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Air Cherenkov Methods in Cosmic Rays: A Review and Some History

Air Cherenkov Methods in Cosmic Rays: A Review and Some History. A.S. Lidvansky, Institute for Nuclear Research, Moscow. The Vavilov-Cherenkov radiation of high energy cosmic rays in air:.

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Air Cherenkov Methods in Cosmic Rays: A Review and Some History

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  1. Air Cherenkov Methods in Cosmic Rays: A Review and Some History A.S. Lidvansky, Institute for Nuclear Research, Moscow

  2. The Vavilov-Cherenkov radiation of high energy cosmic rays in air: • Only extensive air showers (EAS) can produce sufficient signal to be observed against the night sky background • Observations are possible only in clear moonless nights (no more than 10% of calendar time) • There are three different lines of research in this field differing in both energy range and instrumentation

  3. All these three lines of research were initiated by a single man! (A.E. Chudakov)

  4. Two outstanding “CH”s P.A. Cherenkov (1904-1990) A.E. Chudakov (1921-2001)

  5. A.E. Chudakov about P.A. Cherenkov: • “Always a modest individual, he was extremely scrupulous not to pretend to be involved in the developing applications just because of his contribution to the effect’s discovery…” A.E. Chudakov, Pavel Alexeevich Cherenkov (Obituary), Physics Today, December 1992

  6. “He even may have been avoided using the Cherenkov technique in his own experiments…” A.E. Chudakov, Pavel Alexeevich Cherenkov (Obituary), Physics Today, December 1992

  7. However, in developiong the air Cherenkov technique Chudakov had some predecessors: • P. Blackett in 1948 first discussed the possibility to detect the Cherenkov radiation of extensive air showers • It was first detected by Galbraith and Jelly in 1952: • W. Galbraith and J. V. Jelley, Nature, 171, 349 (1953). • J. V. Jelley and W. Galbraith, Phil. Mag., 44, 619 (1953).

  8. Chudakov's experimental setup in Pamirs experiments(1953-1957)

  9. Investigations of Extensive Air Showers • In these experiments, carried out in the Pamirs Mountains, the idea of calorimetric measurements of the cascade energy by recording its Cherenkov radiation was realized. Experimental ratio between the cascade energy and the observed number of particles was measured for the first time. The energy spectrum of primary cosmic rays was measured in a wide range.

  10. Modern Cherenkov Air Shower Array (Tunka) Basic Integral Detectors Pulse Shape Detectors Remote Detector

  11. Panorama of the Tunka array (675 m above sea level)

  12. Pulse shape detector of Cherenkov light

  13. QUASAR-370 light receiver

  14. Some results of the Tunka array Shower maximum depth Differential energy spectrum p Fe

  15. CASA-BLANCA: Cherenkov array BLANCA(144 detectors with an average separation of 35-40 m) and CASA air shower array (a lattice of 900 scintillation detectors with a step of 15 m ).

  16. Cherenkov and fluorescence data on cosmic ray composition

  17. A Station of the Yakutsk EAS Array

  18. A plan of the location of detector stations of the Yakutsk EAS Array

  19. The Cherenkov Light Detector of Yakutsk EAS array

  20. Estimation of shower energy E0The calorimetric method • The relation between parameters S300 or S600 and primary particle energy E0 for showers close to the vertical has been determined by the calorimetric method. For the average showers with different S300 or S600 E0 is estimated as the sum separate a components: • E0 = Ei + Eel + Eμ+ Eμi + Eν + Eh • Ei = kis the energy lost by a shower over the observation level. It is estimated by measurements of total Cerenkov light flux, and • k = 2.16104 / (0.37 + 1.1(Xm /1000) in the interval of waves 300-800nm In view of mean atmospheric transmittance • Eel = 2.2106NsNis the energy conveyed below the array level. It is estimated by the attenuation lengthNof the number of charged particlesNsthrough the atmosphere depth • E = Nis the energy of the muon component. It is estimated by the total number of muonsNand average energyon one muon = 10.6109 eV

  21. Ei + E = 0.76E are the energy of muons losses on ionization and the neutrino Eh = 0.06Eiis the energy on nuclear reactions in the atmosphere. Red components are added on the basis of model calculation results. For E0 1019 eV : Ei / E0 74%; Eel / E0 15%; Eμ / E0 3.6%; (Eμi + Eν + Eh) / E0 7.4%

  22. Lateral distribution of EAS Cerenkov light, <30, 1015 <E0 < 31019 eV Q(R) = Q150((62+R)/212)-1((200+R)/(350))1-m, m = (1.150.05) + (0.300.06)log(Q150)

  23. Ratio between shower energy E0 and S300(0º) determined by the calorimetric method EO = (5.66  1.4)1017(S300(0)/10)0.94  0.02

  24. VHE Gamma Ray Astronomy The gamma ray telescope constructed by Chudakov was the first instrument ever specially designed for observations of gamma rays from space. The method was suggested in a paper by G.T. Zatsepin and A.E. Chudakov, «On the methods of searching for local sources of high energy photons», J. Exp. Theor. Phys., vol. 41 (1961), p. 655 (In Russian).

  25. First Gamma-Ray Telescope Katsively, Crimea (1960- 1963)

  26. One Cherenkov light receiver of the first gamma ray telescope

  27. Four mirrors were installed in the season 1960, and all twelve mirrors were used in the remaining seasons 1961, 1962, and 1963.

  28. Crab Nebula is the first detected object and the ‘standard candle’ ofthe VHE gamma ray astronomy

  29. First Gamma-Ray Telescope

  30. The negative result of Chudakov’s experiment was important in one respect: • It was generally believed at that time that the synchrotron radiation in the Crab Nebula is due to electrons of secondary origin (produced by pions generated in proton-proton collisions via  e decay). • If so, one would expect a significant gamma ray flux from decays of neutral pions. • The upper limit obtained by Chudakov was a proof of direct acceleration of electrons in the Crab Nebula (and other sources).

  31. The idea of air fluoresence experiments was also put forward by A.E. Chudakov V.A.Belyaev & A.E. Chudakov, Ionization glow of air and its possible use for air shower detection, Bulletin of USSR Academy of Sciences, Phys. Ser., 1966, vol. 30, no. 10, p. 1700

  32. EUSO: Extreme Universe Space Observatory Accommodation onboard the ISS

  33. Multiple mirror-telescopes

  34. Stereoscopic observations in VHE astronomy

  35. French telescope CAT (Perinei mountains)

  36. TelescopeHegra at Canary Islands CT-3 CT-4

  37. Australian-Japanese telescope Cangaroo II

  38. Stereoscopic CANGAROO III telescope (Project)

  39. CANGAROO III under construction (July 2003)

  40. HESS (High Energy Stereoscopic System) air Cherenkov telescope in Namibia

  41. One HESS reflector

  42. VERITAS (Very Energetic Radiation Imaging Telescope Array System) An array of seven 10m - 12m optical reflectors for gamma-ray astronomy in the GeV - TeV energy range

  43. One Veritas reflector The new array design will be based on the design of the existing 10m gamma-ray telescope of the Whipple Observatory.

  44. PM tube camera of Veritas (499 pixels) The full field of view is 3.5°.

  45. New 17 m MAGIC telescope. Plans…

  46. … and reality MAGIC under construction

  47. MAGIC site

  48. Magic I is operational, Magic II is planned

  49. MAGIC VERITAS HESS CANGAROO-3 Global coverage of most powerful VHE Cherenkov telescopes

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