Supernova remnants in the AKARI FIS All-Sky Survey

1. Il-GyoJeong, Bon-Chul Koo(Seoul National Univ.), Ho-Gyu Lee (The University of Tokyo) Distributions of Known SNRs Supernova remnants in the AKARI FIS All-Sky Survey Why Far-IR for SNRs ??? IR detection rate ► All-Sky Survey • IRAS - Arendt et al. (1989): 19% (30/157) - Saken et al. (1992): 22% (35/161) • AKARI - This work: 23% (63/274) ► Glimpse Field (65°>|l|>10°, |b|<1°) - IRAS: 17% (Arendt et al. 1989), 18% (Saken et al. 1992) - Spitzer IRAC band: 16% (16/100; Lee 2005) 20% (18/95; Reach et al. 2006) - Spitzer MIPS band: 32% (39/121; Goncalves et al. 2011) - This work: 26% (31/121) • Observations of SNRs are relatively rare in far-IR. • The swept-up dust is the major coolant of a SNR and plays a role • in the SNR evolution. • Far-IR is a better means of studying the dust formed during the • process of supernova explosion. • Far-IR is more sensitive to old supernova remnants. • Far-IR emission is enhanced, where a SNR interacts with dense • ISM.

2. Morphological Type of Far-IR emission •Shell Type – 19/63 (30%) ex) 3C391 (7’X5’) • Central Brightened Type – 44/63 ex) G349.7+0.2 (2.5’X2’) Far-IR (WL, N160) bright SNR • SED fitting result (distance: 1.5kpc) - Tdust: 19 ~ 78 K, - Mdust: 0.02 ~ 32 M (Data: IRAS(24, 60, 100μm) + AKARI) • IC443 (G189.1+3.0; 45’) → White circles (1~3): shocked molecular regions (Snell et al. 2005). → Bright Far-IR emissions show spatial agreement with shocked molecular region. These features show the evidence of the shocked medium.