Supernovae shed light on GRBs	  	  	  	  	  	  	  M.	  Della	  Valle	  	  (Capodimonte	  Obs.	  INAF-­‐Napoli	  &	  ICRANet-­‐Pescara)	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  	  Summary• Supernova Taxonomy• GRB-SN properties• GRB and SN rates• Conclusions

1. Supernova taxonomy
thermonuclear < 8M¤

core-collapse > 8M¤

HIII
Si

IIL IIP IInIa

HeIb

brightfaintvery
brightIc à High KE SNe-Ic à Hypernovaeà GRB-SNe

2. SNe & GRBs at z < 0.2GRBSNzRef.

GRB	  980425	  SN	  1998bw	  0.0085	  Galama	  et	  al.	  1998	  GRB	  060218	  SN	  2006aj	  0.033	  Campana	  et	  al.	  2006	  Pian	  et	  al.	  2006	  GRB	  080109	  SN	  2008D	  0.007	  Soderberg	  et	  al.	  2008	  Mazzali	  et	  al.	  2008	  GRB	  100316D	  SN	  2010bh	  0.06	  Bufano	  et	  al.	  2012	  Chornock	  et	  al.	  2010	  Cano	  et	  al.	  2011	  MarguK	  et	  al.	  2013	  GRB	  030323	  SN	  2003dh	  0.16	  Hjorth	  et	  al.	  2003	  Stanek	  et	  al.	  2003	  GRB	  031203	  SN	  2003lw	  0.11	  Malesani	  et	  al.	  2004	  GRB	  130702A	  SN	  2013dx	  0.15	  4D’Elia	  et	  al.	  2014	  Properties of GRB-SNe (broad-lined SNe-Ic)

Lack of H and He in the ejecta:
SNe-Ic(b)Very broad features: large
expansion velocity (0.1c)
Kinetic energy (non-relativisticejecta) ~ 1052 erg ≳ 10 larger than
Usual CC-SNe
Range of luminosity: in some caselarge 56Ni mass ( ~ 0.5±0.2 M)
Explosions are aspherical (profilesof nebular lines O vs. Fe andPolarization)

Progenitor Mass ?

6Modeling lightcurves and spectra
1998bw
40 M

2003dh2003lw
2006aj2008D
35-40 M 40-50 M 20-25 M 20-30 M

Maeda et al.
2006

Iwamoto et al. 1998

Mazzali et al. Mazzali et al. Mazzali et al. Tanaka et al.
2003
2006
2006
2008

Maeda et al. 2006

Bufano et al. 2012

Distant GRB/SNe ?

up to z ~ 1
GRB021211

GRB 990712

Della Valle et al. 2003

Bjornsson et al. 2001

Sahu et al. 2000
GRB 050525A

Lazzati et al. 2005

Della Valle et al. 2006

Garnavich et al. 2003

GRB census > 0.2
GRBGRB	  021202	  GRB	  050525A	  GRB	  101219B	  GRB	  060729	  GRB	  090618	  GRB	  081007	  SNSN	  2002lt	  SN	  2005nc	  SN	  2010ma	  SN	  	  no	  name	  	  SN	  	  no	  name	  SN	  2008hw	  z
1.002	  0.606	  0.55	  0.54	  0.54	  0.53	  Ref.

GRB	  091127	  SN	  2009nz	  0.49	  Cobb	  et	  al.	  2010	  Berger	  et	  al.	  2011	  GRB120714B	   SN	  2012eb	  GRB	  130427A	   SN	  2013cq	  0.40	  0.34	  Klose	  et	  al.	  2012	  GRB	  120422A	   SN	  2012bz	  0.28	  Melandri	  et	  al.	  2012	  Della	  Valle	  et	  al.	  2003	  Della	  Valle	  et	  al.	  2006	  Sparre	  et	  al.	  2011	  Cano	  et	  al.	  2011	  Cano	  et	  al.	  2011	  Della	  Valle	  et	  al.	  2008	  Zhi-­‐ping	  et	  al.	  2008	  Melandri	  et	  al.	  2014	  Xu	  et	  al.	  2013	  Berger et al. 2011
SN 2009nz @ z=0.49

Zhi-Ping et al. 2013
SN 2008hw @ z=0.53

DV et al. 2013
SN 2002lt @ z=1

Progenitor Mass ?

