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CTA The next generation ultimate gamma ray observatory

CTA The next generation ultimate gamma ray observatory. M. Teshima Max-Planck-Institute for Physics. Physics Objectives. AGNs. Pulsars. Cosmological g -Ray Horizon. Origin of Cosmic Rays. Quantum Gravity. SNRs. Cold Dark Matter. GRBs. Galactic Sources. HESS Galactic plane Survey

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CTA The next generation ultimate gamma ray observatory

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  1. CTAThe next generation ultimate gamma ray observatory M. Teshima Max-Planck-Institute for Physics

  2. Physics Objectives AGNs Pulsars Cosmological g-Ray Horizon Origin of Cosmic Rays Quantum Gravity SNRs Cold Dark Matter GRBs

  3. Galactic Sources HESS Galactic plane Survey Survey in 2-3% Crab unit Astro-ph/0510397 17 sources + Several PWNs Shell type SNRs X-Ray Binary Un-ID sources

  4. Extragalactic sources PKS2005 PG1553 Spectral Indices of new sources range 3~4 New Sources

  5. PG 1553(z>0.25) Very Soft energy spectrum the attenuationby pair creation X-Ray Intensity =6.5μJy Mrk421 9.9 μJy Mrk501 9.4 μJy

  6. Absorption of gamma rays in the universe Pair Creation; γ＋γ  e+ + e-

  7. The SSC framework Higher Z  Higher source luminosity  Lower IC peak  softer spectrum X-ray intensity at 1keV PG 1553 6.5 μJy z~0.3 Mrk421 9.9 μJy z=0.03 Mrk501 9.4 μJy z=0.03 PG1553’s source luminosity ~100 x Mrk 2005 1553 2344 Fossati et al. 1998

  8. From HESS & MAGIC to CTA • About 30 sources are now identified as VHE gamma sources. • GLAST will see ~3000 of GeV sources around 2010 • Our target in VHE Energy • ~100 VHE sources in 2010 by HESS-II and MAGIC-II • ~1000 VHE sources in 2020 by CTA • CTA Sensitivity must be 10 times better than HESS, and MAGIC • Importance of all sky observatory  full sky survey  relatively large FOV is favored • Extend HESS galactic plane survey to entire sky

  9. By W.Hofmann ∝Ntel 50hrs ∝Area Background Limited Signal Limited

  10. Kifune’s Plot (my optimistic expectation) ~1000 sources by CTA ~3000 sources by GLAST, AGILE GLAST AGILE

  11. VHE Log(S)-Log(N) plot HESS-I ~30 sources MAGIC-I ~20 sources Log(N) ~ -1.0 Log(S) ??? HESS-II ~60 sources MAGIC-II ~40 sources CTA South ~300 sources CTA North ~200 sources CTA HESS-II MAGIC-II

  12. Option: Mix of telescope types ~10 central huge telescopes ~100 small telescopes outside Picture: Courtesy of W.Hofmann

  13. Strategy in Low Energy~10GeV Eth • Image quality is limited by the number of photons and air shower fluctuations • Increase photo-collection efficiency • Increase telescope density (gain x 4) • ~100m spacing  ~50m spacing • Many sampling points  reduce shower fluctuation effect • Increase telescope diameter (gain x 3) • 12m-17m φ 20-30m φ • Increase Q.E. of photo-detectors (gain x 3) • Q.E. 20%  60-80% • Timing between telescopes may help  S. Biller • Total gain 30~40 in photo collection efficiency could be realistic • 10GeV threshold energy with reasonable sensitivity • Photon sampling rate: HESS, MAGIC ~ 1/1000 • Photon sampling rate in CTA should be ~1/30 (10% mirror area, 50% Q.E.) • Significant improvement in data quality  intensive M.C. is necessary

  14. Strategy in High energyup to 100TeV • Extension of the sensitivity up to 100TeV to study galactic cosmic ray source  CTA south only • Current IACTs’ sensitivity is just limited by the number of gamma events • Emax ~10TeV  Emax ~100TeV • ~105 m2 (300m x 300m) ~107 m2 (3km x 3km)

  15. Multi-Messengers observationAll sky observatory (N,S stations) Gamma Rays Gamma Ray & X-Ray Satellites Neutrinos CTA North CTA South IceCube: 2010 Completion of the construction

  16. HESS-II and MAGIC-II can be good R&Ds for CTA March 2006 HESS-II 28m diameter telescope Lower threshold energy In 2008 MAGIC-II 2x17m, High Q.E. detectors Lower threshold energy High Precision In 2007

  17. Summary • We definitely need CTA for the development of VHE astrophysics after HESS-II and MAGIC-II • 500~1000 sources will be observed in 10-20 years operation  10-20 hrs/source (time limited) • CTA could be an ultimate ground based gamma ray observatory and we should consider north & south stations (All sky observatory) • The number of galactic sources may be limited • Multi-wavelength and multi-messenger observation are very important to understand the nature of high energy sources • New advanced photon detector development will have a strong impact in the design of CTA (HPD, SiPM)

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