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ITEP � petr.baklanov@itep.ru 1/47
A Massive Progenitor ofStrongly Lensed Supernova Refsdal
Petr Baklanov, Sergey Blinnikov, Ken'ichi Nomoto
Kavli IPMU
October 27, 2016
Sjur Refsdal
(Dec 30 1935 � Jan 29 2009)
Sjur Refsdal was a Norwegian
astrophysicist.
In 1964 he �rst proposed usingtime-delayed images from a lensedsupernova to study the expansion of theuniverse.Refsdal, S. (1964). On the Possibility ofDetermining Hubble's Parameter and theMasses of Galaxies from the GravitationalLens E�ect.Monthly Notices of the Royal AstronomicalSociety, 128(4), 307�310.
In 2014 the �rst detected stronglylensed supernova was nicknamed�SN Refsdal� in his honor.
SN Refsdal: discovery
A strongly lensedsupernova was found inthe MACS J1149.6+2223galaxy cluster �eld on 11November 2014
Kelly et al.arxiv:1411.6009
Simulation of Cosmic Lens
The Whirlpool Galaxy Seen Through a Cosmic Lens
Thanks to Dr. Rachael Livermore of the University
of Texas at Austin and Dr. Frank Summers of the
Space Telescope Science Institute.
What if we could take awell-known galaxy and put itbehind one of our FrontierFields galaxy clusters? Whatwould that look like?
SN Refsdal: discovery
A strongly lensedsupernova was found inthe MACS J1149.6+2223galaxy cluster �eld on 11November 2014
Kelly et al.arxiv:1411.6009
Cluster MACSJ1149.5+2233 and SN Refsdal
by NASA, ESA
MACSJ1149.5+2233
z = 0.54 (Grillo, 2015)
DL = 3.14 Gpc
Da = 1.32 Gpc
Members (Treu, 2015):
0.520 < z < 0.570
SN Refsdal is located
at the outer spiral arm
(Rc ∼ 7 kpc)
z = 1.49DL = 11 Gpc
Da = 1.771 Gpc
Cluster MACSJ1149.5+2233 and SN Refsdal
by NASA, ESA by T.Treu (2016)
The lens equation
β = θ − α, Σ(θ) =
∫ρ(θ, z)dz
α(θ,Σ) = ∇θψ(θ,Σ),
[∼
4GM
c2p= 2
Rg
p
]ψ(θ) =
4GDlDls
c2Ds
∫d2θ′Σ(θ′)ln(θ − θ′)
t(θ) =1 + zl
c
DlDs
Dls
1
2(θ − β)2︸ ︷︷ ︸geom
−ψ(θ)︸ ︷︷ ︸grav
, µ =θ
β
dθ
dβ
θ is the observed position of the source, α is the de�ection angle,Σ(θ) is the surfacemass density of the cluster at the position θ, β is the position of the backgroundsource, Dl , Ds and Dls are the angular diameter distances to the lens, the source andfrom the lens to the source.geom: time delay due to the extra path length of the de�ected light ray relative to anunperturbed null geodesicgrav: time delay due to general relativistic time dilation, Shapiro time delay
Models of Lens (Diego, 2016)
β = θ − α(θ,Σ)
θ is the observed position ofthe source, α is thede�ection angle,Σ is thesurface mass density of thecluster at the position θ andβ is the position of thebackground source
The surface mass density is described by the combination oftwo components:(i) A soft (or di�use) component that is parametrized as asuper- position of Gaussians on a grid of constant width(regular grid) or varying width (adaptive grid).(ii) A compact component that accounts for the massassociated with the individual haloes (galaxies) in thecluster. This component is modelled either as Navarro Frenkand White pro�les with a mass proportional to the light ofeach galaxy or adopting directly the light pro�le (in one ofthe IR bands).
Models of Lens (Diego, 2016)
β = θ − α(θ,Σ)
θ is the observed position ofthe source, α is thede�ection angle,Σ is thesurface mass density of thecluster at the position θ andβ is the position of thebackground source
The surface mass density is described by the combination oftwo components:(i) A soft (or di�use) component that is parametrized as asuper- position of Gaussians on a grid of constant width(regular grid) or varying width (adaptive grid).(ii) A compact component that accounts for the massassociated with the individual haloes (galaxies) in thecluster. This component is modelled either as Navarro Frenkand White pro�les with a mass proportional to the light ofeach galaxy or adopting directly the light pro�le (in one ofthe IR bands).
