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The Type Ia Supernova Rate and Progenitor from Transient Survey
Jun Ernesto Okumura@SN+SNR 16/10/2012
Yutaka Ihara, Mamoru Doi , Tomoki Morokuma, Reynald Pain , Tomonori Totani, Kyle Barbary, Naohiro Takanashi,
Naoki Yasuda, Greg Aldering, Kyle Dawson, Gerson Goldhaber, Isobel Hook, Chris Lidman, Saul Perlmutter,
Anthony Spadafora, Nao Suzuki, Lifan Wang
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Contents
1. IntroductionSN Ia progenitor, SN Ia rate and Delay Time Distribution
2. Rate Calculation from Subaru/XMM-Newton Deep SurveyTransient Surveys (SXDS)
Rate Calculation
Classification
3. Results and FutureRate ResultFuture Survey
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Type Ia Supernova
‣ Thermonuclear Explosion of White Dwarf (WD) which exceeds Chandrasekhar limit
‣ Progenitor system forms binary‣ ~ 1051 erg, MBmax= -19.1mag
‣ Spectrum is basically “Black Body+lines”
‣ Homogeneous LC→Cosmology
C+OWD? Ni
Si, S, Ca
Supectrum
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Type Ia Supernova
‣ Thermonuclear Explosion of White Dwarf (WD) which exceeds Chandrasekhar limit
‣ Progenitor system forms binary‣ ~ 1051 erg, MBmax= -19.1mag
‣ Spectrum is basically “Black Body+lines”
‣ Homogeneous LC→Cosmology
? Ni
Si, S, Ca
Supectrum
Kim97’
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SN Ia Progenitor models
‣ Companion: Main Sequence, Sub-Giant
‣ mass accretion from Roche-love overflow
‣ Recurrent Nova > stable nuclear burning
Single Degenerate (SD)
C+OWD
MSSub-G
Double Degenerate (DD)
C+OWD
C+OWD
‣ Companion: WD
‣ gravitational wave radiation
‣ merge of two WDs > SN Ia1. Gravitational Wave
1. Mass Transfer
2. Exceed ChandrasekharMass (~1.4 Msun)
2. Shrinkage
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Observational Constraints on the progenitor
MSSub-G
C+OWD
1. Dense circumstellar matter (CSM)
No Radio & X-ray detection
(Panagia+06, Chomiuk+12’, Hancock+11’)
see also Dilday+12’, Taddia+12’→CSM
2. Hydrogen from the companion
SN2005am, SN2005cf(Leonard 07’) SN2011fe (Shappee+12’)
CSM
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Observational Constraints on the progenitor
MSSub-G
1. Dense circumstellar matter (CSM)
No Radio & X-ray detection
(Panagia+06, Chomiuk+12’, Hancock+11’)
see also Dilday+12’, Taddia+12’→CSM
2. Hydrogen from the companion
SN2005am, SN2005cf(Leonard 07’) SN2011fe (Shappee+12’)
CSM
Chomiuk+12’
Leonard 07’
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Observational Constraints on the progenitor
MSSub-G
C+OWD
Survivor 3. No detection of SurvivorSN2011fe (Li+11’)Tycho, SN1006 (Ruiz Lapuente+04’, Fuhrman 05’, Ihara+07’, Gonzales-Hernandez+09’, Kerzendorf+09’, Gonzales-Hernandez+12’)
4. Supersoft X-ray Sources (SSS)Di Stefano 10’, Gilfanov&Bogdan 10’but see also Hachisu+10’, Meng&Yang 11’
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Observational Constraints on the progenitor
MSSub-G
C+OWD
Survivor 3. No detection of SurvivorSN2011fe (Li+11’)Tycho, SN1006 (Ruiz Lapuente+04’, Fuhrman 05’, Ihara+07’, Gonzales-Hernandez+09’, Kerzendorf+09’, Gonzales-Hernandez+12’)
4. Supersoft X-ray Sources (SSS)Di Stefano 10’, Gilfanov&Bogdan 10’but see also Hachisu+10’, Meng&Yang 11’
Nomoto+07’
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Observational Constraints on the progenitor
MSSub-G
C+OWD
