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.)

SWAS (1.4-2.8GHz, chemical composition,

Submillimeter Wave Astronomy Satellite )

ISO (2.5-240 um, Infrared Space Observatory )

COSMOS(x-rayradio, Cosmic Evolution Survey)

SDSS( Sloan Digital Sky Survey )

Spitzer(10d<|l|<65d, |b|<1d, Galactic Legacy Infrared

Mid-Plane Survey Extraordinalire [GLIMPSE])

• DA530(G 93.3 +6.9 )

• IRAS(12,25,60,100)um

• 0.5-2arcmin / 27x20 arcmin

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

• 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

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)

Sloan Digital Sky Survey

1E0102.2-7219 (SMC 52kpc)

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.

• Spitzer (24,70,160um)

• 2.4-15 arcsec

THANKS