Lens mass
Summary of Models (Table 5)Short name Team Type rms Images
Die-a Diego et al. Free-form 0.78 gold+silGri-g Grillo et al. Simply param 0.26 goldOgu-g Oguri et al. Simply param 0.43 goldSha-g Sharon et al. Simply param 0.16 goldZit-g Zitrin et al. Light-tr-mass 1.3 gold
Magni�cation maps
by Treu+ arxiv:1510.05750
The circlesidentify thepositions of theobserved andpredicted imagesof SN Refsdal andthose of themultiple images ofits host galaxy.
Magni�cation & Time delay
Magni�cation: µ = θβ
dθdβ
Source µ(S1) µ(S2) µ(S3) µ(S4) µ(SX )Diego+(2015) µ(Si )/µ(S1) 1.89± 0.79 0.64± 0.19 0.35± 0.11 0.31± 0.1
Sharon+(2015) 18.5+6.4−4.5 14.47.5
−5.5 20.5+19.1−3.9 11.0+6.9
−4.2
Oguri+(2015) 15.4± 1.6 17.7± 1.9 18.3± 1.9 9.8± 1.4 4.2± 0.3
Grillo+(2016) 13.5+17.4−10.3 12.47.9
−18.8 13.4+19.210.3 5.7+3.7
−8.1 4.8+4.5−5.3
Time delay: t(θ) = 1+zdc
DdDsDds
[12(θ − β)
2 − ψ(θ)]
Source ∆t(S2− S1) ∆t(S3− S1) ∆t(S4− S1) ∆t(SX − S1)Diego+(2015) 17± 19 −4.3± 27 73± 43 262± 55
Sharon+(2015) 2.0+10−6 −5.013
−7 7.0+16−3 237+37
−50
Oguri+(2015) 9.4± 1.1 5.6± 0.5 20.9± 2.0 335.6± 20.7
Grillo+(2016) 10.6+7.6−16.8 4.83.0
−8.0 25.9+34−21.6 361+334
−381
Magni�cation & Time delay
Magni�cation: µ = θβ
dθdβ
Source µ(S1) µ(S2) µ(S3) µ(S4) µ(SX )Diego+(2015) µ(Si )/µ(S1) 1.89± 0.79 0.64± 0.19 0.35± 0.11 0.31± 0.1
Sharon+(2015) 18.5+6.4−4.5 14.47.5
−5.5 20.5+19.1−3.9 11.0+6.9
−4.2
Oguri+(2015) 15.4± 1.6 17.7± 1.9 18.3± 1.9 9.8± 1.4 4.2± 0.3
Grillo+(2016) 13.5+17.4−10.3 12.47.9
−18.8 13.4+19.210.3 5.7+3.7
−8.1 4.8+4.5−5.3
Time delay: t(θ) = 1+zdc
DdDsDds
[12(θ − β)
2 − ψ(θ)]
Source ∆t(S2− S1) ∆t(S3− S1) ∆t(S4− S1) ∆t(SX − S1)Diego+(2015) 17± 19 −4.3± 27 73± 43 262± 55
Sharon+(2015) 2.0+10−6 −5.013
−7 7.0+16−3 237+37
−50
Oguri+(2015) 9.4± 1.1 5.6± 0.5 20.9± 2.0 335.6± 20.7
Grillo+(2016) 10.6+7.6−16.8 4.83.0
−8.0 25.9+34−21.6 361+334
−381
What Is a SN Refsdal?
Q: What was before the supernova explosion? Can we derive the
parameters for the supernova progenitor?
Q: Can we reproduce a supernova in our simulations?
ITEP � petr.baklanov@itep.ru 12/47
Observations: LC of SN Refsdal
The multi-color photometric data were obtained for 400 days
following the discovery.
There is a slow rise to maximum light (over ∼ 150 days).
by Rodney et.al.(2015) arxiv:1512.05734
Observations: the spectra of SN Refsdal
Spectrum of Hα taken −47d
by HST WFC3 Grism
Spectrum of Hα taken 16d
by the VLT
Hα P-Cygni expansion velocity
by Kelly et.al (2015) arxiv:1512.09093
The analysis of observations
Rodney S.A. et.al. arxiv:1512.05734
I The hydrogen lines are shown in SN Refsdal's spectra so it shouldbe SN II.
