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TeVγ 線天文学の現状と将来

TeVγ 線天文学の現状と将来. 森　正樹 東京大学宇宙線研究所. 「高エネルギー宇宙物理学の現状と将来」 2000 年 9 月 29-30 日 大阪大学. Cherenkov telescope. Cherenkov light from gamma-ray showers Lateral distribution & Timing distribution. Konopelko, TMACD-V, 1999. Imaging Cherenkov technique. γ. p.

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TeVγ 線天文学の現状と将来

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  1. TeVγ線天文学の現状と将来 森　正樹 東京大学宇宙線研究所 「高エネルギー宇宙物理学の現状と将来」 2000年9月29-30日 大阪大学

  2. Cherenkov telescope Cherenkov light from gamma-ray showers Lateral distribution & Timing distribution Konopelko, TMACD-V, 1999

  3. Imaging Cherenkov technique γ p

  4. Satellite vs Ground-based gamma-ray telescope

  5. Cherenkov telescopes in the world (終了)

  6. TeV gamma-ray source catalog T.C. Weekes, Heidelberg WS, 2000

  7. TeV gamma-ray sky

  8. GeV gamma-ray sky Third EGRET catalog E > 100 MeV

  9. Crab nebula • Unpulsed spectrum Aharonian & Atoyan, astro-ph/9803091 / Heidelberg WS, 2000 synchrotron IC

  10. Crab pulsar spectrum: where is the cutoff? Musquere, 26th ICRC, 1999

  11. Supernova remnant: SN1006 T. Naito

  12. SNR: SN1006 - interpretation Naito et al. Astron. Nach. 320, 1999 • Synch+IC • Only IC? • No pro-tons?

  13. Supernova remnant: Cas A Goret et al. 26th ICRC OG2.2.18, 1999 ●HEGRA2000

  14. Supernova remnant: RXJ1713 Muraishi et al., A&Ap 354, 2000 RXJ1713.7-3946 “SN1006 Jr.” CANGAROO Tomida, Ph.D., 1999

  15. AGN: Mrk 421 (April 1998) Maraschi et al. ApJL 526, 1999 Whipple • Rapid variability:Faster at TeV? BeppoSAX BeppoSAX

  16. AGN: Mrk 421 spectrum Takahashi et al. astro-ph/0008505 • Synchrotron+ inverse Comptonmodel synchrotron inverse compton One-zone SSC model δ=14, B=0.14G

  17. AGN: TeV gamma-ray absorption by IR background Mean free path for e+e- pair production IR Background Protheroe et al. astro-ph/0005349

  18. AGN: Mrk 501 spectrum Crisis?↓ Protheroe et al. astro-ph/0005349 Aharonian et al. A&Ap 349, 1999

  19. Next generation projects

  20. H.E.S.S. (High Energy Stereoscopic System) 23o16'18'' S 16o30'00'' E 1800 m a.s.l.

  21. H.E.S.S. telescope • 16 (4 init.) telescopes(120m spacing) • Davies-Cotton design, F/0.8 (f=15m), 108m2 mirror area(382 x 60cm) • Camera:960 x 29mm (0.16°) PMTs, 5° FOV, 600kg • Readout: 1GHz FADC • Total 52 ton each

  22. VERITAS (Very Energetic Radiation Imaging Telescope Array System) Mt. Hopkins, AZ (Montosa canyon or north site) 23o N 111o W >2000 m a.s.l.

  23. VERITAS telescope • 7 telescopes (80m spacing) • Reflector: Davies-Cotton design, D=10m (78.6m2), f=12m, 244x 60cm hexagonal mirrors (glass) • Camera: 499x 1” PMTs (0.15o spacing), 3.5o FOV • Readout: 500MHz FADC? (This is the present 10m telescope: new design not available!)

  24. MAGIC (MajorAtmosphericGamma-rayImagingCherenkovTelescope) La Palma, Canary Island 28.75o N 17.89o W 2200 m a.s.l.

  25. MAGIC telescope • Reflector: parabolic, D=17m (234m2), f=17m, 976x (50x50cm2) Al mirrors • Camera: [classical] 397x 1” PMTs (0.10o )+ 126x 1.5” PMTs (0.20o), 3.5o FOV, ~100kg [standard] HPDs (center) + PMTs • First Light in Summer 2001 (June 21, 2001)

  26. CANGAROO-III 31o06' S 136o47' E 160 m a.s.l. Woomera, South Australia

  27. CANGAROO-III telescope • 4 telescopes (100m spacing) • Parabola reflector consisting of 114 mirrors of 80cmφ(57m2), f=8m, F/0.8 • Camera: 4FOV, 427x 3/4”PMTs (0.16, Hamamatsu R3478UV, TTS 0.36ns) • Readout: q-ADC & TDC

  28. Sensitivity of Cherenkov telescopes Major backgrounds: p: CR proton e: CR electron : CR muon NSB: night sky background VERITAS, ICRC1999

  29. Expected sensitivity

  30. Monitoring the gamma-ray sky ⇒？ ⇒？ ⇒？

  31. Future trends • Lowering energy threshold (→5 GeV)Larger light collectorHigher altitude • Increasing FOV (→1 sr)“All-sky” TeV gamma-ray monitor

  32. High altitude Cherenkov telescope • High altitude→higher photon density→lower energy→high statistics/overlapping to satellites

  33. Cherenkov light density at high altitude γ p Aharonian et al. astro-ph/0006163

  34. Sensitivity of 4×50m2 telescope array at 5km a.s.l. (e.g. Atacama) Aharonian et al. astro-ph/0006163

  35. All-sky TeV gamma-ray monitor • 5 mφ, 1 sr telescope, 1 TeV threshold・ CR rate (>1 TeV):8･10-6cm-2s-1 × 3・108cm2 = 3 kHz・ Muons (>1 GeV):7・10-3cm-1s-1 × 2・105cm2 = 1.4 kHz・ High threshold to reduce N.S.B.・ 0.1o resolution camera (many channels…)・ Stereo if necessary・ Good monitor for GRBs • Not far away from the present technology! Kifune and Takahashi, TMACD-IV, 1997

  36. All-sky monitor optics • EUSO/OWL type large FOV optics ↑ □ movable camera? ↓ EUSO proposal, 2000

  37. Science to come • Plerions (pulsar nebula)Inverse Compton? ←synchrotron origin? • PulsarsCutoff in pulse component? ← polar cap/outer gap • SNRsπ0 contribution? ← cosmic ray origin • AGNsGamma-ray source: e± or p?Intergalactic IR ← cosmology • EGRET unIDs, Neutralinos, GRBs, QG,Diffuse gamma,…, and more?

  38. Gamma-rays and cosmic-rays T. Kifune, 2000

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