Three SN rebrightenings in GRB
afterglow light curves in the context
of the full GRB-SN sample
Felipe Olivares E.
Physics Department
Universidad Andres Bello, Chile
GRB Conference
Kyoto, November 11, 2013

Kyoto on bike! Know more in less time.
●●If you don't want to travel underground
Bike 4 Rent shop: ROJI – YA
Close to Nijojo-mae station
500 Yen per day ; cheapest fare in Kyoto!

GRB fireball model<3

The SN collapsar model

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The multi-wavelength imager GROND@ the 2.2 m MPG teslescope in La Silla5

The multi-wavelength imager GROND@ the 2.2 m MPG teslescope in La Silla

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The multi-wavelength imager GROND@ the 2.2 m MPG teslescope in La Silla

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The Fantastic 3GRBSNzυ
[km/s]

0810072008hw

0.530

--

0.8

1.28

40091127

2009nz0.490

17 000

1.15

14.93

36101219B 2010ma

0.552

--

1.78

5.60

70

k

Eγ,iso[1051 erg]

Epeak
[keV]

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SN bumps in GRB AG light curves

GRB 101219B
Sparre+11

SN 2010ma
9SED for GRB 081007

10JHK Bolometric correction

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Bolometric Light Curves of GRB-SNe
Corrected for :- host extinction (afterglow SED)- UV & NIR contributions

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Bolometric Light Curves of GRB-SNe
Corrected for :- host extinction (afterglow SED)- UV & NIR contributions

Olivares+1213

Corrected for :- host extinction (afterglow SED)- UV & NIR contributions

max NIR correction

Bolometric Light Curves of GRB-SNe

Olivares+1214

The full sample of GRB-SNe
GRB and SN parameters for:- 4 GRB-SNe analysed (addition of 10bh, Olivares E.+12)- 25 objects from the literature (Olivares E.+14, in prep)

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Optical Light Curve Parametersmed( kopt ) = 0.95 ± 0.71
med( Mv ) = -19.27 ± 0.81
kopt KS P-value = 0.97

< sopt > = 0.96 ± 0.24
sopt KS P-value = 0.62

Only 2 objects (7%) are significantly
brighter than SN 98bw

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Masses of the SN explosion< MNi > = 0.41 ± 0.15 M⊙ med( Mej ) = 3.5 ± 4.0 M⊙
Compared to “normal” type Ic SNe (Drout+11 ):MNi KS P-value = 0.03
Mej KS P-value = 0.43
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Properties of SN-associated GRBs

KS Comparisons:T90 vs Swift: P = 0.02
Epeak vs HETE-2: P = 0.03
Eγ,iso vs HETE-2: P = 0.004
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To Be Done & Conclusions●

NIR correction●

Arnett modelling for all GRB-SNe●

Explore correlations between GRB and SN●●

Only 7% of GRB-associated SNe are brighter thanSN 1998bw
But the median luminosity of GRB-SNe is aboutthat of SN 1998bw

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●

●

Short Quiz:
1 How do you pronounce (“su”) in Japanese?
2 Which city is more expensive, Tokyo or Kyoto?
3 Remember the location of the bike4rent shop.
4 What Japanese city has been the capital the longest?
Question: Does anyone have a micro-SD to SD
adapter that I can borrow?

Tokyo Beach
Arigato Gosaimas!

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Spectroscopic GRB-SN associations
GRBSNzυ[km/s]

980425

1998bw

0.009

14 00010.001148030329

2003dh0.169

17 0001.5

5.3468031203

2003lw

0.106

24 000

1.28

0.003

5.3060218

2006aj0.033

18 000

0.67

0.003

41100316D 2010bh

0.059

28 000

0.65

0.142

19.6

kEγ,iso[1051 erg]

Epeak
[keV]

All type Ic SNe
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Spectroscopic GRB-SN associations
GRBSNzυ[km/s]

980425

1998bw

0.00914 000

10.001148030329

2003dh0.169

17 0001.5

5.3468031203

2003lw

0.106

24 000

1.28

0.003

5.3060218

2006aj0.033

18 0000.670.003

41100316D 2010bh

0.059

28 000

0.65

0.142

19.6

kEγ,iso[1051 erg]

Epeak
[keV]

All type Ic SNe
Hjorth+0322

GRB neutrinos++p + γ → Δ → n+ π+

SN neutrinos+-p + e → n + νe

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Bolometric Light-Curve Modelling
Optically thick regime:

L ph = M Ni e− x [ ( ϵ Ni − ϵCo )∫0x A( z ) dz+ ϵCo ∫0x B( z ) dz ]−2zy+ z 2−2zy+2zs+ z 2with A( z )=2z e
and B ( z )=2z ewhere x≡t / τ m , s≡ τ m ( τ Co− τ Ni )/(2 τ Co τ Ni )

κ opt 1/ 2 10 M 3ej 1/ 46 Ek
2For homogeneous density τ m =and υ ph =βc3 Ek
5 M ej( )()Optically thin (nebular) regime:

L neb=[Ni decay]+[Co Decay]+[e + Annihilation ]+[e + Kinetic Energy ]L neb ∝ M Ni
Arnett82, Maeda+03, Tautenberger+06, Valenti+08, Olivares+1224

The MNi-Mej planeGroup 1: high massloss at theend of their lives
only, allowing
the core growth atearlier stages,
which translates intoa larger NiGroup 2: higher
mass loss at earlystages inhibited thecore growth,hence less Ni issynthesised25

GRB-SN energy anti-correlations

Moderate MNi -Epeak
correlation:
z-statisics gives R2 = 0.97
after excluding SNe
2010bh and 2006aj due totheir peculiar high energy
emission.

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GRB-SN energy anti-correlations
Moderate Ek -Eγ,isocorrelation:
z-statisics gives R2 = 0.93
after excluding SN 2006aj
due to their peculiar highenergy emission.

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