Survivor 3. No detection of SurvivorSN2011fe (Li+11’)Tycho, SN1006 (Ruiz Lapuente+04’, Fuhrman 05’, Ihara+07’, Gonzales-Hernandez+09’, Kerzendorf+09’, Gonzales-Hernandez+12’)
4. Supersoft X-ray Sources (SSS)Di Stefano 10’, Gilfanov&Bogdan 10’but see also Hachisu+10’, Meng&Yang 11’
Nomoto+07’
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Delay Time Distribution (DTD)
‣ SFH and Delay Time Distribution (DTD)
‣ Delay Time: time duration between the birth of the binary and the explosion as a Supernova
Totani+08’
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Delay Time Distribution (DTD)
‣ SFH and Delay Time Distribution (DTD)
‣ Delay Time: time duration between the birth of the binary and the explosion as a Supernova
Maoz+10’
SN Ia rate is coupled with SFH and DTD
RIa =� t
0�(t�)DTD(t� t�) dt�
Totani+08’
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Delay Time Distribution (DTD)
‣ Population Synthesis Calculation
‣ SD: Lifetime of the secondary DD: WDs sepalation
‣ Theoretical absolute number lies a factor below the observation
0.01
0.1
1
10
0.1 1 10
SN Ia
DTD
[cen
tury
-1 (1
010L K
,0)-1
)]
Delay Time [Gyr]
Meng+08Belczynski+05
Ruiz-Lapuente+98Yungelson+00
0.01
0.1
1
10
0.1 1 10
SN Ia
DTD
[cen
tury
-1 (1
010L K
,0)-1
)]
Delay Time [Gyr]
Greggio+05Yungelson+00
Ruiz-Lapuente+98Belczynski+05SD DD
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Delay Time Distribution (DTD)
‣ Population Synthesis Calculation
‣ SD: Lifetime of the secondary DD: WDs sepalation
‣ Theoretical absolute number lies a factor below the observation
0.01
0.1
1
10
0.1 1 10
SN Ia
DTD
[cen
tury
-1 (1
010L K
,0)-1
)]
Delay Time [Gyr]
Meng+08Belczynski+05
Ruiz-Lapuente+98Yungelson+00
0.01
0.1
1
10
0.1 1 10
SN Ia
DTD
[cen
tury
-1 (1
010L K
,0)-1
)]
Delay Time [Gyr]
Greggio+05Yungelson+00
Ruiz-Lapuente+98Belczynski+05SD DD
tIa ⇠ tGW / a4 a : separation
fsep(a) / a�
fD / fsep(a)da
dtIa/ t�(3��)/4
Ia
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Delay Time Distribution (DTD)
‣ Population Synthesis Calculation
‣ SD: Lifetime of the secondary DD: WDs sepalation
‣ Theoretical absolute number lies a factor below the observation
0.01
0.1
1
10
0.1 1 10
SN Ia
DTD
[cen
tury
-1 (1
010L K
,0)-1
)]
Delay Time [Gyr]
Meng+08Belczynski+05
Ruiz-Lapuente+98Yungelson+00
0.01
0.1
1
10
0.1 1 10
SN Ia
DTD
[cen
tury
-1 (1
010L K
,0)-1
)]
Delay Time [Gyr]
Greggio+05Yungelson+00
Ruiz-Lapuente+98Belczynski+05SD DD
1. SN Ia rate can constrain SFHxDTD2. theoretical DTDs consists with DD model (t-1 DTD)3. Still remains contradiction in the absolute number
tIa ⇠ tGW / a4 a : separation
fsep(a) / a�
fD / fsep(a)da
dtIa/ t�(3��)/4
Ia
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Delay Time Distribution (DTD)
‣ Population Synthesis Calculation
‣ SD: Lifetime of the secondary DD: WDs sepalation
‣ Theoretical absolute number lies a factor below the observation
0.01
0.1
1
10
0.1 1 10
SN Ia
DTD
[cen
tury
-1 (1
010L K
,0)-1
)]
Delay Time [Gyr]
Meng+08Belczynski+05
Ruiz-Lapuente+98Yungelson+00
0.01
0.1
1
10
0.1 1 10
SN Ia
DTD
[cen
tury
-1 (1
010L K
,0)-1
)]
Delay Time [Gyr]
Greggio+05Yungelson+00
Ruiz-Lapuente+98Belczynski+05SD DD
1. SN Ia rate can constrain SFHxDTD2. theoretical DTDs consists with DD model (t-1 DTD)3. Still remains contradiction in the absolute number
Ruiter+11’Mennekens+10’
tIa ⇠ tGW / a4 a : separation
fsep(a) / a�
fD / fsep(a)da
dtIa/ t�(3��)/4
Ia
Mennekens+10’
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Why SN Ia rate?