I SN Refsdal's slow rise to maximum light (over ∼ 150 days) is clearlyinconsistent with the rise times for the most common SN types(e.g., Ia, Ib/c, II-P, and II-L).
I Rodney have compared the SN Refsdal observations with thesenormal SN classes, using a library of 42 templates drawn from theSupernova Analysis software suite � unsuccessfully
I Rodney concludes that the peculiar SN 1987A-like sub-classprovides the best matches to the observed shape of the SN Refsdallight curve.
There is a need for research to be targeted at this supernova.
We have used a progenitor model calculated by Nomoto & Hashimoto(Nomoto, Hashimoto 1988, Phys. Rep., 163, 13)
Model assumptions and implementation
Hydrodynamics, spherical symmetry, self-gravity, Saha-Boltzmann
ion populations (with some NLTE control), no blackbody
assumptions on radiation �eld, arti�cial thermal bomb explosion.
Using STELLA code, developed for supernova light curve
simulations, (Blinnikov et al., 1998, 2006)
I Multigroup time dependent radiation hydrodynamics
I Non-relativistic (O(v/c)), spherically symmetric
I Lagrangean coordinates, staggered mesh
I Full implicit time-dependent predictor-corrector solver for sti�
ODE systems, modi�ed Gear method, �exible dynamic step
and error control
ITEP � petr.baklanov@itep.ru 16/47
The progenitor model: chemical composition
We have used as initial model the evolutionary model of Nomoto &Hashimoto (1988)
Density as a function of the interior massand radius
0.0e+00 5.0e+11 1.0e+12 1.5e+12 2.0e+12 2.5e+12 3.0e+12 3.5e+12
−10
−5
05
R, [cm]
ρ,[g
/cm
3 ]
nommixa
5 10 15
−10
−5
05
M [Msun]
ρ,[g
/cm
3 ]
Abundance distribution as a function ofenclosed mass for the ejecta
M_r [Solar mass]
Xi
2 5 10
1e−05
1e−03
1e−01
HHeCOSi
CaArFeNiNi56
nommixa
SN 1987A: E = 1.7× 1051 ergs, M = 16.6 M�, M56Ni = 0.078 M�
Modeling Light curves of the supernovae:
with SN 1987A
0 50 100 150 200Time [days]
0
2
4
6
8
Magnit
ude
ts= z=0.00 D=5.14e+04 mu=1.0 EbvU lvl14E1nommixaa
B lvl14E1nommixaa
V lvl14E1nommixaa
R lvl14E1nommixaa
I lvl14E1nommixaa
I SN 1987A
R SN 1987A
B SN 1987A
U SN 1987A
V SN 1987A
Good �t!
with SN Refsdal
0 100 200 300 400Time [days]
24
26
28
30M
agnit
ude
ts=-56950 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00F105W lvl14E1nommixaa
F125W lvl14E1nommixaa
F140W lvl14E1nommixaa
F160W lvl14E1nommixaa
F606W lvl14E1nommixaa
F814W lvl14E1nommixaa
F105W obs.
F125W obs.
F140W obs.
F160W obs.
F435W obs.
F814W obs.
