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Current status and future plans of TeV gamma-ray observations

Current status and future plans of TeV gamma-ray observations. Hidetoshi Kubo (Kyoto University). Outline. TeV gamma-ray telescopes Observations Results Galactic HESS plane survey G.C., Diffuse emission PWN, SNR, etc. Extragalactic sources AGN, Starburst galaxy Future plans Summary.

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Current status and future plans of TeV gamma-ray observations

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  1. Current status and future plans of TeV gamma-ray observations Hidetoshi Kubo (Kyoto University)

  2. Outline • TeV gamma-ray telescopes • Observations Results • Galactic • HESS plane survey • G.C., Diffuse emission • PWN, SNR, etc. • Extragalactic sources • AGN, Starburst galaxy • Future plans • Summary

  3. TeV gamma-ray observation • Cherenkov shower pool • Better angular resolution=0.20.07/g • Better energy resolutionE/E=30%15% • E>100GeV at present • Higher E threshold at larger zenith angle • 1%Crab for 25hrs(HESS) • FOV＜5, ＜3 (FWHM) ~300m Altitude 10～20km +Water Cherenkov telescope, Air Shower Array

  4. CANGAROO-III 114 80cm FRP mirrors T2 T2 T4 T3 T1 427ch (4 FOV)

  5. TeV gamma-ray telescopes TIBET MILAGRO MAGIC STACEE VERITAS TACTIC CANGAROO HESS TIBET ARGO-YBJ MILAGRO STACEE TACTIC PACT GRAPES R.Ong (2005)

  6. RXJ 1713 MSH 15-52 RXJ 0852 GC Vela X PSR B1259 HESS J1303 HESS Galactic Plane Survey in 2004 Survey Region • 30°in longitude, 3° in latitude • 230hrs(95 hrs scanning + follow-up observations) • E > 200GeV • Flux > 2%Crab Aharonian et al. (2005)

  7. Detections with CANGAROOBefore the HESS survey Gal. Centre 30° 0° 330° 359° 330° RX J1713.7-3946

  8. HESS Survey: New sources Gal. Centre HESS J1804-216 HESS J1825-137 HESS J1837-069 HESS J1834-087 HESS J1813-178 G0.9+0.1 30° 0° LS 5039 330° 359° 330° Sources > 6 sigma (10 new, 12 total) HESS J1614-518 HESS J1640-485 RX J1713.7-3946 HESS J1616-508 Aharonian et al. (2005)

  9. HESS Survey: New Sources Gal. Centre HESS J1804-216 HESS J1825-137 HESS J1837-069 HESS J1834-087 HESS J1813-178 G0.9+0.1 30° 0° LS 5039 HESS J1713-381 HESS J1702-420 HESS 1632-478 HESS J1745-303 HESS J1634-472 HESS J1708-410 330° 359° Sources > 6 sigma (10new, 12 total) Sources > 4 sigma (6 new) HESS J1614-518 HESS J1640-465 RX J1713.7-3946 HESS J1616-508 Aharonian et al. (2005)

  10. HESS GP Source Associations ◎ >6 s ○ >4 s ◎ PWN ○ XRB ○ XRB/SNR ◎ SNR/UID ○ ○ ○ SNR ◎ SNR ◎ SNR/BH ○ UID ◎ PWN ◎ SNR/PWN ◎ SNR PWN/UID ◎ ◎ SNR UID ◎ J1826-148 LS5039 XRB ◎ Aharonian et al. (2005)

  11. Pulsar Nebula AGN Other, UNID SNR The VHE Sky - 1995 Mrk421 Mrk501 Crab R.A.Ong Aug 2005

  12. Pulsar Nebula AGN Other, UNID SNR The VHE Sky - 2003 12 sources Mrk421 H1426 M87 Mrk501 1ES1959 RXJ 1713 Cas A GC TeV 2032 Crab 1ES 2344 PKS 2155 R.A.Ong Aug 2005

  13. Pulsar Nebula AGN Other, UNID SNR The VHE Sky - 2005 33 sources + 8-15 add. sources in galactic plane. 1ES 1218 Mrk421 H1426 M87 Mrk501 PSR B1259 1ES 1101 1ES1959 SNR G0.9 RXJ 1713 RXJ 0852 Cas A LS 5039 GC Vela X TeV 2032 Crab 1ES 2344 HessJ1303 Cygnus Diffuse MSH 15-52 PKS 2155 H2356 PKS 2005 R.A.Ong Aug 2005

