IC443(09.09-)&Kes78 (09.05-) Ping, Zhou

Part1: IC443 CO observation, map and spectrum Compare with other wavelength Part2: Kes78 12CO(1-0), 13CO(1-0) Search for interaction evidence between kes78 and MCs

Red: IR Green: optical Blue: X-ray  G IC443, 3C157 (Green’s catalogue)  Right Ascension:  Declination:  Size (/arcmin): 45  Type: C  Flux density at 1 GHz (/Jy): 160  Spectral Index: 0.36  Radio: Limb-brightened to NE, with faint extension to the E.  Optical: Brightest to the NE, with faint filaments outside the NE boundary.  X-ray: Shell, brightest to the NE, plus compact source with nebula.  Point sources: X-ray source and nebula in S.  Distance: Mean optical velocity suggests 0.7– 1.5 kpc, association with S249 gives 1.5–2 kpc.

12CO(3-2,2-1) KOSMA provided by M. Martin, observed by Koo CO data 12,13CO(1-0) PMOD provided by ZhiYu, Zhang

 Left: beam size 9’ KOSMA: beam size~2’

 Red;12co2-1  Green:24um  Blue: optical

 Double Peak, hign 12co 3-2/1-0 I?

P-V image of Clump B(left) & I(right)

 Strongly shocked clumps: B,C,G  A tail at 0-10km/s

 green:optical blue:X-ray red:12co

1. map High quality 12CO 2-1,3-2 map of IC ratio Extremely High 12CO 3-2/1-0 ratio in the shocked clumps 3.tail 1) in the west, Vlsr= 5km/s, match along with opitical emission 2) show no line broadening. Probably is quiescent gas, which lies between IC443 and us.

1. Physical analysis with IC443, such as MCs mass, shock velocity…. 2. Detailed 12CO 3-2/2-1, 2-1/1-0 ratio 3. Use LVG(large velocity gradient) Model to find the temperature, column density of each clump 4. Other interesting things: find out why there is double-peak In clump I, 1665/1667 MHz OH maser at clump B….

 G32.8−0.1 Kes 78  Right Ascension:  Declination: −  Size (/arcmin): 17  Type: S?  Flux density at 1 GHz (/Jy): 11?  Spectral Index: 0.2?  Notes: Part has been called G33.1−0.1.  Radio: Elongated shell?

Multi-wavelength MC spectrum MC shape

green. 24Um Blue: x-ray contour,radio

red.radio green&blue:xmm

Left---Red contour :radio grey:12co Right---white:12co1-0,red:13co1-0

blue:12co1-0 contour:radio cross:maser point Maser velocit: 86km/s

Image:contour:radio grey:12co1-0 Line: white:12co1-0 green:13co1-0

contour:radio(VGPS) grey:13co1-0 (FCRAO) contour:radio red:13co1-0 green:24um blue:x-ray

Left---Red contour :radio grey:12co Right---white:12co1-0,red:13co1-0

Left---Red contour :radio grey:12co Right---white:12co1-0,red:13co1-0

Left---Red contour :radio grey:12co Right---white:12co1-0,red:13co1-0

Left---Red contour :radio grey:12co Right---white:12co1-0,red:13co1-0

Left---Red contour :radio grey:12co Right---white:12co1-0,red:13co1-0

The shell ^_^: shape:match along with radio, x-ray, partly match along with 24um IR ^_^:show some broaden in the 12co line, but with no confident evidence. The East ^_^:shape: 13co1-0 along with radio >_<:Large MC, too conplicated to anlayse line broaden >_<:No 12co peak in the maser point at 86km/s

blue:12co1-0 contour:radio cross:maser point

green. 24Um red:12co1-0 blue:x-ray contour,radio

^_^: shape:match along with 24um IR and radio >_<: show No line broaden The 24um emissions in the east are probably ralate with the Mcs at 100km/s

blue:12co1-0 contour:radio cross:maser point

^_^. 12CO along with radio, partly along with X-ray ^_^.High 12co to 13co ratio >_<.no enough evidence to prove the MC is shocked.

1. Discovered X-ray from ROSAT and XMM 2. Near the MASER velocity, find a shell in the east, which match along with radio,IR and X-ray, and the line show some broadening. 3. We need 12CO 2-1,3-2 observations to find the shocked MCs.