Rie Yoshii ( RIKEN/Tokyo Univ. of Science)

すざくで観測した N103BObservation 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)

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

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 14N(α, γ)18F(β+, ν)18O(α, γ) 22Ne

Metallicity Z neutron excess∝ η

A new method to measure progenitor metallicity

metallicity Z number of C+N+O∝

the CNO pile up into 14N due to CNO cycle

〜 Metallicity neutron excess∝ 〜

η ＝ 1- 2<ZA/A>= 0.101 × Z (Timmes et al. 2003)

52Fe (Z=26, N=26) →52Mn → 52Cr55Co (Z=27, N=28) → 55Fe → 55Mn56Ni (Z=28, N=28) → 56Co → 56Fe

On the explosionIn 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

MMn/MCr = 5.3 Z0.65

(Badenes+ 2008)

〜 the neutron excess increases Mn 〜

the neutron excess Z: atomic number, N: neutron number

A new method to measure progenitor metallicity

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?

N103B, SNR 0509-67.5 & SNR 0519-69.0

SNR 0519-69.0SNR 0509-67.5

( from Chandra HP )

N103B SNR 0509-67.5 SNR 0519-69.0type Ia Ia Iaage 〜 1000 years 〜 400 years 〜 600 years

radius 〜 7.3 pc 〜 3.6 pc 〜 4 pcSuzaku

observation〜 50 ksec (2005)

〜 220 ksec(2009)

〜 50 ksec 〜 350 ksec

N103B

( from Chandra HP )

SNRs located in LMC ( 〜 50 kpc from the Earth )

( from Chandra HP )

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

vpshock model for ISM (1), vpshock model for ejecta （ high net (2), low net (3) ), emission line [gaussian model] (0.73keV(4), Cr(5))

Analysis of N103B (0.4keV 〜 6keV)

black ： FI (2005)red ： FI (2009)green ： BI (2009)

(1) (2)

(3)

(4)

(5)

[solar]

N103B (2009vers.)

Suzaku image

model ：

abund. ratio observed Type Ia

W7Type II

(20Msun)

Mg/Si 0.44 ± 0.03 0.061 2.07

S/Si 1.76 ± 0.12 1.074 0.5

Ar/Si 2.04 ± 0.14 0.751 0.35

Ca/Si 3.00 ± 0.24 0.891 0.42

χ ２ /dof =2176 /1634

Relative abundances suggest type Ia origin.

χ ２ /dof =153/163

Cr ：Fe ：

FluxFlux [x10[x10-6 -6 ph/cmph/cm22/s]/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[x10x10-2-2keV]

< 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)

Analysis of N103B (4.3 〜 7.5 keV)model : bremss +gaussian (Ca, Cr, Fe)

FeCaCr

We introduced a line emission for Mn.

An upper limit of Mn norm is …

4.3 7.5

Analysis of SNR 0509-67.5 & 0519-69.0

SNR 0509-67.5

vpshock model for ejecta （ low kTe(1), high kTe (2) ), emission line [gaussian model] (0.73keV(3))

model ：black ： FI(1)red ： BIgreen:FI(2)

SNR 0509-67.5

SNR 0519-69.0

Type Ia

W7

Type II (20Msun)

O/Si 0.05 ±

0.01

(ND)0.070 1.14

Ne/Si 0.02

±0.01

(ND)0.005 1.08

Mg/Si 0.03

±0.01 0.10 ±0.01 0.061 2.07

S/Si 1.28 ±

0.17 1.60 ±0.16 1.074 0.5

Ar/Si 1.23 ±

0.33 2.08 ±0.22 0.751 0.35

Ca/Si 1.55 ±

0.84 3.10 ±0.34 0.891 0.42

Fe/Si 0.33 ±

0.06 1.18 ±0.13 1.88 0.30

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

model : bremss + three gaussian (Ca, Cr, Fe)SNR 0519-69.0

χ ２ /dof = 127/89

black ： FIred ： BI

Cr ：Fe ：

FluxFlux [x10[x10-6 -6 ph/cmph/cm22/s]/s]

5.65(5.576 – 5.76)6.489(6.482 – 6.495)

= Fe7.5 (6.5– 8.4)

line center E [keV]

0.4(0.1 – 0.7)9.5 (9.0 – 10.1)

CaCr

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[x10x10-2-2keV]

4 4 7.57.5

Discussion

Upper limit of MMn/MCr 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)

MMn/MCr = 1.057 × ( FMn /FCr ) / ( εMn /εCr ),

the line flux ratiothe ratio of atomic masses

the ratio of specific emissivities per ion

N103B

SNR0519-69.0

(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

LMCSMC

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.

In spectra at 4 keV 〜 ,

In this talk

N103B, SNR 0509-67.5 & SNR 0519-69.0

(Hughes+ 1995)

N103BSNR 0509-67.5 SNR 0519-69.0

ASCA での観測

Mn/Cr flux ratio

flux

ratio

of M

n/Cr

red ： N103B, green : SNR 0519-69.0blue ： 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