  14. TeV gamma-ray sources Based on R.A.Ong ICRC2005

  15. Galactic Center Yusef-Zadeh & Morris(1987) VLA@5GHz SGR A Contour: Radio HESS (E>125GeV) CANGAROO (E>300GeV) EGRET(E>500MeV) r<0.2  Consistent with SGR A* to 6’’±10”stat±20”sys Point like core + slightly extended tail Tsuchiya et al. (2004) Mayer-Hasselwander et al. (1998) Aharonian et al.(2004),Rolland et al.(2005)

  16. Galactic Center Unbroken power-law. Hard spectrum G = 2.2 (HESS). No evidence for variability π0→2γ HESS CANGAROO-III(stereo) under analysis

  17. Galactic Center Region gamma rays HESS CS CS gamma rays (subtracted) CS Hinton et al.(2005) G=2.29±0.07±0.20 Harder than Diffuse model

  18. Galactic Diffuse emission E-2.51±0.05 Milagro(2000～2002) Sinnis et al.(2005) Milagro EGRET longitude latitude R1 40-100°±5° R2140-200°±5° x1/100 4.5 s -1.3 s CANGAROO-IIUL l=+13,b=0, l=-19.5,b=-3,0,+3 Ohishi et al.(2005)

  19. Cygnus region Milagro (2000～2005) +100 6.7s Excess >5° (1.55Crab for E>2TeV) from Cygnus region +80 +60 HEGRA unID TeV 2032+4130 +40 +20 PSF Smith et al.(2005) Contour: 1420MHz

  20. Crab ーstandard candle in VHEー PWN(1/5) UL for pulse Continuum HESS (440GeV<E<10TeV) Consistent with point source (PSFσ～0.14°) Error 5”(stat)±20”(sys) G=2.6 Masterson et al.(2005) Gravity of the X-ray emission E>100GeV Weisskopf et al. (2000) Aharonian et al.(2004)

  21. SNR MSH-52(PSR B1509-58) PWN(2/5) HESS Chandra Gray:Radio Contours:ROSAT PSF Contours: X-ray(ROSAT) Major axis 6.4’±0.7’ Minor 2.3’±0.5’ Photon index 2.27 ± 0.03 ± 0.20 Dust=2.3eV/cm3 B～17mG Aharonian et al.(2005)

  22. Vela PWN(3/5) HESS No emission from Vela pulsar position, but Extented hard spectrum G ≈1.9 or G ≈1.5  cutoff extends to50 TeV Khelifi et al.(2005) HESS Vela pulsar CANGAROO-II also detected ROSAT contours Preliminary Enomoto et al.(2005)

  23. HESS J1825-137(4/5) TeV Offset by 11’ south to PSR B1823-13(101ms) in PWN G18.0-0.7 17%Crab(E>200GeV) Aharonian et al.(2005)

  24. PWN in SNR G0.9+0.1(5/5) SNR G0.9+0.1 HESS ・Consistent with point sourceat core, not SN shell ・2% Crab flux(E>200GeV) HESS Aharonian et al.(2005) G=2.40 ±0.11±0.20 G.C. GLAST 1yr Radio (90 cm) Radio Chandra Gaensler et al.(2001) Hard spectrum Point Src (No pulsed emission) Newton Porquet al.(2003) Softening of spectrum with increasing distance from the center 6mG

  25. RXJ 1713.7-3946 SNR(1/4) From the NW rim, non-thermal X-ray emission detected with ASCA (Koyama et al.1997) TeV -g detection E>1TeV CANGAROO-I in 1998 E>400GeV CANGAROO-II in 2000+1 Enomoto et al.(2002) Berge et al.(2005) Shellstructure clearly resolved. Morphology does not change with energy. HESS Spectral index: little variation across SNR

  26. RXJ 0852.0-4622 “Vela Jr.” SNR(2/4) TeV flux ～ Crab CANGAROO-II HESS Aharonian et al.(2005) 4850MHz ASCA Katagiri et al.(2005) Contour: ROSAT

  27. SNR RXJ 0852.0-4622 “Vela Junior” p0 decay? Brems.? IC? p0 decay GLAST 1yr Synchrotron Bremsstrahlung IC Katagiri et al.(2005)

  28. Cas A SNR(3/4) HEGRA Center of TeV g excess GLAST 1yr Chandra image p0 decay? IC+Bremsstrahlung? Aharonian et al.(2001)

  29. SN1006 SNR(4/4) CANGAROO-III 2s U.L. 10-12 10-13 Earlier detection by CANGAROO-I from NE rim. & HEGRA CT1. Upper limit HESS & CANGAROO-III ASCA Tanimori et al.(2005)  SN1006 not detected at previous levels.

