GLAST and NANTENMolecular clouds as a probe of high energy phenomena

Yasuo Fukui

Nagoya University May 22, 2007 UCLA

NANTEN & NANTEN2

@Atacama, alt.4800m@Las Campanas, alt.2400m

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

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

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

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

12CO(J=1-0) and X-ray in G347.3-0.5

　　　　 Fukui et al. 2003

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

Ｄ

Ａ

B

C

G347.3-0.5 Velocity distribution

VLSR and kinematic distance

Parameters d = 1 kpc d = 6 kpc

Radius (pc) 8.7 52

Age (yr) 1600 >10000

Evolutionary phase Free-exp SedovAmbient density

(cm-3)< 0.01 0.003

Shock velocity (km/s)

5500 3200

Etotal of accelerated particles *(erg)

~ 1048 ~ 1050

* (Eacc/1048)(Mcloud/200)(l/3)-3(d/1)-5 = 1.35 (Enomoto et al.2002)

Physical parameters of G347.3-0.5

XMM and NANTEN

Moriguchi et al. 2005

ASTE CO J=3-2

TeV-gamma & molecular clouds

H.E.S.S. image (Aharonian et al. 2004)

17 pc

SNR G347.3-0.5 (RSJ1713.7-3946)

-Shell-like structure: similar with X-rays- No significant variation of spectrum index across the regions-spatial correlation with surrounding molecular gas Aharonian et al. 2005

SNR G266.2-1.2 (RX J0852-4622, Vela Jr.)

Molecularobservations(Moriguchi et al. 2001)

Age: 680 - several x 1000 yr ?Distance: 200 - 1000 kpc ?

44Ti line Detectionby COMPTEL (Iyudin et al. 1998)

Concentration of Masersnerby SNR

Association with UCHII:W28A2

Hotspots around SNR

2-3 % Crab@E>0.35TeV

Size ~ 0.1-0.2 deg

Spectra: dN/DE ~ E-0.26

H.E.S.S. detection toward W28

[Preliminary]

HESS 1813-178

Molecular clouds associated with counterparts of TeV sources

- HII region W33, SNR 12.82-0.02 (AXJ1813-178)- distance ~ 4 kpc -> consistent with kinematic dist

HLC Survey toward far-infrared excess clouds

32 HLCs are newly detected

Onishi et al. 2005

Per shell of HLC

Yamamoto,et al.

ApJ, in press, 2006

ASTE CO J=3-2

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

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

LVG analysisLarge Velocity Gradient model (e.g. Goldreich & Kwan 1974, Kim et al. 2002)

One-dimensional uniformvelocity gradient.

gradV = 5 km/sX(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 cloudsn(H2) ~ 103-4 cm-3, Tkin ~ 10 - 20 K

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