12

Fruchter et al. 2006

Kelly et al. 2008 find that local SNe-Ic erupt in thebrightest regions of their hosts (like GRBs, see Fruchter etal. 2006)

1998bw
40 M

2003dh2003lw
2006aj2008D
35-40 M 40-50 M 20-25 M 20-30 M

Maeda et al.
2006

Mazzali et al. Mazzali et al. Mazzali et al. Tanaka et al.
20032006
2006
2008

Long-GRBs have ~ 40 M Raskin et al. 2008

3. Ingredients for a “healthy”
SN and GRB rates

Cooking GRB and SN rates

Main Courses• Fraction of SNe-Ib/c which
produces (long)GRBs

Main Courses• Fraction of SNe-Ib/c which
produces (long)GRBs• HL-GRB vs LL-GRB rates

Main Courses• Fraction of SNe-Ib/c which
produces (long)GRBs• HL-GRB vs LL-GRB rates• Fraction of SNe-Ib/c which produces
HNe

What is the rate of SNe-Ib/c ?
Asiago Survey (Cappellaro et al. 1999)

Rate for Ib/c: 0.152 ± 0.064 SNu

Guetta & DV 2007

1.8 x 104 SNe-Ibc Gpc-3 yr-1 à 1.1x 104 up to 2.6x 104

22

What is the rate of SNe-Ib/c ?
Lick Survey (Li et al. 2011)

Rate for Ib/c: 2.6 x 104 SNe-Ibc Gpc-3 yr-1
2.2 x 104 à 3 x 104 SNe-Ibc Gpc-3 yr-123+
2.4±0.2 x 104 SNe-Ibc Gpc-3yr-1

24

What is the rate of (long) GRBs ?
GRB Gpc-3 yr-1
1.5 Schmidt 1999
0.15 Schmidt 2001
0.5 Guetta et al. 2005
1.1 Guetta & DV 2007
1.1 Liang et al. 2007
> 0.5 Pelangeon et al. 2008
1.3 Wanderman and Piran 2010

Guetta et al. 201125

What is the local rate of (long) GRBs ?

0.7 GRB Gpc-3 yr-1

(0.5-0.8)26What is the fraction of SNe-Ib/c which
produces (long)GRBs ?
Rate for Ibc: 2.4 x 104 SNe-Ibc Gpc-3 yr-1
GRB rate: 0.7 GRB Gpc-3 yr-1

27

What is the fraction of SNe-Ib/c which
produces (long)GRBs ?
Rate for Ibc: 2.4 x 104 SNe-Ibc Gpc-3 yr-1
GRB rate: 0.7 GRB Gpc-3 yr-1
<fb-1> ~500
<fb-1> ~75<fb-1> < 10<fb-1> ~ 1(Frail et al. 2001)(ϑ ~ 4°)(Guetta, Piran & Waxman 2004)(ϑ ~ 9°)(Guetta & DellaValle 2007 )(ϑ > 25°) for sub-lum GRBs

(Ruffini et al. 2006)(ϑ ~ 4 π)

28

To Beaming, or not to Beaming
Racusin et al. 2008

GRB 080319B

In some cases there is not evidence for beaming, i.e. an
achromatic break was not detected (see Campana et al. 2007) .

(2013)1° < ϑ < 30°ϑpeak ~ 4°

What is the fraction of SNe-Ib/c which
produces (long)GRBs ?
Rate for Ibc: 2.4 x 104 SNe-Ibc Gpc-3 yr-1
GRB rate: 0.7 GRB Gpc-3 yr-1
<fb-1> ~500
<fb-1> ~75<fb-1> < 10<fb-1> ~ 1(Frail et al. 2001)(ϑ ~ 4°)(Guetta, Piran & Waxman 2004)(ϑ ~ 9°)(Guetta & DellaValle 2007 )(ϑ > 25°) for sub-lum GRBs

(Ruffini et al. 2006)(ϑ ~ 4 π)

GRB/SNe-Ibc: 1.5%-0.003%
32

Soderberg et al. 2006
62 SNe-Ibc
Bietenholz al. 201159 SNe-Ibc

GRB/SNe-Ibc <10%33

GRB/SNe-Ibc ~ 1/146
GRB/SNe-Ibc ~ 0.7%
< 5% at 99%

GRB/SNe-Ibc: 1.5%-0.003%

HL-GRBs

Fermi

LL-GRBs

SwiftSNe & GRBs at z < 0.1
GRB

SNz

Eiso (erg)

GRB 980425

SN 1998bw

0.0085~ 1048

GRB 060218

SN 2006aj

0.033~ 1050

GRB 080109

SN 2008D

0.007~ 1046GRB 100316D SN 2010bh

0.06~ 1050

LL-GRBs sample a volume 106 smaller àRate: up to x 103 Gpc-3 yr-1

(Della Valle 2005, Pian et al. 2006, Cobb et al. 2006, Soderberg et al. 2006,
Liang et al. 2006, Guetta & Della Valle 2007, Amati et al. 2007)36

SNe & GRBs at z < 0.1
GRB

SNz

D max

Sky Cov.