  30. PSR B1259-63/SS2883 PSR B1259-63 (P=48ms) around Be star SS2883 in a highly eccentric 3.4yr orbit 331 R* 1.4GHz periastron HESS Aharonian et al. (2005)

  31. PSR B1259-63/SS2883 electron origin? Hadronic origin? GLAST? Aharonian et al. (2005) Kawachi et al.(2004)

  32. Microquasar LS 5039 first detection of TeV emission from a microquasar • compact 4 (?) Mobject in eccentric 4 day orbit around 20-30 Mstar • closest approach ~1012cm or ~2 stellar radii HESS European VLBI@5GHz Jets RA (mas) Paredes et al. (2002) Aharonian et al.(2005)

  33. Microquasar LS 5039 1998 RXTE G=2.12 ± 0.15 2003 XMM Flux (E>250GeV) (5.1±0.8stat±1.3sys)x10-12 ph cm-2s-1 L～1033 erg/s at 3kpc

  34. unID TEV J2032+4130 HEGRA observations 1999～2002 3EGJ2033+4118 Hard spectrum Γ=1.9±0.1’stat±0.3’sys Extented with radius 6.2’(±1.2’stat±0.9’sys) Flux (6.2±1.5stat±1.3sys)x10-13 ph cm-2s-1TeV-1@1TeV Higher angular resolution of GLAST can resolve it Aharonian et al. (2005)

  35. TeV g –ray detected AGNs 501 421 HBL 2155 1101 1426 LBL 2344 2356 2005 Costamante & Ghisellini (2002) Total :11 sources R.Ong (2005)

  36. Extragalactic Background Light Reference shape TeV photon + EBL →e+ + e- More transparent than previously thought TeV GLAST If we assume G>1.5 (electron index>2) for intrinsic spectrum HESS limits GLAST Aharonian et al.(2005)

  37. Mrk 421 & Mrk 501 Wide range:300GeV – 30TeV Mrk 501 Big Flare in Jul 2005 Rapid variation GLAST Light Curve: 2 min time bins. Mazin et al.(2005) MAGIC 4Crab STACEE Simulataneous obs. with GLAST is needed Carson et al.(2005) Mirzoyan et al.(2005)

  38. Radio galaxy M87(16Mpc) HESS (2003+2004) 5.8 s Beilicke et al. (2005) HEGRA Georganopoulos et al.(2005)

  39. Starburst galaxy NGC253 • Nearby(2.5Mpc) spiral galaxy • Radio Halo extending to ~9kpc CANGAROO-II Detected with CANGAROO-II in 2000 and 2001 with 11s (E>0.5TeV) First TeV gamma-ray detection from a normal spiral galaxy other than our own Multi-band spectrum Itoh et al. A&AL 2002 CANGAROO DSS2 GLAST 1yr Crab(65%) E-1.5e-√E/(0.25±0.01)

  40. Future plans of TeV g-ray observations Project Site Current Plan From E> VERITAS USA 12m x 1 12m x 4 200650GeV CANGAROO Australia 10m x 3 10m x 4 100GeV HAGAR India(4.2km) 0.9m x 1 0.9m x 7 2006 60GeV MACE India(4.2km) 21m x 2 15GeV MAGIC Canary is. 17m x 1 17m x 2 2007 20GeV HESS Namibia 12m x 4 +28m x 1 2008 20GeV Ashra Hawaii HAWC 300mx300m pond Lower Energy Threshold at higher altitude

  41. Future plans of TeV g-ray observations

  42. Cherenkov telescope network ・Continuous monitoring of time variable objects such as blazars ・Simultaneous observations with GLAST HAGAR, Mace ＋

  43. Summary • 33 sources detected in TeV g-ray region, including newcomers (Pulsar Binary, Microquasar, Starburst Galaxy, unID). Candidates for GLAST detection. • Improved resolution of TeV(<0.1/g) + GLAST enable us to investigate detail morphology of SNRs, PWNs, etc. • TeV + GLAST reveal electron or proton origin of g-ray emission in SNR etc., the intrinsic spectrum of blazars, and the EBL spectrum. • Simultaneous monitoring with Cherenkov telescope network and GLAST for variable sources. • New telescopes are under construction in order to lower the energy threshold to <100GeV, overlapped with GLAST region.

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