2. Nuclearimagingspectroscopyw/ETCC · 2016. 6. 20. · Detection significance [s] 3 4...
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Detection significance [s] 3 4 5 Conservative (SD, DD) [Mpc] 70, 55 60, 48 55, 45 Optimistic (SD, DD) [Mpc] 110, 85 95, 75 85, 65 [email protected] - u.ac.jp 14 th International Symposium on Nuclei in the COSMOS, Niigata, Japan, June 19-24, 2016 Yoshitaka Mizumura 1,2 , Toru Tanimori 2 , Atsushi Takada 2 , on behalf of SMILE group 3 1 Unit of Synergetic Studies for Space, Kyoto University, Kyoto, Japan 2 Division of Physics and Astronomy, Kyoto University, Kyoto, Japan 3 http://www-cr.scphys.kyoto-u.ac.jp/research/MeV-gamma/wiki/wiki.cgi All-sky nuclear imaging spectroscopy is a promising tool for systematic study of supernova (SN) explosions. Especially, progenitor scenarios of type Ia SNe are not well-understood yet. Here, we report an nuclear imaging telescope, Electron-Tracking Compton Camera (ETCC), and its expected performance with satellite-based all-sky imaging, which enable us to observe nuclear lines from SN Ia at a distance beyond 40 Mpc (~several SNe/years). 100 days(@40-140 d), 0.7-4.0 MeV 20 40 60 Mpc Distance distri. in 5 yrs 56 Ni gen Inclination angle 20 40 60 ±20% ±30% 20 40 60 20 Mpc 40 Mpc 40 Mpc 20 Mpc 100 keV 4 MeV 2 MeV 200 keV 500 keV 812 1561 keV 480 270 158 56 Ni 56 Co 847 1038 1238 1771 2038 2598 3253 keV 750 0.7 MeV 1 MeV SD DD 56 Ni (t 1/2 = 6.1 d) → 56 Co (77.2 d) → 56 Fe SD DD IR-Opt.-UV Uncertainty from inclination angle of the orbit SD DD 50 keV—4 MeV Obvious diff. b/w SD and DD ©David A. Hardy/ AstroArt Mass accretion from companion star ( SD ) ©NASA Violent merger of white dwarfs ( DD ) Which scenario is? 1. Progenitor scenarios of Ia SNe A. Summa, et al., A&A 554, A67 (2013) 80 0 Nuclear gamma-ray is a powerful tool to distinguish SD and DD. R. Diehl, et al., Science 345, 1162 (2014) E. Churazov, et al., Nature 406, 512 (2014) SN2014J: SN [email protected] (Very rare: ~1/40 SN/yr) SPI IBIS 847 keV 1238 keV 1038 keV INTEGRAL successfully observed 56 Ni and 56 Co lines, but it is difficult to resolve the puzzle of SD vs. DD True nuclear imaging spectroscopy and systematic study are required!! MeV g MeV g COMPTEL type ETCC type COMPTEL type ETCC obs. improvement Instruments on satellite: 4 x (50 cm) 3 ETCC Effective Area: 240 cm 2 @1 MeV PSF: 2 o @1 MeV ΔE/E: 5%@662 keV Field of View: 2p sr Effective Exposure: 33% Assumed B.G. flux: 2 times of reported flux e- Energy: Ke g Energy: Eg Eg Ke Ke Eg c m e = 2 1 cos Details in [23-PS2.78] T. Tanimori, et al., ApJ 810, 28 (2015) 3. Detectable nuclear gamma-ray lines Please check also SMILE balloon experiment series. Sub-MeV gamma-ray Imaging Loaded-on-balloon Experiment Expected performance SN Ia rate(<60 Mpc): ~2x10 -5 [yr -1 Mpc -3 ] Dist. [Mpc] SN rate [yr -1 ] 5 yrs [SNe] 15 0.28 1.4 20 0.67 3.4 40 5.4 27 60 18 90 D. Maoz, and F. Mannucci, Publ. Astron. Soc. Australia 29, 447 (2013) 56 Ni gen. Inclination angle ±20% ±30% Flux uncertainty: 56 Ni gen. 20% (SD & DD) Inclination 30% (only DD) 4. Averaged lightcurve of type Ia SNe SD 3.5 Mpc 20-40 Mpc (23 SNe) 40-60 Mpc (63 SNe) 10 days 20-60 Mpc (86 SNe) SD DD Generated # ( SD, DD) SD ratio [%] Best fitted SD ratio[%] 0, 86 0.0 4 ± 11 20, 66 23.3 23 ± 3 42, 44 48.8 44 ± 3 64, 22 74.4 76 ± 3 86, 0 100 90 ± 3 Can we measure co-existence ratio of SD and DD? A puzzle of SN Ia, SD vs. DD, can be resolved 5. Detection limits & prospects Obs. in 50-100 d BG subtracted BG subtracted BG subtracted BG subtracted DD 3.5 Mpc 56 Co lines will be observed from ~several SNe/years T. Tanimori, et al., ApJ 810, 28 (2015) Distance [Mpc] # [SNe] Averaged dist. [Mpc] 0-20 4 14.0 20-40 23 31.9 40-60 63 51.3 0-60 90 44.7 Emulation of type Ia SNe SD DD SD DD Random numbers Expectation of averaged lightcurves or Co-existence !? Yes!! we can measure the ratio w/ 20-30% err. If we achieve observations of Ia SNe up to 100 Mpc, >400 SNe/5yrs are expected. Nuclear imaging spectroscopy with ETCC enables us to try systematic observational studies of type Ia SNe, and it will open a new era of nuclear physics in the cosmos. SD DD Conservative model: 2xBG, All-sky survey Optimistic model: 1xBG, Pointing mode days 2. Nuclear imaging spectroscopy w/ ETCC Mpc 1 mCrab sensitivity
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Detection significance [s] 3 4 5
Conservative (SD, DD) [Mpc] 70, 55 60, 48 55, 45
Optimistic (SD, DD) [Mpc] 110, 85 95, 75 85, 65
[email protected] International Symposium on Nuclei in the COSMOS, Niigata, Japan, June 19-24, 2016
Yoshitaka Mizumura1,2, Toru Tanimori2, Atsushi Takada2, on behalf of SMILE group3
1 Unit of Synergetic Studies for Space, Kyoto University, Kyoto, Japan2 Division of Physics and Astronomy, Kyoto University, Kyoto, Japan3 http://www-cr.scphys.kyoto-u.ac.jp/research/MeV-gamma/wiki/wiki.cgi
All-sky nuclear imaging spectroscopy is a promising tool for systematic study of supernova (SN) explosions. Especially, progenitor scenarios of type Ia SNe are not well-understood yet. Here, we report an nuclear imaging telescope, Electron-Tracking Compton Camera (ETCC), and its expected performance with satellite-based all-sky imaging, which enable us to observe nuclear lines from SN Ia at a distance beyond 40 Mpc (~several SNe/years).
