1. I. Origin of the dust emission from Tycho’s SNR II. Mapping observations of [Fe II] lines and dust emission of IC443 by IRSF & AKARI III. Summary AKARI infrared observations of SNRs Ishihara Daisuke (Nagoya Univ.)

2. I. Origin of the dust emission from Tycho’s SNR Ishihara, D., et al. 2010

3. - Observed in 1572 by Tycho Brahe - Type Ia - Distance = 1.5 ～ 3.1 kpc - Detection of IR emissioin + IRAS (Schwaltz 1995) + ISO/ISOCAM (Douvion+ 2001) - Size = 8’ (5.3pc) - Extensively studied in X-ray, Radio and Optical Tycho’s SNR - Observed in 1572 by Tycho Brahe - Type Ia - Distance = 1.5 ～ 3.1 kpc - Detection of IR emissioin + IRAS (Schwaltz 1995) + ISO/ISOCAM (Douvion+ 2001) - Size = 8’ (5.3pc) - Extensively studied in X-ray, Radio and Optical Tycho’s SNR 1. Tycho’s SNR - introduction (Warren+ 2005) 4.1 -6.1 keV 1.63-2.26 keV 0.95-1.26 keV,

4. 1. Tycho’s SNR - introduction Fast expansion (0.45”/yr) Slow expansion (0.15”/yr) X-ray (Suzaku 0.1-12 keV) Molecular cloud (12CO) Hot dust (AKARI 18um) Expansion velocity from VLA 1375 Hz (Reynoso+ 1997) - Observed in 1572 by Tycho Brahe - Type Ia - Distance = 1.5 ～ 3.1 kpc - Detection of IR emissioin + IRAS (Schwaltz 1995) + ISO/ISOCAM (Douvion+ 2001) - Size = 8’ (5.3pc) - Extensively studied in X-ray, Radio and Optical Tycho’s SNR

5. 2. AKARI infrared observations X-ray (Suzaku 0.1-12 keV) Molecular cloud (12CO) Hot dust (AKARI 18um) Expansion velocity from VLA 1375 Hz (Reynoso+ 1997) - Observed in 1572 by Tycho Brahe - Type Ia - Distance = 1.5 ～ 3.1 kpc - Detection of IR emissioin + IRAS (Schwaltz 1995) + ISO/ISOCAM (Douvion+ 2001) - Size = 8’ (5.3pc) - Extensively studied in X-ray, Radio and Optical Tycho’s SNR We investigated physical state and origin of the MIR emission using AKARI (9, 15, 18, 24, 65, 90, 140, 160um) images.

6. Flux (Jy) Infrared SED of dust emission 3. Overall picture Flux (Jy) Total SED (AKARI+IRAS) is characterized by two temperatures Dust temperature ⇒ higher at outer edge (shock front) MIR map limb-brightened shell structure ⇒ Shock heated dust of IS origin Infrared SED of dust emission 15/24  m intensity ratioAKARI 9  m bandAKARI 18  m band 0.2 0.3 (100 ～ 136 K) (PAH)(Hot dust) T 1 ～ 25 K ISM T 2 ～ 95 K Shock heated dust

7. ⇒ 150 yr ⇔ 500 yr (Age of the SNR) (Draine & Salpeter 1979, Tielens et al. 1994) Time scale of the dust destruction by sputtering in hot plasma Time scale of PAH destruction is 1/100 ～ 1/1000 faster ⇒ < 1 yr... vanished C=0.79 (silicate), a=1nm, T=8.4x10 K 、 n H =10 cm 6 -3 Flux (Jy) Infrared SED of dust emission 15/24  m intensity ratioAKARI 9  m bandAKARI 18  m band 0.2 0.3 (100 ～ 136 K) (PAH)(Hot dust) ⇒ 150 yr ⇔ 500 yr (Age of the SNR) (Draine & Salpeter 1979, Tielens et al. 1994) Time scale of the dust destruction by sputtering in hot plasma Time scale of PAH destruction is 1/100 ～ 1/1000 faster ⇒ < 1 yr... vanished C=0.79 (silicate), a=1nm, T=8.4x10 K 、 n H =10 cm 6 -3 3. Overall picture T 1 ～ 25 K ISM T 2 ～ 95 K Shock heated dust 150 yr500 yr atom ISM dust is heated at the shock front and destructed by the sputtering in the post-shock hot-plasma ⇒ Shell structure of ～ 100 K

