A Massive Progenitor of Strongly Lensed Supernova Refsdal · SN Refsdal: discovery A strongly...

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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).

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

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?


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


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





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





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







F105W obs.

F125W obs.

F140W obs.

F160W obs.

F435W obs.

F814W obs.

0 100 200 300 400Time [days]

05

10152025

Velo

city


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







F105W obs.

F125W obs.

F140W obs.

F160W obs.

F435W obs.

F814W obs.

0 100 200 300 400Time [days]

05

10152025

Velo

city


Hα, Kelly

The SN model:

R0 = 49 R�

Mtot = 26 M�


Z = 0.1 Z(SN 1987A)

E = 5× 1051 ergs

Is this something

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


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.


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


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



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

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�


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.

A Massive Progenitor of Strongly Lensed Supernova Refsdal · SN Refsdal: discovery A strongly...

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