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