8. Flux (Jy) Infrared SED of dust emission 15/24  m intensity ratioAKARI 9  m bandAKARI 18  m band 0.2 0.3 (100 ～ 136 K) (PAH)(Hot dust) C=0.79 (silicate), a=1nm, T=8.4x10 K 、 n H =10 cm ⇒ 150 yr ⇔ 500 yr (Age of the SNR) (Draine & Salpeter 1979, Tielens et al. 1994) Time scale of the dust destruction by sputtering in hot plasma Time scale of PAH destruction is 1/100 ～ 1/1000 shorter ⇒ < 1 yr... vanished 6 -3 3. Overall picture ISM dust is heated at the shock front and destructed by the sputtering in the post-shock hot-plasma ⇒ Shell structure of ～ 100 K We focus on the two bright spots at NE and NW boundaries. NENW

9. - Large amount of cold dust at NE Spatial distribution of molecular gas, cold dust ⇒ SNR is interacting with dense medium at NE boundary ⇒ NW is relatively rich in warm dust compared with amount of molecular gas NENW Hot dust Gas (H 2 ) 2M 20M 2x10 M - 4 10 4 5 2x10 M - 4 -60 ～ -63 km/s ～ 100 K Ratio Gas/dust AKARI (cold dust) AKARI (cold dust) Flux (Jy) NENW Infrared SED of dust emission Local SED for NE region 4.1. Origin of NE and NW emission

10. Ejecta origin ISM origin ⇒ The NW warm dust could have an SN ejecta origin AKARI 18μm intensity map ー Blast wave ー Conduct discontinuity (Warren+ 2008) Contact discontinuity Blast wave Cold ISM Heated ISM Ejecta from SNR Schematic view around blast wave 4.2. Origin of dust emission at NW boundary

11. -Featureless continuum (No lines, dust features) -Composed of pure Fe? Image : AKARI mid-IR (15μm) Contour: Hα Spitzer / IRS 5~36μm spectrum IRS spectrum of Cas A (Rho+ 2008) 4.3. Composition of newly formed dusts

12. Infrared observations of Tycho’s SNR (AKARI 9-160μm) ⇒ Physical state (temperature, heating source) and origin of hot dusts Overall picture: Dusts of an ISM origin are heated and destroyed in the hot plasma NE region: Interaction with dense ISM NW region: Hot dusts without dense ISM - small gas/hot dust mass ratio - located inside the contact discontinuity ⇒ SN ejecta origin ？ First suggestion of dust formation in Type Ia SNR → impact on the transmigration of the ISM in our galaxy and early universe. Demonstrates advantage of AKARI diffuse maps combined with X-ray and 12 CO maps. 5. Summary

13. II. Mapping observations of [Fe II] lines and dust emission of IC443 by IRSF & AKARI Kokusho, T., et al. in prep.

14. 1. Introduction □ IC443 - Type II (Troja+ 2008) - Distance: ~1.5 kpc - Size: 45 amin (20 pc) - Age: ~10 4 yr - Heavy interaction with the ISM (Saken+ 1992) - Over-ionized X-ray plasma Center-filled, rapid cooling? (Kawasaki+ 2002) - [Fe II] line emission in NE part of the remnant → J-shock (Graham+ 1987) - H 2 line emission in south part of the remnant → C-shock (Rho+ 2001) IC443 Hα image