‣ SN Ia is crucial tool for astronomy
1. Ia cosmology: homogeneous LCs
2. Chemical Evolution: ~0.6Msun Fe per event
3. Cosmic/Galactic Star Formation History (SFH)
‣ ...but we don’t have clear comprehension about explosion mechanism, progenitor, environment
‣ SN Ia rates at high-z are not clear yet!
Numerical Simulation Statistical Constraint
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Why SN Ia rate?
‣ SN Ia is crucial tool for astronomy
1. Ia cosmology: homogeneous LCs
2. Chemical Evolution: ~0.6Msun Fe per event
3. Cosmic/Galactic Star Formation History (SFH)
‣ ...but we don’t have clear comprehension about explosion mechanism, progenitor, environment
‣ SN Ia rates at high-z are not clear yet!
Numerical Simulation Statistical Constraint
10-5
10-4
0 0.5 1 1.5 2
Ia R
ate
[yr-1
Mpc
-3]
redshift
Li+’11Dahlen+’08
Neil+’06Dilday+’11Graur+’11
Barbary+’12Perrett+’12
DTD index -0.5DTD index -1.0DTD index -1.5DTD index -2.0
RIa =� t
0�(t�)DTD(t� t�) dt�
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Contents
1. IntroductionSN Ia progenitor, SN Ia rate and Delay Time Distribution
2. Rate Calculation from Subaru/XMM-Newton Deep SurveyTransient Surveys (SXDS)
Rate Calculation
Classification
3. Results and FutureRate ResultFuture Survey
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Transient Studies
SpectrumLight Curves
ColorsBayesian analysis
classification
production ratehost galaxyprogenitor
(galaxy evolution)
transient sampleTransient Survey
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Subaru/XMM-Newton Deep Survey (SXDS)
‣ Wide (~1deg2), Deep (mlim~27mag)- Optical(Subaru / Sprime-Cam)B, V, Rc, i’, z’
- NIR(UKIDSS Survey)J, H, K
- IR(Spitzer / IRAC)3.6μm, 4.5μm
- X-ray (XMM-Newton) 0.5-2.0, 2.0-10.0keV
NAOJ
‣ 5 fields (SXDS-C, N, S, E, W)
‣ 1~10 day cadence (5-7 epochs)
‣ 1040 Transients (Morokuma+08’)
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Control Time
‣ Control Time = “effective visibility time” for observer
60 days
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Control Time
‣ Control Time = “effective visibility time” for observer
‣ Montecarlo Simulation
<CT> = 57.54 days
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Control Time & Rate Calculation
‣ Ia: spectral template (Hsiao+07’) + Nearby SDSS Ia sample
‣ CC: 12 individual template
Rate Calculation
Expected SN Ia number in redshift bin [z1, z2]
if r(z)=const. during [z1, z2]
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SN candidate Selection
1.AGN-like,2. SN occured after
Transient Search370 remained
faint objects140 remained
Remove
SXDS Transient1040
Remove
24
25
26
27
28
0 50 100 150 200 250 300 350 400
mi’ [
mag
]
MJD - 52547 [day]
23.5
24
24.5
25
25.5
26 0 200 400 600 800 1000 1200
mi’ [
mag
]
MJD - 52547 [day]
25
25.5
26
26.5
27
27.5
28
28.5 0 50 100 150 200 250 300 350 400
mi’ [
mag
]
MJD - 52547 [day]
AGN-like faint
SN candidate
No variability after 2003 1. at last two points brighter than 26mag2. at least two points brighter than 5σbf
