1. 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) 〜 Toru Tamagawa( RIKEN/Tokyo Univ. of Science), Satoru Katsuda (RIKEN)

2. Type Ia SN progenitor have many questions Type Ia SN metallicity depends of luminosity What is the nature of the progenitor? -- Double Degenerate or Single Degenerate? -- prompt or delay channel? What are nucleosynthesis? What is progenitor metallicity? 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. many questions become detectable with Suzaku

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

4. 52 Fe (Z=26, N=26)→ 52 Mn → 52 Cr 55 Co(Z=27, N=28)→ 55 Fe → 55 Mn 56 Ni(Z=28, N=28)→ 56 Co → 56 Fe On the explosion electron capture reaction is slow = keep the state of the neutron excess In incomplete Si burning more Mn was born A tight correlation between the Mn to Cr mass ratio and the progenitor metallicity (Z). independent on explosion mechanisms and initial conditions M Mn /M Cr = 5.3 Z 0.65 (Badenes+ 2008) 〜 the neutron excess increases Mn 〜 the neutron excess Z: atomic number, N: neutron number ※ But reverse shock does not reach the center because the center reacted electron capture. A new method to measure progenitor metallicity

5. 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 … Our Galaxy Detecting Cr and Mn lines in SNRs average abundance : 0.3 times the solar Mn/Cr mass ratio in Large Magellanic cloud (LMC) SNRs is expected to be smaller than those in our Galaxy. (Tamagawa+2009) Tycho SNR What about extra galaxy?

6. N103B, SNR 0509-67.5 & SNR 0519-69.0 SNR 0519-69.0 SNR 0509-67.5 ( from Chandra HP ) N103BSNR 0509-67.5SNR 0519-69.0 typeIa age 〜 1000 years 〜 400 years 〜 600 years radius 〜 7.3 pc 〜 3.6 pc 〜 4 pc Suzaku observation 〜 50 ksec (2005) 〜 220 ksec(2009) 〜 50 ksec 〜 350 ksec (Rest+2005) N103B ( from Chandra HP ) SNRs located in LMC ( 〜 50 kpc from the Earth ) (Hughes+ 1995) ( from Chandra HP )

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

8. vpshock model for ISM (1), vpshock model for ejecta （ high n e t (2), low n e t (3) ), emission line [gaussian model] (0.73keV(4), Cr(5)) Analysis of N103B (0.4keV 〜 6keV) 星間物質 (ISM) kT e : 0.1 [keV] n e t ： 2.1×10 12 ejecta 成分 (2) kT e : 0.7 [keV] n e t ： 5×10 13 ejecta 成分 (3) kT e : 0.1 [keV] n e t ： 2.5×10 11 black ： FI (2005) red ： FI (2009) green ： BI (2009) (1) (2) (3) (4) (5) abund. [solar] Type Ia W7 Type II (**M sun ) O3.2±0.2 Ne3.5±0.3 Mg2.0±0.1 Si4.5±0.2 S7.9±0.4 Ar9.2±0.5 Ca13.5±0. 9 Fe3.9±0.2 [solar] N103B (2009vers.) Suzaku image model ： abund. ratio observed Type Ia W7 Type II (20M sun ) Mg/Si 0.4 4±0.030.0612.07 S/Si 1.7 6±0.121.0740.5 Ar/Si 2.0 4±0.140.7510.35 Ca/Si 3.0 0±0.240.8910.42 χ ２ /dof =2176 /1634 Relative abundances suggest type Ia origin. efecta が確定している元素は

9. χ ２ /dof =153/163 Cr ： Fe ： Flux [x10 -6 ph/cm 2 /s] [x10 -6 ph/cm 2 /s] 5.61(5.59 – 5.64) 6.464(6.458 – 6.472) 6.610(6.602 – 6.616) = Fe line center E [keV] 1.2 (0.9 – 1.6) line width x10 -2 [x10 -2 keV] < 0.5× 10 -6 (90% err) < 0.4× 10 -6 ( 1σ err) 3.3 (1.5– 4.9) 10.5(10.1 – 10.9) black ： FI (2005) red ： FI (2009) green ： BI (2009) N103B (2009vers.) Suzaku image Analysis of N103B (4.3 〜 7.5 keV) model : bremss +gaussian (Ca, Cr, Fe) Fe Ca Cr We introduced a line emission for Mn. An upper limit of Mn norm is … 4.37.5

10. Analysis of SNR 0509-67.5 & 0519-69.0 SNR 0509-67.5 vpshock model for ejecta （ low kT e (1), high kT e (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 Type Ia W7 Type II (20M sun ) O/Si0.05 ± 0.01 (ND) 0.0701.14 Ne/Si0.02±0.01 (ND)0.0051.08 Mg/Si0.03 ± 0.010.10 ±0.010.0612.07 S/Si1.28 ± 0.171.60 ±0.161.0740.5 Ar/Si1.23 ± 0.332.08 ±0.220.7510.35 Ca/Si1.55 ± 0.843.10 ±0.340.8910.42 Fe/Si0.33±0.061.18 ±0.131.880.30 SNR 0519-69.0 (ignroe under 1.1 keV due to a calibration) ※ Fe abundance based on Fe-L Relative abundances resemble those in type Ia. χ ２ /dof =978/716 χ ２ /dof =1573/1139 (1) (2) (4) (3) (1) (2) 1.1

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

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

13. LMC SNRs 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) Summary (Badenes + 2008) We found Mn/Cr mass ratio is smaller than that expected in our Galaxy. We observed N103B, SNR 0509-65.7, 0519-69.0 with Suzaku We need much more photons to better constrain the Mn/Cr ratio and metallicity on the progenitor star. ・ N103B ・・・ ・ Others ・・・ Future work We could not obtain strong constraints due to poor statistics. In wide band spectra, Relative abundances suggest type Ia origin. M Mn /M Cr = 5.3 Z 0.65 In spectra at 4 keV 〜, In this talk

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

16. N103B SNR 0519-69.0 (Badenes+2008) Our Galaxy : 0.019 (Anders & Grevesse 1989) G344.7 (Yamaguchi+2012) solar LMC Kepler

17. Mn/Cr flux ratio black ： FI (2005) red ： FI (2009) green ： BI(2009) black ： FI red ： BI We fixed a emission line of Mn. An upper limit of Mn norm is … SNR 0519-69.0 N103B 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) red ： N103B, green : SNR 0519-69.0 blue ： Tycho (Tamagawa+2009), pink : Kepler SNR, G344.7-0.1 N103B Tycho (Tamagawa+2009) G344.7-0.1 (Yamaguhi+2012) Kepler SNR SNR 0519-69.0