15. 30’ Saken+1992 1. Introduction □ IC443 - Type II (Troja+ 2008) - Distance: ~1.5 kpc - Size: 45 amin (20 pc) - Age: ~10 4 yr - Heavy interaction with the ISM (Saken+ 1992) - Over-ionized X-ray plasma Center-filled, rapid cooling? (Kawasaki+ 2002) - [Fe II] line emission in NE part of the remnant → J-shock (Graham+ 1987) - H 2 line emission in south part of the remnant → C-shock (Rho+ 2001) IC443 IRAS 100μm image

16. 1. Introduction □ IC443 - Type II (Troja+ 2008) - Distance: ~1.5 kpc - Size: 45 amin (20 pc) - Age: ~10 4 yr - Heavy interaction with the ISM (Saken+ 1992) - Over-ionized X-ray plasma Center-filled, rapid cooling? (Kawasaki+ 2002) - [Fe II] line emission in NE part of the remnant → J-shock (Graham+ 1987) - H 2 line emission in south part of the remnant → C-shock (Rho+ 2001) IC443 ASCA 0.7-10 keV image 30’ Contours: softness ratio (Kawasaki+ 2002)

17. 1. Introduction □ IC443 - Type II (Troja+ 2008) - Distance: ~1.5 kpc - Size: 45 amin (20 pc) - Age: ~10 4 yr - Heavy interaction with the ISM (Saken+ 1992) - Over-ionized X-ray plasma Center-filled, rapid cooling? (Kawasaki+ 2002) - [Fe II] line emission in NE part of the remnant → J-shock (Graham+ 1987) - H 2 line emission in south part of the remnant → C-shock (Rho+ 2001) IC443 2MASS image Blue: J, green: H, red: Ks-band (blue; [Fe II],Pβ, red: H 2 )

18. 1. Introduction □ IC443 - Type II (Troja+ 2008) - Distance: ~1.5 kpc - Size: 45 amin (20 pc) - Age: ~10 4 yr - Heavy interaction with the ISM (Saken+ 1992) - Over-ionized X-ray plasma Center-filled, rapid cooling? (Kawasaki+ 2002) - [Fe II] line emission in NE part of the remnant → J-shock (Graham+ 1987) - H 2 line emission in south part of the remnant →C-shock (Rho+ 2001) IC443 2MASS image Blue: J, green: H, red: Ks-band (blue; [Fe II],Pβ, red: H 2 ) Based on observations of [Fe II] line emissions and IR dust emissions, we discuss on supply of Fe element from SNRs to the ISM.

19. 2. FIR images from AKARI all-sky survey 65  m 90  m 140  m160  m 90MJy/sr110MJy/sr 240MJy/sr 300MJy/sr 65 90140160 dust [CII][OI]

20. 2. FIR images from AKARI all-sky survey 90  m 140  m 110MJy/sr 240MJy/sr 65 90140160 dust [CII][OI] [CII] Contours: 140  m

21. 2. FIR images from AKARI all-sky survey 90  m 140  m 110MJy/sr 240MJy/sr 65 90140160 dust [CII][OI] [CII] Contours: 140  m AKARI 2.5 – 5  m spectra

22. 2. FIR images from AKARI all-sky survey 65  m 160  m 90MJy/sr 300MJy/sr 90  m 140  m 110MJy/sr 240MJy/sr 65 90140160 dust [CII][OI]

23. 2. FIR images from AKARI all-sky survey 65  m 160  m 90MJy/sr 300MJy/sr 90  m 140  m 110MJy/sr 240MJy/sr 65 90140160 dust [CII][OI] Broad bands tracing dust emission with small contribution of [OI] 63μm and [CII] 158μm line emissions. → Derive hot-dust mass distribution by fitting dust SEDs composed of Spitzer 24μm, AKARI 90μm, and 140μm intensities.

