1. Infrared SNRs in the Spitzer Space Telescope astro-ph/0509786(APJL, Snezana Stanimirovic et al.) astro-ph/0510518(JKAS, Ho-Gyu Lee) astro-ph/0510630(AJ, Reach & Rho et al.)

6. SWAS (1.4-2.8GHz, chemical composition, Submillimeter Wave Astronomy Satellite ) ISO (2.5-240 um, Infrared Space Observatory ) COSMOS(x-ray  radio, Cosmic Evolution Survey) SDSS( Sloan Digital Sky Survey ) Spitzer(10d<|l|<65d, |b|<1d, Galactic Legacy Infrared Mid-Plane Survey Extraordinalire [GLIMPSE])

7. DA530(G 93.3 +6.9 ) IRAS(12,25,60,100)um 0.5-2arcmin / 27x20 arcmin

17. 1.IRAS: 12+(10)/70 (8), Arendt 1989 14+(4)/75 (8), Saken et al. 1992 2.MSX: 8/200 (5), Kim et al. 2005 3.2MASS: (Crab, IC 443, Cas A, RCW 103) 4.Spitzer: 8+(5+3)/100, Lee 2005JKAS 13+5+(17)/95, Reach & Rho 2005AJ

20. A. shock-heated dust grains, line emission, synchrotron emission. (molecular or ionic shocks or PAH emission) B. complete or partial shells, partial filaments or combination filaments  generally coincide with the radio continuum

22. 1.HII regions of the galactic plane(~8um), PAH(~8um), star light (~3.6um)  IPAC tell us little information about dust emission 2.Molecular shock =/= OH masers(more strict)

25. Sloan Digital Sky Survey 1E0102.2-7219 (SMC 52kpc)

26. 1.The 24 um distribution decreases less sharply than the X-ray distribution. 2.IR emission peaks around 24um(OIV25.88um, FeII25.98um [RCW103, CasA]), and sharply falls off toward shorter and longer wavelengths.

27. Spitzer (24,70,160um) 2.4-15 arcsec

29. THANKS