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

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

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.

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 (5.02-5.28) 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.

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.

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

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

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.

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

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

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.

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.

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

Lee+04