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Rie Yoshii ( RIKEN/Tokyo Univ. of Science)

すざくで観測した N103B. Observation of N103B by Suzaku. 〜together with SNR 0509-67.5 and SNR 0519-69.0 (type Ia SNRs in LMC) 〜. Rie Yoshii ( RIKEN/Tokyo Univ. of Science). Toru Tamagawa ( RIKEN/Tokyo Univ. of Science) , Satoru Katsuda (RIKEN). Type Ia SN progenitor have many questions.

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Rie Yoshii ( RIKEN/Tokyo Univ. of Science)

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  1. すざくで観測したN103B Observation of N103B by Suzaku 〜together with SNR 0509-67.5 and SNR 0519-69.0 (type Ia SNRs in LMC) 〜 Rie Yoshii ( RIKEN/Tokyo Univ. of Science) Toru Tamagawa( RIKEN/Tokyo Univ. of Science), Satoru Katsuda (RIKEN)

  2. Type Ia SN progenitor have many questions Type Ia SN What is the nature of the progenitor? -- Double Degenerate or Single Degenerate? -- prompt or delay channel? What are nucleosynthesis? What is progenitor metallicity? many questions metallicity depends of luminosity etc… to know the environment when the progenitor was born Recently, Badenes et al. (2008) proposed a new method to measure progenitor metallicity from the Cr and Mn lines from SNR in X-ray spectra. become detectable with Suzaku

  3. A new method to measure progenitor metallicity 〜Metallicity ∝ neutron excess〜 Before the explosion metallicity Z ∝ number of C+N+O ・H burning phase the CNO pile up into 14N due to CNO cycle ( In this time, C, N and O is catalysis, and the total number does not change. ) ・He burning phase On the reaction 14N(α, γ)18F(β+, ν)18O(α, γ) 22Ne the neutron excess of the WD material Metallicity Z ∝ neutron excessη η ＝1- 2<ZA/A>= 0.101 × Z (Timmes et al. 2003)

  4. A new method to measure progenitor metallicity 〜 the neutron excess increases Mn 〜 On the explosion In incomplete Si burning Z: atomic number, N: neutron number the neutron excess more Mn was born A tight correlation between the Mn to Cr mass ratio and the progenitor metallicity (Z) . independent on explosionmechanisms and initial conditions MMn/MCr = 5.3 Z0.65 (Badenes+ 2008) ※ But reverse shock does not reach the center because the center reacted electron capture. electron capture reaction is slow = keep the state of the neutron excess

  5. Detecting Cr and Mn lines in SNRs We hope to find emission lines of Cr and/or Mn in type Ia SNR. At this moment, the discovery of the lines are few Tycho SNR, Kepler SNR, G344.7-0.1 … Tycho SNR (Tamagawa+2009) Our Galaxy What about extra galaxy? Mn/Cr mass ratio in Large Magellanic cloud (LMC) SNRs is expected to be smaller than those in our Galaxy. average abundance : 0.3 times the solar

  6. N103B, SNR 0509-67.5 & SNR 0519-69.0 SNR 0519-69.0 SNRs located in LMC (〜50 kpc from the Earth ) SNR 0509-67.5 N103B ( from Chandra HP ) ( from Chandra HP ) ( from Chandra HP ) (Rest+2005) (Hughes+ 1995)

  7. Suzaku (X-ray satellite) Suzaku is the fifth Japanese X-ray astronomy satellite launched on July 10, 2005. Instrument used X-Ray Imaging Spectrometer (XIS) (0.2-12 keV) frontside illuminated (FI), backside illuminated (BI) XIS Characteristics high sensitivity above 5 keV high energy resolution suitable to detect Cr/Mn lines

  8. Analysis of N103B(0.4keV〜6keV) N103B (2009vers.) vpshock model for ISM (1), vpshock model for ejecta（high net (2), low net (3) ), emission line [gaussian model] (0.73keV(4), Cr(5)) model： black：FI (2005) red：FI (2009) green：BI (2009) Suzaku image (3) (4) (2) (1) 星間物質(ISM) kTe: 0.1 [keV] net：2.1×1012 ejecta成分(2) kTe: 0.7 [keV] net：5×1013 ejecta成分(3) kTe: 0.1 [keV] net：2.5×1011 (5) χ２/dof =2176 /1634 [solar] Relative abundances suggest type Ia origin. efectaが確定している元素は

