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

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

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

4. CTA Great success by HESS Galactic 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. CTA SNRs (9) Cas-A RX J1713 Vela Junior CategoryNameDiscovery Obse rv. SNRCas-AHEGRA SNRVela Junior, RX J0852.0-4622 CANGARO O HESS SNR/Un-ID HESS J1640-465 (G338.3- 0.0; 3EG J1639-4702) HESS SNRHESS 1713-381, G348.7+0.3 ?HESS SNRRX J1713.7-3946, G347.3-0.5 CANGARO O HESS SNR/PWN HESS J1804-216 (G8.7- 0.1 / W30; PSR J1803) HESS SNR HESS J1813-178 (G12.8- 0.02; AX J1813-178) HESS MAGI C SNRHESS J1834-087 (G23.3-0.3 / W41)HESS MAGI C SNR/PWN/Un- ID HESS J1837-069 (G25.5+0.0; AX J1838.0-0655) HESS Y. Uchiyama, T. Takahashi Texas Symp. 2006 HESS RXJ1713

6. CTA PWN (8) CategorySourceDiscovery Observati on PWNCrab NebulaWhipplemany PWNVela X CANGARO O HESS PWNHESS J1418-609 (G313.3+0.1, Rabbit)HESS PWN HESS J1420-607 (PSR J1420-6048, Kookaburra) HESS PWNMSH 15-52, PSRB1509-58 CANGARO O HESS PWNHESS J1616-508 (PSR J1617-5055)HESS PWNHESS J1747-281 (G0.9+0.1)HESS PWNHESS J1825-137 (PSR J1826-1334)HESS Kookaburra MSH 15-52HESS J1825 MAGIC Crab Nebula HESS IC emission HESS VelaX

7. CTA Binary System (5) Categor y SourceDiscovery Observatio n Binary PSR B1259- 63 / SS 2883 HESS XRBIGR J16320-4751 HESS J1632- 478 XRB/S NR IGR J16358-4726 ?; G337.2+0.1 ? HESS J1634- 472 XRBLS 5039HESS XRBLSI+61303MAGICVERITAS LS 5039 HESS LS I +61 303 VERITAS MAGIC LSI +61303

8. CTA Un-IDs (Dark Source) CategorySourceDiscovery Observatio n Un-IDTeV J2032+4130HEGRA Un-IDHESS J1303-631HESS Un-IDHESS J1614-518HESS Un-IDHESS J1702-420HESS Un-IDHESS J1708-410HESS Un-ID 3EG J1744- 3011 ? HESS J1745–303 Suzaku (Matsumoto et al. 1996)

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

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

11. CTA Extragalactic sources(16) Source Redshi ft Sp. Inde x Type s Discovery Observ ation M 87 0.0042.9 FR-IHEGRAHESS Mkn 421 0.0312.2 HBLWhipplemany Mkn 501 0.0342.4 HBLWhipplemany 1ES 2344+514 0.0442.9 HBLWhippleMAGIC Mkn 180 0.0453.3 HBLMAGIC 1ES 1959+650 0.0472.4 HBL7TAmany PKS 0548- 322 0.069 HBLHESS PKS 2005- 489 0.0714.0 HBLHESS PKS 2155- 304 0.1163.3 HBLDurhamHESS 1ES 1426+428 0.1293.3 HBLWhippleHEGRA 1ES 0229+200 0.139 HBLHESS H 2356-309 0.1653.1 HBLHESS 1ES 1218+304 0.1823.0 HBLMAGIC VERITA S 1ES 1101- 232 0.1862.9 HBLHESS 1ES 0347- 121 0.188 HBLHESS PG 1553 0.3?4.0 HBL HESS/MAG IC New Sources

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

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

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

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

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

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

18. CTA From HESS & MAGIC to CTA About 30 sources are now identified as VHE gamma sources. GLAST will see ~3000 of GeV sources around 2010 GLAST will see ~3000 of GeV sources around 2010 Our target in VHE Energy 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 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 Extend HESS galactic plane survey to entire sky

19. CTA 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 A few 10GeV to see sources in the cosmological distance 100TeV to understand the origin of galactic cosmic rays 100TeV to understand the origin of galactic cosmic rays ~10 times better sensitivity than HESS, MAGIC Increase number of sources a factor of ~30 Increase number of sources a factor of ~30 All sky observatory North a few 10 GeV – 1TeV North a few 10 GeV – 1TeV ~10 huge telescopes South a few 10 GeV – 100TeV South a few 10 GeV – 100TeV ~10 huge telescopes + ~100 small telescopes Overlap with GLAST mission GLAST Mission 2007-2012+ GLAST Mission 2007-2012+ Budget size ~150MEuro EU will support 80% must be supported by agencies in each country EU will support 80% must be supported by agencies in each country

20. CTA By W.Hofmann ∝ N tel ∝ Area 50hrs Background LimitedSignal Limited

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

22. CTA 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 HESS-II MAGIC-II CTA

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

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

25. CTASummary 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 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.. GLAST, IceCube, KM3, Auger, etc..

26. Thank you

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

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

29. CTA Mkn501 variability June 30 July 9 June 30 July 9

30. CTA 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) Increase telescope density (gain x 4) ~100m spacing  ~50m spacing Many sampling points  reduce shower fluctuation effect Increase telescope diameter (gain x 3) Increase telescope diameter (gain x 3) 12m-17m φ  20-30m φ Increase Q.E. of photo-detectors (gain x 3) Increase Q.E. of photo-detectors (gain x 3) Q.E. 20%  60-80% Total gain 30~40 in photo collection efficiency could be realistic 10GeV threshold energy with reasonable sensitivity 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

31. CTA Strategy in High energy up 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 Emax ~10TeV  Emax ~100TeV ~10 5 m 2 (300m x 300m)  ~10 7 m 2 (3km x 3km) ~10 5 m 2 (300m x 300m)  ~10 7 m 2 (3km x 3km)

32. CTAEtc. 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)

33. CTA MAGIC Highlights of the First Year Crab Nebular SZA & LZA Mrk421 (0.031)Galactic CenterHESS J1813HESS J1834 13 CO cloud 1ES2344 (z=0.044)1ES1218 (z=0.18) New Source 1ES1959 (0.047)PG 1553 (Z>0.25) New source LSI+61 303 Micro-Quasar New Source Mrk180 (0.045) New source Mrk501 (z=0.034)

34. CTA Extragalactic sources Spectral Indices of new sources range 3~4 PKS2005PG1553 New Sources

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

36. CTA The SSC framework Fossati et al. 1998 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 20051553 2344