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The Onion-like Metallicity Structure of Tycho’s SNR as revealed by Doppler Broadened Lines

The Onion-like Metallicity Structure of Tycho’s SNR as revealed by Doppler Broadened Lines. Asami Hayato (RIKEN / Tokyo Univ. of Sci.) T. Tamagawa, H. Yamaguchi (RIKEN), A. Furuzawa, H. Kunieda (Nagoya Univ.), M. Ozawa (Kyoto Univ.), J. P. Hughes (Rutgers Univ.),

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The Onion-like Metallicity Structure of Tycho’s SNR as revealed by Doppler Broadened Lines

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  1. The Onion-like Metallicity Structure of Tycho’s SNR as revealed byDoppler Broadened Lines Asami Hayato (RIKEN / Tokyo Univ. of Sci.) T. Tamagawa, H. Yamaguchi (RIKEN), A. Furuzawa, H. Kunieda (Nagoya Univ.), M. Ozawa (Kyoto Univ.), J. P. Hughes (Rutgers Univ.), U. Hwang (NASA/GSFC), A. Bamba (ISAS/JAXA), K. Makishima (Univ. of Tokyo/RIKEN), and Suzaku Tycho’s SNR team

  2. Tycho’s SNR ◇ Originatedin the SN in 1572 ◇ Observed by Tycho Brahe ◇ Categorized as Type Ia ◇ Distance = ~3kpc ◇ Diameter = ~8 arcmin Ideal prototype of Type Ia SNRs

  3. Past Observations Fe Ka Si, S Low Temp (0.86 keV) High Ionization Age (1011cm-3 s) Fe L, Si, Fe Ka Fe Ka High Temp (1.6 keV) Low Ionization Age (109cm-3 s) ◇ Image Analysis ◇ Spectral Analysis ASCA　(Hwang & Gotthelf 97) ASCA (Hwang+98) Si Fe K XMM-Newton　(Decucell+01) Si Fe K

  4. Suzaku Observation ◇ Observation Date: June 27-29, 2006 (SWG time) Exposure: 95 ks ◇ XIS Image ◇ Spectrum of Entire SNR ◇ Non-thermal emission ⇒ Tamagawa+09 ◇ Low abund. metals (Cr, Mn) ⇒ Poster XIII-30 (Tamagawa+), Tamagawa+09 ◇ Onion-like Structure ⇒ This talk XIS HXD Si (He-like) Ka, Fe Ka,>7keV

  5. Fe Kα Line Broadening 6 7 (keV) Furuzawa+09

  6. Spatially Resolved Spectra Si He-like Kβ S He-like Kα Ar He-like Kα Ca He-like Kα Fe Kα Blend 1 2 3 4

  7. Radial Line Profiles 5eV 17eV 1 13eV 2eV 2 3 4 16eV 6eV 41eV 27eV 42eV 12eV Line Center (keV) 1σ Width (eV) Si S Ar Ca Gain variation across the SNR is within ±0.2-0.5% (Ota+07) Fe 1 2 3 4 1 2 3 4 Radius (arcmin)

  8. Why are lines broadened? ◇ Plasma in multi-nt (ionization age) ? ◇ Doppler effects by shell expansion ? Non-equilibrium ionization collisional plasma model High nt Low nt E E Si Kα Fe Kα Low nt Observer Red Shifting Blue Shifting E E High nt Line Center Line Width Line Center Line Width Observation ~30 eV (Si, S) ~100 eV (Fe) radius radius radius radius

  9. Analysis with Shell Expansion Model 2DE DE v = E0 c Si S Ar Fe

  10. Velocities of Ejecta Si S Fe Fe Si, S Iwamoto+99 Velocity of each element, Independent of the distance. Si S Velocity in km/s (This work) Ar Fe Radial peak in arcmin (ASCA: Hwang & Gotthelf 97)

  11. Summary ◇ Suzaku observed Tycho’s SNR inJune 2006. ◇ Line broadening was detected at the center of the SNR. ◇ We successfully derived velocities of ejecta for the first time, assuming the shell expansion model. ◇ Si and S ejecta have higher velocities (~3500 km s-1) than Fe ejecta (~3000 km s-1). ◇ We are looking forward to see the data from SXS/Astro-H !

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