A bad agreement with the
observations
The path to the best model
I We have increased the ejectedmass M = 16.6→ 26.6 M�
I We have increased theexplosion energyE = 1.7→ 5× 1051 ergs
I We have increased the mass of56Ni:M56Ni = 0.078→ 0.116 M�
I We've increased the degree of56Ni mixing
I But we've decreased themetallicityZ → Z (SN 1987A)/10
0 100 200 300 400Time [days]
24
26
28
30
Mag
nitu
de
ts=-56950 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00
F105W 14E1nommixaaF125W 14E1nommixaaF140W 14E1nommixaaF160W 14E1nommixaaF435W 14E1nommixaaF606W 14E1nommixaaF814W 14E1nommixaaF105W Sn, RodneyF125W Sn, RodneyF140W Sn, RodneyF160W Sn, RodneyF435W Sn, RodneyF606W Sn, RodneyF814W Sn, Rodney
0 100 200 300 400Time [days]
5
10
15
20
Velo
city
Vel 14E1nommixaaHα, Kelly
0 100 200 300 400Time [days]
24
26
28
30
32
Mag
nitu
de
ts=-56950 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00
F105W lvl14E1nommixaaM26F125W lvl14E1nommixaaM26F140W lvl14E1nommixaaM26F160W lvl14E1nommixaaM26F435W lvl14E1nommixaaM26F606W lvl14E1nommixaaM26F814W lvl14E1nommixaaM26F105W Sn, RodneyF125W Sn, RodneyF140W Sn, RodneyF160W Sn, RodneyF435W Sn, RodneyF606W Sn, RodneyF814W Sn, Rodney
0 100 200 300 400Time [days]
5
10
15
Velo
city
Vel lvl14E1nommixaaM26Hα, Kelly
0 100 200 300 400Time [days]
24
26
28
30
Mag
nitu
de
ts=-56950 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00
F105W lvl14E3nommixaaM26F125W lvl14E3nommixaaM26F140W lvl14E3nommixaaM26F160W lvl14E3nommixaaM26F435W lvl14E3nommixaaM26F606W lvl14E3nommixaaM26F814W lvl14E3nommixaaM26F105W Sn, RodneyF125W Sn, RodneyF140W Sn, RodneyF160W Sn, RodneyF435W Sn, RodneyF606W Sn, RodneyF814W Sn, Rodney
0 100 200 300 400Time [days]
5101520
Velo
city
Vel lvl14E3nommixaaM26Hα, Kelly
0 100 200 300 400Time [days]
24
26
28
30
Mag
nitu
de
ts=-56950 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00
F105W lvl14E3nommixM26Ni012b1p5m3F125W lvl14E3nommixM26Ni012b1p5m3F140W lvl14E3nommixM26Ni012b1p5m3F160W lvl14E3nommixM26Ni012b1p5m3F435W lvl14E3nommixM26Ni012b1p5m3F606W lvl14E3nommixM26Ni012b1p5m3F814W lvl14E3nommixM26Ni012b1p5m3F105W Sn, RodneyF125W Sn, RodneyF140W Sn, RodneyF160W Sn, RodneyF435W Sn, RodneyF814W Sn, Rodney
0 100 200 300 400Time [days]
05
101520
Velo
city
Vel lvl14E3nommixM26Ni012b1p5m3Hα, Kelly
0 100 200 300 400Time [days]
24
26
28
30
Magnit
ude
ts=-56950 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00F105W lvl14E5R50M26Ni2m2b1m3Z01
F125W lvl14E5R50M26Ni2m2b1m3Z01
F140W lvl14E5R50M26Ni2m2b1m3Z01
F160W lvl14E5R50M26Ni2m2b1m3Z01
F606W lvl14E5R50M26Ni2m2b1m3Z01
F814W lvl14E5R50M26Ni2m2b1m3Z01
F105W obs.
F125W obs.
F140W obs.
F160W obs.
F435W obs.
F814W obs.
0 100 200 300 400Time [days]
05
10152025
Velo
city
Vel lvl14E5R50M26Ni2m2b1m3Z01
Hα, Kelly
Best model: lvl14E5R50M26Ni2m2b1m3Z01
0 100 200 300 400Time [days]
24
26
28
30
Magnit
ude
ts=-56950 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00F105W lvl14E5R50M26Ni2m2b1m3Z01
F125W lvl14E5R50M26Ni2m2b1m3Z01
F140W lvl14E5R50M26Ni2m2b1m3Z01
F160W lvl14E5R50M26Ni2m2b1m3Z01
F606W lvl14E5R50M26Ni2m2b1m3Z01
F814W lvl14E5R50M26Ni2m2b1m3Z01
F105W obs.
F125W obs.
F140W obs.
F160W obs.
F435W obs.
F814W obs.
