB/s, which results in up to 800 GB raw data per night.[8]

Collaborating Institutions

During foggy nights, the laser reference beams of MAGIC's active control could be seen. However, they are no longer needed for operation.

Physicists from over twenty institutions in Germany, Spain, Italy, Switzerland, Croatia, Finland, Poland, Bulgaria and Armenia collaborate in using MAGIC; the largest groups are at

References

  1. ↑ "Technical status of the MAGIC telescopes", MAGIC collaboration, Proc. International Cosmic Rays Conference 2009, arXiv:0907.1211
  2. ↑ Albert, J. (2006). "Variable Very-High-Energy Gamma-Ray Emission from the Microquasar LS I +61 303". Science 312 (5781): 1771–3. arXiv:astro-ph/0605549. Bibcode:2006Sci...312.1771A. doi:10.1126/science.1128177. PMID 16709745.
  3. ↑ Albert, J.; Aliu, E.; Anderhub, H.; Antoranz, P.; Armada, A.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J. K.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Bock, R. K.; Bordas, P.; Bosch-Ramon, V.; Bretz, T.; Britvitch, I.; Camara, M.; Carmona, E.; Chilingarian, A.; Coarasa, J. A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; Curtef, V.; Danielyan, V.; et al. (2007). "Very High Energy Gamma-Ray Radiation from the Stellar Mass Black Hole Binary Cygnus X-1". The Astrophysical Journal 665: L51. arXiv:0706.1505. Bibcode:2007ApJ...665L..51A. doi:10.1086/521145.
  4. ↑ Aliu, E.; Anderhub, H.; Antonelli, L. A.; Antoranz, P.; Backes, M.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J. K.; Bednarek, W.; Berger, K.; Bernardini, E.; Bigongiari, C.; Biland, A.; Bock, R. K.; Bonnoli, G.; Bordas, P.; Bosch-Ramon, V.; Bretz, T.; Britvitch, I.; Camara, M.; Carmona, E.; Chilingarian, A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; Covino, S.; et al. (2008). "Observation of Pulsed -Rays Above 25 GeV from the Crab Pulsar with MAGIC". Science 322 (5905): 1221–1224. arXiv:0809.2998. Bibcode:2008Sci...322.1221A. doi:10.1126/science.1164718.
  5. ↑ Albert, J.; Aliu, E.; Anderhub, H.; Antonelli, L. A.; Antoranz, P.; Backes, M.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J. K.; Bednarek, W.; Berger, K.; Bernardini, E.; Bigongiari, C.; Biland, A.; Bock, R. K.; Bonnoli, G.; Bordas, P.; Bosch-Ramon, V.; Bretz, T.; Britvitch, I.; Camara, M.; Carmona, E.; Chilingarian, A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; et al. (2008). "Very-High-Energy Gamma Rays from a Distant Quasar: How Transparent is the Universe?". Science 320 (5884): 1752–4. arXiv:0807.2822. Bibcode:2008Sci...320.1752M. doi:10.1126/science.1157087. PMID 18583607.
  6. ↑ Albert, J.; Aliu, E.; Anderhub, H.; Antoranz, P.; Backes, M.; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J. K.; Bednarek, W.; Berger, K.; Bigongiari, C.; Biland, A.; Bock, R. K.; Bordas, P.; Bosch‐Ramon, V.; Bretz, T.; Britvitch, I.; Camara, M.; Carmona, E.; Chilingarian, A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; Curtef, V.; Danielyan, V.; Dazzi, F.; De Angelis, A. (2008). "Upper Limit for γ‐Ray Emission above 140 GeV from the Dwarf Spheroidal Galaxy Draco". The Astrophysical Journal 679: 428–431. arXiv:0711.2574. Bibcode:2008ApJ...679..428A. doi:10.1086/529135.
  7. ↑ "Gamma Ray Delay May Be Sign of 'New Physics'".
  8. 1 2 Cortina, J.; for the MAGIC collaboration (2004). "Status and First Results of the MAGIC Telescope". Astrophysics and Space Science 297 (2005): 245–255. arXiv:astro-ph/0407475. Bibcode:2005Ap&SS.297..245C. doi:10.1007/s10509-005-7627-5.

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