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lightcurve fitting
‣ Ia: spectral template (Hsiao+07’)
redshift, stretch [0.7~1.2], MB [-17.5~-20.0], day at Max
‣ CC: 12 individual LC template
redshift, MB [-17.5~-20.0], day at Max
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lightcurve fitting
‣ Ia: spectral template (Hsiao+07’)
redshift, stretch [0.7~1.2], MB [-17.5~-20.0], day at Max
‣ CC: 12 individual LC template
redshift, MB [-17.5~-20.0], day at Max
Ptype(z) / PDF (z)⇥ exp (��2LC(z)
2
)
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SN template fittingIa other type
~42 SN Ia detected!
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Possible Contamination?
Rate Calculation
the rate derivation in redshift bin [z1, z2]
1. PIa(z) : completeness of the fitting 2. 1-PII(z) : misclassification as CC SN
PIa(z): completeness
1-PII(z): misclassification ratioNest(z) = NIa(z)PIa(z) +NII(z)(1� PII(z))
NII(z) = 0.55⇥ (1 + z)3.6CTII(z)V (z)
nearby SN II rate (Botticella+08’)cosmic star formation rate (Hopkins&Beacom 06’)
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SN Ia rate
‣ SN Ia rate rising up to z~1.4
‣ most of high-z results were derived from one epoch obs., which SXDS result have LC confirmation.
10-5
10-4
0 0.5 1 1.5 2
Ia R
ate
[yr-1
Mpc
-3]
redshift
This WorkLi+’11
Dahlen+’08Neil+’06
Dilday+’11Graur+’11
Barbary+’12Perrett+’12
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Hyper Suprime-Cam
FoV: 1.77deg2 (7 times larger than SC, 5 times smaller than LSST)0.17”/pix (typical seeing @MK ~0.7”)6 broad-band filters(ugrizy)+several narrow-band filter
ACS
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Hyper Suprime-Cam
FoV: 1.77deg2 (7 times larger than SC, 5 times smaller than LSST)0.17”/pix (typical seeing @MK ~0.7”)6 broad-band filters(ugrizy)+several narrow-band filter
ACS
1.5deg
HSC
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Hyper Suprime-Cam
FoV: 1.77deg2 (7 times larger than SC, 5 times smaller than LSST)0.17”/pix (typical seeing @MK ~0.7”)6 broad-band filters(ugrizy)+several narrow-band filter
ACS
1.5deg
HSC
LSST
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Hyper Suprime-Cam
FoV: 1.77deg2 (7 times larger than SC, 5 times smaller than LSST)0.17”/pix (typical seeing @MK ~0.7”)6 broad-band filters(ugrizy)+several narrow-band filter
ACS
1.5deg
HSC
LSST
10-5
10-4
10-3
0 0.5 1 1.5 2
Ia R
ate
[yr-1
Mpc
-3]
redshift
HSCOkumura+12’
Li+’11Dahlen+’08
Neil+’06Dilday+’11Graur+’11
Barbary+’12Perrett+’12
DTD index -0.5DTD index -1.0DTD index -1.5DTD index -2.0
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Summary
‣ The importance of statistical (rate) studies of SNe are growing
‣ Subaru is one of the promising candidate for these studies
‣ Ia rate from SXDS has been derived
‣ Ia rate is consistent with other works and showing expectation to reduce the error in the near future (HSC-Survey!)
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Supplemental Slides