0 100 200 300 400Time [days]
05
10152025
Velo
city
Vel lvl14E5R50M26Ni2m2b1m3Z01
Hα, Kelly
The SN model:
R0 = 49 R�
Mtot = 26 M�
M56Ni = 0.13 M�(mixed)
Z = 0.1 Z(SN 1987A)
E = 5× 1051 ergs
SN 1987A velocities
Best model: lvl14E5R50M26Ni2m2b1m3Z01
0 100 200 300 400Time [days]
24
26
28
30
Magnit
ude
ts=-56950 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00F105W lvl14E5R50M26Ni2m2b1m3Z01
F125W lvl14E5R50M26Ni2m2b1m3Z01
F140W lvl14E5R50M26Ni2m2b1m3Z01
F160W lvl14E5R50M26Ni2m2b1m3Z01
F606W lvl14E5R50M26Ni2m2b1m3Z01
F814W lvl14E5R50M26Ni2m2b1m3Z01
F105W obs.
F125W obs.
F140W obs.
F160W obs.
F435W obs.
F814W obs.
0 100 200 300 400Time [days]
05
10152025
Velo
city
Vel lvl14E5R50M26Ni2m2b1m3Z01
Hα, Kelly
The SN model:
R0 = 49 R�
Mtot = 26 M�
M56Ni = 0.13 M�(mixed)
Z = 0.1 Z(SN 1987A)
E = 5× 1051 ergs
Is this something
unusual?
SN Refsdal is not unusual
SN Refsdal is not unusual
The lens models: Magni�cation & Time delay
Magni�cation
Source µ(S1) µ(S2) µ(S3) µ(S4) µ(SX )Diego+(2015) µ(Si )/µ(S1) 1.89± 0.79 0.64± 0.19 0.35± 0.11 0.31± 0.1
Sharon+(2015) 18.5+6.4−4.5 14.47.5
−5.5 20.5+19.1−3.9 11.0+6.9
−4.2
Oguri+(2015) 15.4± 1.6 17.7± 1.9 18.3± 1.9 9.8± 1.4 4.2± 0.3
Grillo+(2016) 13.5+17.4−10.3 12.47.9
−18.8 13.4+19.210.3 5.7+3.7
−8.1 4.8+4.5−5.3
Time delay
Source ∆t(S2− S1) ∆t(S3− S1) ∆t(S4− S1) ∆t(SX − S1)Diego+(2015) 17± 19 −4.3± 27 73± 43 262± 55
Sharon+(2015) 2.0+10−6 −5.013
−7 7.0+16−3 237+37
−50
Oguri+(2015) 9.4± 1.1 5.6± 0.5 20.9± 2.0 335.6± 20.7
Grillo+(2016) 10.6+7.6−16.8 4.83.0
−8.0 25.9+34−21.6 361+334
−381
SN Refsdal and lens models: Sharon et al., 2015
0 100 200 300 400
24
26
28
30
Obs.
Magnit
ude (
AB
)
S1: sha-a
0 100 200 300 400
24
26
28
30
Obs.
Magnit
ude (
AB
)
S2: sha-a
F105W S2
F125W S2
F140W S2
F160W S2
F606W S2
F814W S2
F105W obs.
F125W obs.
F140W obs.
F160W obs.
F606W obs.
F814W obs.
0 100 200 300 400Time [days]
24
26
28
30
Obs.
Magnit
ude (
AB
)
S3: sha-a
0 100 200 300 400Time [days]
24
26
28
30
Obs.
Magnit
ude (
AB
)
S4: sha-a
Lens model sha-g
Magni�cation:
µS2/µS1 = 0.84+0.18−0.06
µS3/µS1 = 1.68+0.55−0.21
µS4/µS1 = 0.57+0.11−0.04
Time delay:
∆tS2−S1 = 66−5
∆tS3−S1 = −17−5
∆tS4−S1 = 176−5
via Tommaso Treu(arxiv:1510.05750)
SN Refsdal and lens models: Diego et al., 2015
0 100 200 300 400
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S1: die-a
0 100 200 300 400
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S2: die-a
F105W S2F125W S2F140W S2F160W S2
F435W S2F606W S2F814W S2
F105W Sn, RodneyF125W Sn, RodneyF140W Sn, Rodney
F160W Sn, RodneyF606W Sn, RodneyF814W Sn, Rodney
0 100 200 300 400Time [days]
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S3: die-a
0 100 200 300 400Time [days]
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S4: die-a
Lens model die-a:
Magni�cation:
µS2/µS1 = 1.89± 0.79
µS3/µS1 = 0.64± 0.19
µS4/µS1 = 0.35± 0.11
µSX/µS1 = 0.31± 0.1
Time delay:
∆tS2−S1 = −17± 19
∆tS3−S1 = −4± 27
∆tS4−S1 = 74± 43
∆tSX−S1 = 262± 55
via Tommaso Treu(arxiv:1510.05750)
SN Refsdal and lens models: Grillo et al., 2015
0 100 200 300 400
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S1: gri-g
0 100 200 300 400
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S2: gri-g
F105W S2F125W S2F140W S2F160W S2
F435W S2F606W S2F814W S2
F105W obs.F125W obs.F140W obs.