24. 3. Observations of [Fe II] lines [Fe II] 1.256μm : 4 D 7/2 → 6 D 9/2 [Fe II] 1.644μm : 4 D 7/2 → 4 F 9/2 Transitions from same level. → The intensity ratio is theoretically derived from Einstein A-coeffs. (Narayan+ 2010) → Accurate Av correction → Av-free [Fe II] intensity Narrow-band filters for [Fe II] 1.256μm & 1.644μm IRSF telescope of Nagoya Univ. (at South Africa) Nagayama+ 2008 (μm) (%) J J H H 1.256 1.644 Pβ

25. 3. Origin of [Fe II] emission ISM: ~98 % of Fe is depleted on dust grains [Fe II] 1.64μm / Br γ ~1 SNRs: Fast shocks (~100 km/s) ⇒ destruction of dust grains [Fe II]1.64μm / Br γ ~100 (Koo+ 2007) [Fe II] IP: 7.9 eV (< 13.6 eV) In equilibrium hot plasma (T=10 7 K), most of Fe is Fe 20+ no Fe 1+ → Tracers of fast shocks, young SNRs (Mazzotta+ 1998) atom

26. 3. [Fe II] distribution IRSF [Fe II] 1.256μm IRSF [Fe II] 1.644μm → Derive Fe mass distribution from Av-free [Fe II] intensities assuming LTE with T~10 4 K. (erg/s/cm 2 /sr) 2MASS J, H, Ks

27. 3. [Fe II] distribution [Fe II]1.644μm Contours: Hα + [NII] AKARI 18μm (hot dust) AKARI 9μm (PAH, H 2 lines) atom

28. → M dust 4. Comparison of dust mass and Fe mass □ Dust mass related to the SNR □ Fe + mass SED fitting by 2 temp. B.B. - Hot dust … shock heated - Cold dust … (foreground or background ?) Hot dust component assuming, a=0.1μm, Q abs =30cm 2 g -1 (Hildebrand 1983) (μm) M Fe = N ・ (unit mass)

29. 4. Discussion Fe / hot dust mass ratio 10’ - Fe / hot dust mass ratio shows excess in some regions. Solar abundance ~ 0.4 (excess amount ~10 6 M sun ) Dust mass Fe + mass AKARI IR SED IRSF [Fe II]

30. 4. Comparison of time scales Fe 1+ disappears at ionization equilibrium (T e =10 7 K) □ Life time of dust grains in hot plasma: □ Time scale to reach ionization equilibrium : (Darine+ 1979) In the hot plasma of T e =10 7, n e =1.7 cm -1, a dust =0.1μm (Yamaguchi+ 2009, Petre+ 1988) (yr) (Masai 1994) ⇒ ~ 1x10 5 yr ⇒ ~ 2x10 4 yr → [Fe II] line emissions attenuate faster than IR dust emission.

31. 4. Discussion Fe / hot dust mass ratio 10’ ⇒ Fe ejected from SNR ? - Fe / hot dust mass ratio shows excess in some regions. Solar abundance ~ 0.4 (excess amount ~10 6 M sun ) Dust mass Fe + mass AKARI IR SED IRSF [Fe II] - [Fe II] line emissions attenuate faster than IR dust emission.

32. 5. Summary AKARI mid-& far-infrared & IRSF near-IR observation of IC443 Northern region: [Fe II] originated by dust sputtering in J-shock Southern region: H 2 and [O I] in C-shock Accurate correction of extinction by observing two [Fe II] lines Fe + / hot dust mass ratio shows excess in some parts of IC443 → [Fe II] line emissions attenuate faster than IR dust emission → Fe of an SN ejecta origin ?

33. III. Summary Interaction of SNRs with the dense ISM → IR observations Fe in ejecta of SNRs Tycho’s SNR (10 -4 M sun ) … Type Ia IC443 (10 -6 M sun ) … Type II Utilization of AKARI All-Sky diffuse maps (shock tracer, past shock tracer, as well as indicators of dust temperature, dust mass, etc.)