  9. Analysis of N103B (4.3〜7.5 keV) N103B (2009vers.) model : bremss +gaussian (Ca, Cr, Fe) black：FI (2005) red：FI (2009) green：BI (2009) Fe Ca Cr Suzaku image We introduced a line emission for Mn. An upper limit of Mn norm is … 4.3 7.5 χ２/dof =153/163 Flux [x10-6 ph/cm2/s] line center E [keV] line width [x10-2keV] < 0.5× 10-6 (90% err) < 0.4× 10-6 ( 1σ err) Cr： Fe： = Fe 5.61(5.59 – 5.64) 6.464(6.458 – 6.472) 6.610(6.602 – 6.616) 1.2 (0.9 – 1.6) 3.3 (1.5– 4.9) 10.5(10.1 – 10.9)

  10. Analysis of SNR 0509-67.5 & 0519-69.0 vpshock model for ejecta（low kTe(1), high kTe(2) ), emission line [gaussian model] (0.73keV(3)) model： black：FI(1) red：BI green:FI(2) SNR 0509-67.5 SNR 0519-69.0 (2) (2) (3) (1) (1) (4) χ２/dof =1573/1139 χ２/dof =978/716 1.1 (ignroe under 1.1 keV due to a calibration) Relative abundances resemble those in type Ia. ※ Fe abundance based on Fe-L

  11. Analysis of SNR 0509-67.5 & 0519-69.0(4keV〜) SNR 0519-69.0 model : bremss + three gaussian (Ca, Cr, Fe) SNR 0519-69.0 SNR 0509-67.5 black：FI red：BI Fe Ca Cr χ２/dof = 127/89 7.5 4 7.5 4 Flux [x10-6 ph/cm2/s] line center E [keV] line width [x10-2keV] Not enough statistics … Cr： Fe ： = Fe 7.5 (6.5– 8.4) 0.4(0.1 – 0.7) 9.5 (9.0 – 10.1) 5.65(5.576 – 5.76) 6.489(6.482 – 6.495) upper limit of Cr： < 0.4 × 10-6 (90% err) < 0.2 × 10-6 ( 1σ err ) An upper limit of Mn flux is … < 0.3 × 10-6 (90% err) < 0.2 × 10-6 ( 1σ err)

  12. Discussion If the emissivities of N103B or SNR 0519-69.0 are similar to those of Tycho SNR (Badenes+2008) Their Mn to Cr mass ratio is MMn/MCr = 1.057 × ( FMn /FCr ) / ( εMn /εCr ), the ratio of specific emissivities per ion the ratio of atomic masses the line flux ratio LMC Upper limit of MMn/MCr is … N103B : < 0.3 SNR 0519-69.0 : < 0.43 (1σ err) SMC our Galaxy SNR 0519-69.0 N103B N103B measured Mn/Cr mass ratio suggests lower metallicity than that in our Galaxy as expected. (Badenes+2008)

  13. Summary Suzaku is able to detect Mn/Cr lines, which allows us to estimate metallicity of Ia progenitor for the first time ; a tight correlation between the Mn to Cr mass ratio and the progenitor metallicity (Z) (Badenes + 2008) MMn/MCr = 5.3 Z0.65 In this talk We observed N103B, SNR 0509-65.7, 0519-69.0 with Suzaku LMC SNRs In wide band spectra, Relative abundances suggest type Ia origin. In spectra at 4 keV〜 , We found Mn/Cr mass ratio is smaller than that expected in our Galaxy. ・N103B ・・・ ・Others ・・・ We could not obtain strong constraints due to poor statistics. Future work We need much more photons to better constrain the Mn/Cr ratio and metallicity on the progenitor star.

  14. N103B, SNR 0509-67.5 & SNR 0519-69.0 ASCAでの観測 (Hughes+ 1995) SNR 0509-67.5 SNR 0519-69.0 N103B

  15. Mn/Cr flux ratio flux ratio of Mn/Cr • N103B • < 0.7 × 10-6 (90% err) • < 0.5 × 10-6 ( 1σ err) • SNR 0519-69.0 • < 0.3 × 10-6 (90% err) • < 0.2 × 10-6 ( 1σ err) G344.7-0.1 (Yamaguhi+2012) SNR 0519-69.0 Tycho (Tamagawa+2009) Kepler SNR N103B red：N103B, green : SNR 0519-69.0 blue：Tycho (Tamagawa+2009), pink : Kepler SNR, G344.7-0.1 N103B SNR 0519-69.0 We fixed a emission line of Mn. An upper limit of Mn norm is … black：FI (2005) red：FI (2009) green：BI(2009) black：FI red：BI

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