100 days(@40-140 d), 0.7-4.0 MeV
20 40 60 Mpc
Distance distri.
in 5 yrs
56N
i ge
nIn
clin
atio
n an
gle
20 40 60
±20%
±30%
20 40 60
20 Mpc 40 Mpc 40 Mpc20 Mpc
100keV
4MeV
2MeV
200keV
500keV
812
1561keV
480270
158
56Ni
56Co 847
1038
1238 1771
2038
2598
3253keV
750
0.7 MeV
1MeV
SD
DD
56Ni (t1/2 = 6.1 d) → 56Co (77.2 d) → 56Fe
SD
DDIR-Opt.-UV
Uncertainty from inclination
angle of the orbit
SD DD
50 keV—4 MeV
Obvious diff.b/w SD and DD
©David A. Hardy/AstroArt
Mass accretion from companion star (SD)
©NASA
Violent merger of white dwarfs (DD)Which
scenario is?
1. Progenitor scenarios of Ia SNe
A. Summa, et al., A&A 554, A67 (2013)
800
Nuclear gamma-ray is a powerful tool to distinguish SD and DD.
R. Diehl, et al., Science 345, 1162 (2014)E. Churazov, et al., Nature 406, 512 (2014)
SN2014J: SN [email protected] (Very rare: ~1/40 SN/yr)
SPIIBIS
847keV 1238
keV1038keV
INTEGRAL successfully observed 56Ni and 56Co lines,but it is difficult to resolve
the puzzle of SD vs. DD
True nuclear imaging spectroscopy and systematic
study are required!!
MeV g
MeV g
COMPTEL type ETCC type
COMPTEL type ETCC obs.
improvement
Instruments on satellite:4 x (50 cm)3 ETCC
Effective Area:240 cm2@1 MeV
PSF: 2o @1 MeV
ΔE/E: 5%@662 keV
Field of View: 2p srEffective Exposure: 33%Assumed B.G. flux:2 times of reported flux
e- Energy: Keg Energy: Eg
Eg
Ke
KeEg
cme
=
2
1cos
Details in [23-PS2.78]T. Tanimori, et al., ApJ 810, 28 (2015)
3. Detectable nuclear gamma-ray lines
Please check also SMILE balloon experiment series.Sub-MeV gamma-ray Imaging Loaded-on-balloon Experiment
Expected performance
SN Ia rate(<60 Mpc): ~2x10-5 [yr-1 Mpc-3] Dist.[Mpc]
SN rate[yr-1]
5 yrs[SNe]
15 0.28 1.420 0.67 3.440 5.4 2760 18 90
D. Maoz, and F. Mannucci,Publ. Astron. Soc. Australia 29, 447 (2013)
56Ni gen.
Incl
inat
ion
angl
e
±20%
±3
0%
Flux uncertainty:56Ni gen. 20% (SD & DD)
Inclination 30% (only DD)
4. Averaged lightcurve of type Ia SNe
SD
3.5 Mpc
20-40 Mpc (23 SNe) 40-60 Mpc (63 SNe)10
days
20-60 Mpc (86 SNe)
SD
DD
Generated #(SD, DD)
SD ratio[%]
Best fittedSD ratio[%]
0, 86 0.0 4 ± 1120, 66 23.3 23 ± 342, 44 48.8 44 ± 364, 22 74.4 76 ± 386, 0 100 90 ± 3
Can we measure co-existence ratio of SD and DD?
A puzzle of SN Ia, SD vs. DD,
can be resolved
5. Detection limits & prospects
Obs. in 50-100 d
BG subtracted BG subtracted BG subtracted BG subtracted
DD
3.5 Mpc
56Co lines will be observed from ~several SNe/years
T. Tanimori, et al., ApJ 810, 28 (2015)
Distance[Mpc]
#[SNe]
Averageddist.[Mpc]
0-20 4 14.020-40 23 31.940-60 63 51.30-60 90 44.7
Emulation of type Ia SNe
SDDD
SDDD
Random numbers
Expectation of averaged lightcurves
orCo-existence
!?
Yes!! we can measure the ratio w/ 20-30% err.
If we achieve observations of Ia SNeup to 100 Mpc, >400 SNe/5yrs are expected.
Nuclear imaging spectroscopy with ETCC enables us to try systematic observational studies of type Ia SNe, andit will open a new era of nuclear physics in the cosmos.
SD
DD
Conservative model: 2xBG, All-sky surveyOptimistic model: 1xBG, Pointing mode
days
2. Nuclear imaging spectroscopy w/ ETCC
Mpc
1 mCrab sensitivity
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