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GLAST and NANTEN Molecular clouds as a probe of high energy phenomena

GLAST and NANTEN Molecular clouds as a probe of high energy phenomena. Yasuo Fukui Nagoya University. May 22, 2007 UCLA. NANTEN & NANTEN2. @Las Campanas, alt.2400m. @Atacama, alt.4800m. Galactic Plane Survey. 12 CO(J=1-0), Grid size ~ 4  (|b|<5  ), 8  (5  <|b|<10  )

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GLAST and NANTEN Molecular clouds as a probe of high energy phenomena

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  1. GLAST and NANTEN • Molecular clouds as a probe of • high energy phenomena Yasuo Fukui Nagoya University May 22, 2007 UCLA

  2. NANTEN & NANTEN2 @Las Campanas, alt.2400m @Atacama, alt.4800m

  3. Galactic Plane Survey • 12CO(J=1-0), Grid size ~ 4 (|b|<5), 8 (5<|b|<10) • Integ. time (typ) ~5sec/point, 1,100,000 observed points

  4. POINTS • Cosmic ray protons: identify the sites of acceleration by establishing the hadoronic origin of gamma rays • X factor = H2/W(CO) is determined • GLAST offers a useful tool with NANTEN CO dataset

  5. Molecular clouds toward GC TeV ridge - NANTEN 13CO(J=1-0), velocity channel maps (increment: 10km/s)

  6. Galactic Center Molecular Loop2Fukui,Y. et al. Science, 314, 106, 2006

  7. 12CO(J=1-0) and X-ray in G347.3-0.5 Ｄ Ａ B C molecular hole surrounding boundary of the SNR CO peaks⇔X-ray peaks show good spatial correlation (northwestern bright rim) 　　　　↓ indicates interaction of the SNR with molecular clouds. -11 km/s < VLSR < -3 km/s Fukui et al. 2003

  8. G347.3-0.5 Velocity distribution

  9. VLSR and kinematic distance

  10. Physical parameters of G347.3-0.5 * (Eacc/1048)(Mcloud/200)(l/3)-3(d/1)-5 = 1.35 (Enomoto et al.2002)

  11. XMM and NANTEN Moriguchi et al. 2005

  12. ASTE CO J=3-2

  13. TeV-gamma & molecular clouds 17 pc H.E.S.S. image (Aharonian et al. 2004)

  14. Shell-like structure: similar with X-rays • - No significant variation of spectrum index • across the regions • spatial correlation with surrounding molecular • gas SNR G347.3-0.5 (RSJ1713.7-3946) Aharonian et al. 2005

  15. SNR G266.2-1.2 (RX J0852-4622, Vela Jr.) Age: 680 - several x 1000 yr ? Distance: 200 - 1000 kpc ? 44Ti line Detection by COMPTEL (Iyudin et al. 1998) Molecular observations (Moriguchi et al. 2001)

  16. H.E.S.S. detection toward W28 Hotspots around SNR 2-3 % Crab@E>0.35TeV Size ~ 0.1-0.2 deg [Preliminary] Spectra: dN/DE ~ E-0.26 Concentration of Masers nerby SNR Association with UCHII: W28A2

  17. HESS 1813-178 - HII region W33, SNR 12.82-0.02 (AXJ1813-178) - distance ~ 4 kpc -> consistent with kinematic dist Molecular clouds associated with counterparts of TeV sources

  18. HLC Survey toward far-infrared excess clouds 32 HLCs are newly detected Onishi et al. 2005

  19. Per shell of HLC Yamamoto,et al. ApJ, in press, 2006

  20. ASTE CO J=3-2

  21. 12CO(J=3-2) wing-like profiles

  22. 12CO(J=1-0) wing-like profiles

  23. Large Velocity Gradient model (e.g. Goldreich & Kwan 1974, Kim et al. 2002) LVG analysis One-dimensional uniform velocity gradient. gradV = 5 km/s X(CO) = 10-4.5 R(3-2)/(1-0) ~ 0.7-0.8 ↓ n(H2) ~ 103-4 cm-3 Tkin ~ 30 - 50 K For typical dark clouds n(H2) ~ 103-4 cm-3, Tkin ~ 10 - 20 K

  24. POINTS • Cosmic ray protons: identify the sites of acceleration by establishing the hadoronic origin of gamma rays • X factor = H2/W(CO) is determined • GLAST offers a useful tool with NANTEN CO dataset

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