1. 1/25 Suzaku Observations of HESS sources Hironori Matsumoto (Kyoto Univ.) Hideki Uchiyama (Kyoto Univ.), Aya Bamba, Ryoko Nakamura, Takayasu Anada (ISAS/JAXA), and the Suzaku team

2. 2/25 Outline HESS unID objects: “Dark particle accelerators” Suzaku Observations –HESSJ1614-518 –HESSJ1616-508 –HESSJ1713-381 (CTB37B) –HESSJ1804-216 –HESSJ1825-137 –HESSJ1837-069 Summary

3. 3/25 HESS Galactic Plane Survey First systematic Galactic plane survey with TeV γ- ray (>200GeV) New TeV objects with no obvious counterpart. (Aharonian et al. 2005, 2006) HESSJ1804-216 HESSJ1616-508 HESSJ1614-518 Gal. Cent. HESSJ1713-381 HESSJ1837-069 Dark particle accelerators HESSJ1825-137

4. 4/25 HESSJ1614-518 (l, b)=(331.52, -0.58) HESS TeV γ-ray image (excess map) XIS FOV 50ks Brightest among the new objects. HESSJ1614

5. 5/25 XIS FI (S0+S2+S3): 3-10keV band Extended object TeVγ-ray XIS image Swift XRT also detected (Landi et al. 2006) Obs. 50ks Src A Src B

6. 6/25 XIS spectra NH=1.2(±0.5)e22cm -2 Γ=1.7(±0.3 ） F(2-10keV)=5e-13erg/s/cm 2 NH=1.2(±0.1)e22cm -2 Γ=3.6(±0.2 ） F(2-10keV)=3e-13erg/s/cm 2 Featureless  non-thermal Featureless, but extremely soft Src A Src B Src A spectrum Src B spectrum

7. 7/25 H.E.S.S. src A B=10μG B=1μG B=0.1μG Src A Src B Src A F(1-10TeV)/F(2-10keV)=34 Plausible X-ray counterpart: src A Matsumoto et al. 2008, PASJ, 60. S163 (Suzaku special issue No.2) Difficult to explain both the TeV gamma-ray and X-ray from the electron origin. The origin of srcA is not clarified.

8. 8/25 HESSJ1616-508 HESS TeV image (excess map) (l, b)=(332.391, -0.138) XIS FOV 45ks Provided by S. Funk (MPI) HESSJ1616

9. 9/25 XIS image XIS FI (S0+S2+S3): 3 — 12keV No X-ray counterpart F(2-10keV)<3.1e-13 erg/s/cm 2 TeV image 45ks F(TeV)/F(X)>55

10. 10/25 If we assume electrons… Very weak B (B<1μGauss) HESSJ1616 SED Suzaku upper limit Strong cut-off or realistic? Matsumoto et al. 2007, PASJ, 59, 199 (Suzaku Special Issue No.1)

11. 11/25 PSRJ1617-5055? INTEGRAL 18-60keV PSRJ1617 Landi et al. 2007 XMM-Newton 0.5-10keV PSRJ1617 Why is there no trace in X-ray band? Why is there no clear PWN in the radio (Kaspi et al. 1998) and X-ray bands? SNR RCW103

12. 12/25 HESSJ1713-381 (CTB37B) SNR CTB37B HESSJ1713-381 coincides with the SNR CTB37B Color: TeV White: radio

13. 13/25 Non-thermal hard X-ray Nakamura 2008 in preparation Suzaku 0.3-3.0keV Suzaku 3.0-10.0keV Green: TeV (HESS) Blue: radio White: X-ray (Suzaku) reg1 reg2 Foreground src Reg1: coincides with the TeV peak Reg2: offset hard emission

14. 14/25 Suzaku 3.0-10.0 keV reg1 reg2 Thermal (kT=0.9keV)+PL(Γ=3.0) A point source discovered by Chandra (Aharonian et 1l. 2008) contributes much to the PL component. Hard PL (Γ=1.5) + Leakage from reg1 due to PSF. Roll-off energy > 15keV The hard PL suggests efficient acceleration. F(TeV)/F(X)~0.2  B~8uG assuming IC. Emax > 170 TeV

15. 15/25 HESSJ1804-216 HESS TeV γ-ray image (excess map) Provided by S. Funk (MPI) (l, b)=(8.401, -0.033) XIS FOV 40ks Softest TeV spectrum among the new objects. HESSJ1804

16. 16/25 XIS image XIS FI (S0+S2+S3): 3-10keV src1 src2 src1: point-like src2: extended or multiple TeV image 40ks Swift XRT (Landi et al. 2006) Chandra (Kargaltsev et al. 2007)

17. 17/25 XIS spectra src1 src2 src1: point-like src2: extended src1src2 Γ-0.3±0.51.7±1.2 NH (10 22 cm -2 ) 0.2(<2.2)11±8 F(2-10keV) 10 -13 erg/s/cm 2 2.54.3 See Bamba et al. 2007, PASJ, 59, S209 (Suzaku Special Issue No.1) F(TeV)/F(X) 50 25

18. 18/25 HESS J 1825-137 30arcmin~30pc @4kpc HESS J1825-137 Aharonian et al. 2006 H.E.S.S TeV γ excess map PSR J1826-1334 Distance from Pulsar (deg) Photon Index Γ IC by high-energy electrons from the pulsar? Spin-down luminosity ~ 2.8×10 36 erg s -1 Characteristic age 21.4 kyr (Clifton 1992) D~4kpc softening

19. 19/25 Previous X-ray study (XMM-Newton) PSR J1826-1334 (B1823-13) Photon index ~ 2.3 NH~1.4×10 22 /cm 2 L X ~3×10 33 erg s -1 1arcmin~1pc@4kpc Pulsar PWN XMM-Newton 0.5-10keV H.E.S.S TeV γ excess map Gaensler et al. 2003 Why is the X-ray image much smaller? More extended if observed with high sensitivity?  Suzaku observation!

20. 20/25 Suzaku: Very extended PWN XIS 3F 1-9 keV source 6arcmin ~6pc@4kpc 2006/9 50ksec bgd Suzaku can detect X-rays much more extended than the XMM results. TeV image

21. 21/25 1.2× (CXB+GRXE) CXB+GRXE Galactic Ridge X-ray Emission CXB Background Source Radial profile Unresolved Point sources X-rays are extended at least up to 15 arcmin (~15 pc)

22. 22/25 X-ray spectra Region A Region B Region C Region D Γ=1.78(1.68-1.88) Γ=1.99(1.91-2.08) Γ=2.03 (1.95-2.14) A B C D Reg B-D: no change in photon index.  electrons reach to 15pc before cooled. =pulsar+PWN Synchrotron cooling time~1400yrs.  Velectron~10000 km/s

23. 23/25 HESSJ1837-069 HESS image INTEGRAL/ISGRI (Malizia et al. 2005) 1degx1deg X-rays were detected up to 300 keV by INTEGRAL

24. 24/25 AXJ1838.0-0655 AXJ1837.3-0652 X-ray counterparts are offset from the TeV gamma-ray peak. TeV peak Pulsations of 70.5 ms were recently discovered from AXJ1838 with RXTE (Gotthelf et. al. 2008). Offset pulsar wind nebula Anada et al. in preparation

25. 25/25 Summary X-rayOrigin HESSJ1614-518O? HESSJ1616-508X? HESSJ1713-381OSNR CTB37B Efficient acceleration HESSJ1804-2162? HESSJ1825-137Very extendedPWN HESSJ1837-0692 extendedOffset PWN Can you construct a “Grand Unification Theory (GUT)” of the dark particle accelerators?