1 / 31

Current Status of TeV Gamma Ray Astronomy

Current Status of TeV Gamma Ray Astronomy. M. Teshima Max-Planck-Institute for Physics, Munich. Major IACTs in the world. Veritas. MAGIC + MAGIC II. artist view. CANGAROO III. H.E.S.S. I and HESS II. Scien tific Objectives. SNRs. Pulsars and PWN. Micro quasars X-ray binaries. AGNs.

lelia
Download Presentation

Current Status of TeV Gamma Ray Astronomy

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. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Current Status of TeV Gamma Ray Astronomy M. Teshima Max-Planck-Institute for Physics, Munich

  2. Major IACTs in the world Veritas MAGIC + MAGIC II artist view CANGAROO III H.E.S.S. I and HESS II

  3. Scientific Objectives SNRs Pulsars and PWN Micro quasars X-ray binaries AGNs GRBs Origin of cosmic rays Space-time & relativity Dark matter Cosmology

  4. Great success by HESSGalactic place survey HESS Galactic plane Survey Survey in 2-3% Crab unit Astro-ph/0510397 17 sources + Several PWNs Shell type SNRs X-Ray Binary (Microquasars) Un-ID sources

  5. SNRs (9) HESS Vela Junior HESS RXJ1713 Y. Uchiyama, T. Takahashi Texas Symp. 2006 RX J1713 Cas-A

  6. PWN (8) MAGIC Crab Nebula IC emission HESS HESS HESS HESS VelaX Kookaburra MSH 15-52 HESS J1825

  7. Binary System (5) LS 5039 HESS LS I +61 303 VERITAS MAGIC LSI +61303

  8. Un-IDs (Dark Source) Suzaku (Matsumoto et al. 1996)

  9. Galactic Center(1)B.H., SNR, DM? HESS HESS HESS Observation MAGIC Observation MAGIC MAGIC

  10. Probing Cosmic rays in the Galaxy H.E.S.S. Nature Feb. 2006 Spectral index 2.29 ± 0.07 ± 0.20 Implies harder CR spectrum than in our solar system Galactic plane Point sources subtracted

  11. Extragalactic sources(16) New Sources

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

  13. PG 1553(z>0.25unknown) Very Soft energy spectrum the attenuationby pair creation or nature of SSC mechanism MAGIC+HESS  Z < 0.42 D.Mazin and F.Goebel

  14. Distance of PG1553 Test with combined spectrum (Z<0.42)

  15. Mrk501 MAGIC observationTime lag for higher energies? 4min bin 4min bin June 30 July 9

  16. Very fast time variationPKS2155-304 HESS Obs. July 28, 2006 PKS2155(z=0.116) 2 min bins

  17. Number of sources (45+α) SNRs BLLac PWNs BNRs Un-IDs BL-Lac is the champion in the number!!

  18. 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

  19. Idea of CTA • The next generation detector (Observatory) for gamma ray astronomy after HESS and MAGIC • Energy range a few 10GeV-100TeV • A few 10GeV to see sources in the cosmological distance • 100TeV to understand the origin of galactic cosmic rays • ~10 times better sensitivity than HESS, MAGIC • Increase number of sources a factor of ~30 • All sky observatory • North a few 10 GeV – 1TeV • ~10 huge telescopes • South a few 10 GeV – 100TeV • ~10 huge telescopes + ~100 small telescopes • Overlap with GLAST mission • GLAST Mission 2007-2012+ • Budget size ~150MEuro • EU will support <20% of total budget, other >80% must be supported by agencies in each country

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

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

  22. VHE Log(S)-Log(N) plot HESS-I ~33 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

  23. 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

  24. 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

  25. Summary • Now we know about 50 TeV sources in the sky. The physics in TeV gamma ray astronomy is very rich and still there are many open questions. • We definitely need CTA for the development of TeV gamma ray astronomy after HESS, MAGIC, VERITAS and CANGAROO. • ~1000 sources will be observed in 10-20 years by CTA. • All sky observatory is ideal (north & south stations) • Maybe two steps construction • Multi-wavelength and multi-messenger observation are very important to understand the nature of high energy sources • GLAST, IceCube, KM3, Auger, etc..

  26. Thank you

  27. Mrk501 MAGIC observationTime lag for higher energies? 4min bin 4min bin June 30 July 9

  28. Option: Mix of telescope types ~10 central Huge telescopes ~100 Medium + Small Telescopes Picture: Courtesy of W.Hofmann

  29. Etc. • Historical issue • Proposal to ESFRI Astophysics sub-committee • Berlin Meeting on 4-5 on May.2006 • Conveners meeting in Frankfurt on 11.July.2006 • Extended conveners meeting in Munich on 30.Nov.2006 • Working group • Physics Working Group • MC Working Group • Telescope structures & mirrors WG • Camera designs & Electronics WG • Site evaluation, Calibration & Atmosphere WG • Computing WG • Schedule • Write up LOI for CTA (first draft in Munich meeting) • Application to FP7 Design Study (Spring 2007)

  30. MAGIC-I and MAGIC-II Current status Stereo Observation with two 17m telescopes will start in fall 2007

  31. 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

More Related