F160W obs.F606W obs.F814W obs.
0 100 200 300 400Time [days]
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S3: gri-g
0 100 200 300 400Time [days]
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S4: gri-g
ts=-56912 z=1.49 D=1.10e+10 mu=15.4 ebv=0.00
Lens model gri-g:
Magni�cation:
µS2/µS1 = 0.92+0.43−0.52
µS3/µS1 = 0.99+0.52−0.33
µS4/µS1 = 0.42+0.19−0.20
µSX/µS1 = 0.36+0.11−0.09
Time delay:
∆tS2−S1 = 10.6+6.2−3.0
∆tS3−S1 = 4.8+3.2−1.8
∆tS4−S1 = 25.9+8.1−4.3
∆tSX−S1 = 361+19−27
via Tommaso Treu(arxiv:1510.05750)
SN Refsdal and lens models: Oguri et al., 2015
0 100 200 300 400
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S1: ogu-g
0 100 200 300 400
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S2: ogu-g
F105W S2F125W S2F140W S2
F160W S2F606W S2F814W S2
F105W obs.F125W obs.F140W obs.
F160W obs.F606W obs.F814W obs.
0 100 200 300 400Time [days]
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S3: ogu-g
0 100 200 300 400Time [days]
24
26
28
30
Obs.
Mag
nitu
de (A
B)
S4: ogu-g
Lens model ogu-g:
Magni�cation:
µS2/µS1 = 1.14± 0.24
µS3/µS1 = 1.22± 0.24
µS4/µS1 = 0.67± 0.17
µSX/µS1 = 0.27± 0.05
Time delay:
∆tS2−S1 = 8.7± 0.7
∆tS3−S1 = 5.1± 0.5
∆tS4−S1 = 18.8± 1.7
∆tSX−S1 = 311± 24
via Masamune Oguri(MNRAS, 2015)
SN Refsdal: the prediction of image SX
MACSJ1149.5+2233: Treu+ arxiv:1510.05750
SN Refsdal: the prediction of image SX
MACSJ1149.5+2233: Treu+ arxiv:1510.05750
SN Refsdal: the prediction of image SX
MACSJ1149.5+2233: Treu+ arxiv:1510.05750
Image SX
SX - S1 Time Delay (Observer-Frame Days)
by Kelly et.al.(2015) arxiv:1512.04654
Light Curves of SX
10 90 190 290 390Time [days]
24
26
28
30
32
Obs.
Mag
nitu
de (A
B)
SX: ogu-a
10 90 190 290 390Time [days]
SX: gri-g
F125W SX F160W SX F125W obs. F160W obs.
10 90 190 290 390Time [days]
SX: sha-a
10 90 190 290 390Time [days]
SX: ogu-g
10 90 190 290 390Time [days]
SX: die-a
Summary of Models (Table 5)Short name Team Type rms Images
Die-a Diego et al. Free-form 0.78 gold+silGri-g Grillo et al. Simply param 0.26 goldOgu-g Oguri et al. Simply param 0.43 goldOgu-a Oguri et al. Simply param 0.31 allSha-g Sharon et al. Simply param 0.16 gold
Conclusions
I Our major result is that SN Refsdal was the massive andhigh-energy version of SN 1987A.
I The progenitor of SN Refsdal was the BSG with next parameters:
R0 = 49 R�
Mtot = 26 M�
M56Ni = 0.13 M�(mixed)
Z = 0.1 Z(SN 1987A)
E = 5× 1051 ergs
I To make a prediction for magni�cations & time delays ofgravitational lens models, to make constraints for the structure ofdark matter halos in galaxies
I To make a prediction of the maximum of SX image
I It is amazing that the progenitors of the closest and the mostdistant SN IIP are the BSG stars.
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