1. Suzaku Observation of Tycho’s Supernova Remnant
Asami Hayato
(RIKEN / Tokyo Univ. of Sci.)
and
Suzaku Tycho’s SNR Team

2. Tycho’s SNR (G120.1+1.4) Suzaku Observation
◇ Originated in the SN in 1572
◇ Observed by Tycho Brahe
◇ Categorized as Type Ia
◇ Distance = ~3 kpc
Ideal prototype of
Type Ia SNRs
Suzaku Observation
◇ Image
◇ Spectrum of Entire SNR
1. Non-thermal Emission
2. Rare Metals (Cr, Mn)
3. Onion-like Structure
XIS
HXD
Si Hea, Fe Ka, <7keV

3. Past Observations Past observations have difficulty distinguishing
1. Non-thermal Emission
Past Observations
4-6 keV
◇ ASCA
◇ Chandra
(Hwang+ 1998)
(Warren+ 2005)
Low temp. (0.86keV)
High temp. (1.6 keV)
Additional Component
No line feature at the rim
(Γ~2.7 or kT~2 keV) 1 2 10 1 2
5 (keV)
Past observations have difficulty distinguishing
the non-thermal from thermal emission.

4. Suzaku Spectra (Tamagawa et al. 09)
1. Non-thermal Emission
Suzaku Spectra (Tamagawa et al. 09)
◇ Single Thermal Model
◇　Double Thermal Model
kT=5.14 ( ) keV
Data Excess
kThigh >10 keV
Counts s-1 keV-1
XIS
Unrealistic (Temp is too high.)
HXD
◇ Thermal + Non-thermal Model χ
G~2.7
F10-20keV~1.3x10-11 5 10 20
Energy　(keV)
Consistent
with Chandra
Observation
Another component is required.
Suzaku can discriminate non-thermal & thermal emission.

5. Detection of Cr and Mn 2. Rare Metals
◆ Past Observations of Cr and Mn in SNRs
◇ W49B : Miceli+ 06, Hwang+ 00
◇ CasA, Kepler, Tycho (Only Cr) : Yang+ 09
◇ N103B : Yamaguchi+ 09
◆ Suzaku Spectrum of Tycho’s SNR (Tamagawa+ 09)
The ionization degrees of Cr and Mn
are almost same as that of Fe.

6. What do Cr and Mn tell us ? 2. Rear Metals
Mn : Very efficient at storing the neutron excess
Cr : Insensitive to the neutron excess
Both are produced during incomplete Si burning
MMn/MCr : Excellent tracer of the progenitor metallicity Z .
Aspulnd+ 05
Suzaku
measurement
0.74±0.47
Badenes+ 08

7. Radial Line Profiles (Furuzawa+ 09) (Hayato+ 09)
3. Onion-like Structure
(Furuzawa+ 09)
(Hayato+ 09)
Radial Line Profiles NE NW SE SW
He-like S Kα
He-like Ar Kα
He-like Ca Kα
Fe Kα Blend
He-like Si Kα

8. Why are lines broadened ?
3. Onion-like Structure
Why are lines broadened ?
◇ Plasma in multi status
(temp., ionization age)
◇ Doppler effects by
shell expansion？
Outside
Outside
Inner
Inner
Observer
Observer
Red Shifting
Blue Shifting
◆ “Plasma in multi status” can not make Si Hea line broaden.
◆ “Plasma in multi status” make the centroids vary with radius.
“Plasma in multi status” conflicts with our observations.

9. Analysis with Shell Expansion Model
3. Onion-like Structure
Analysis with Shell Expansion Model
Si Hea
S Hea
Red-shifting
Blue-shifting
Aa Hea
Fe Ka
Ca Hea

10. Velocities of Ejecta (Hayato et al. 09)
3. Onion-like Structure
Velocities of Ejecta (Hayato et al. 09)
Iwamoto+ 99

11. Summary
◇ Suzaku XIS+HXD spectra allow to distinguish the non-thermal emission from the thermal emission.
◇ Suzaku detects the line emission of Cr and Mn from Tycho’s SNR for the first time.
◇ The spectrum analysis with a shell expansion model confirms an onion-like structure of Tycho’s SNR; the ejecta are stratified with the inner Fe and outer Si, S, Ar, and Ca.

13. It does not change our results: the inner Fe and outer IME.
3. Onion-like Structure
Red = Blue ?
Si Hea
S Hea
Red-shifting
Blue-shifting
Fe Ka
Ar Hea
Ca Hea
It does not change our results: the inner Fe and outer IME.

14. 3. Onion-like Structure
Red = Blue ?
Observer
Observer

15. Lee+04