Δt (yr)GRB
980425

SN
1998bw

0.0085170 Mpc

0.08

7

GRB060218

SN 2006aj

0.033

160 Mpc

0.17

9GRB080109

SN 2008D0.007

200 Mpc

0.179GRB100316D

SN 2010bh

0.06

268 Mpc

0.17937

LL-GRBs Rate
LL-GRBs counts (beppo-Sax) ~ 0.2 – 3.3 (1σ)
SkyCov +Vmax + Δt à “observed” ~ 90 Gpc-3 yr-1 (18 up to300)
LL-GRBs counts (Swift) ~ 1.3 – 6 (1σ) à SkyCov + Vmax +Δtà “observed” ~ 65 Gpc-3 yr-1 (48 up to 111)
LL-GRBs “observed” ~ 71 GRBs Gpc-3 yr-1 (51 up to 104)

38

LL-GRBs Rate
LL-GRBs counts (beppo-Sax) ~ 0.2 – 3.3 (1σ)
SkyCov +Vmax + Δt à “observed” ~ 90 Gpc-3 yr-1 (18 up to300)
LL-GRBs counts (Swift) ~ 1.3 – 6 (1σ) à SkyCov + Vmax +Δtà “observed” ~ 65 Gpc-3 yr-1 (48 up to 111)
LL-GRBs “observed” ~ 71 GRBs Gpc-3 yr-1 (51 up to 104)
<fb-1>LL-GRBs~ 1-2 GRB 060218 θ>80o (Soderberg et al. 2006)< 7 GRB 031203 θ>30o (Malesani 2006)< 10 statistic
θ>25o (Guetta & Della Valle 2007)39

LL vs. HL Rates
LL-GRBs ~ 71 x (1 ÷ 10) ~ 70 ÷ 700 LL-GRBs Gpc-3 yr-1

<fb-1>HL-GRBs ~ 75 ÷ 500

HL-GRBs ~ 0.7 x <fb-1> ~ 50 ÷ 350 Gpc-3 yr-1

LL-GRB/HL-GRB < 1540

GRB	  130427A+SN	  2013cq	  	  Xu et al. 2013
Melandri et al. 2014 41

q Testing the GRB-SN paradigm with the brightest “close” event;GRB 130427A T90=162s
Ø Recent detection of the very energetic (Eiso = 1054 erg)
“neraby” (z = 0.34) GRB030427A
Ø Unique occasion to test the GRB-SN connection for“cosmological” GRBs

Melandri et al. 2014

?(@&/-+ABCD!"#$%&'()&*+,-./+&0123!

4567859&:+;&!".&<5=>&!

43!11&56E7&41961F&1%&56,&D9'#G&/-+C,AA+/

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PG#&$%&#F#?@8#9*:0#,#2#F#G?=7GX#,#N#F#?=?W#O#?8%)Q>.0"RJ"-4445

BHs hyperaccretion
spindown of Kerr BH
NSàBHEk

NSs spindown/magnetar
Failed Jet
SN s-bCampana
Kawanaka
et al.
et al.
2006,
2013;
Soderbergvan Putten
et etal. al.
2008,
2011,Mazzali
Ruedaetetal.
al.2008,
2012; Lazzati
andetREFERENCES
al. 2012, Fan etTHEREIN
al. 2013 and REFERENCES THEREIN
46

Mazzali et al. 2013
See also Nomoto et al.
2005; Smartt et al. 2008;
Zampieri et al. 2003

What is the fraction of SNe-Ib/c which
produces HNe?

48

How	  to	  compute	  rates	  1.

The observing log:
epoch, limiting
magnitude
2. Target apparent
light curve: SNtype, target distance
3. Galaxy sample:
distance, type,inclination …….

observinglog
JAN FEB MAR APR MAY JUN JUL AGO SEP NOVDECSNi ,VSNB

SN
BVGV

B to V
K-correction

galacticextinctionm (t ) = M (t0 ) + µ ( zi ) + K (t0 ) + At0 = t /(1+z)

SN light curvein B absolutemagnitude

galaxydistancemodulus

SNi

CTi = Li ∫τ (m)ε (m) d m
galaxyluminosity

time SNstays atm-m+dm

detection
efficiency

r SN = (1 + zi )N SNNSNCT∑i i

SNe-Ib=81
SNe-Ic=132
SNe-Ibc=50
HNe=18

HNe/SNe-Ibc: ~ 7%

HL-GRBs/HNe: 20%-3%

A simplified Scheme for a GRB-SN event-an almost isotropic
component carrying mostenergy 1052 erg and mass(~5-10M¤)-highly collimatedcomponent 4°-10° for
HL-GRBs containing atiny fraction of themass (10 -4/-5 M)
moving at Γ ~ x 102-3

HL-GRBs/HNe: 20%-3%

30,000 km/s

line of sight
HN

line of sight
HN + GRB

SNe-Ib=81
SNe-Ic=132
SNe-Ibc=50
HNe=18

LL-GRBs/HNe ≥ 40%

4. Conclusions
GRBs are very rare phenomena (compared to SN
explosions)
GRB/SNe-Ibc: 0.003%-1.5%
Ibc/CC ~ 0.30
GRB/CC-SN ~ 10-5 ÷ 5 x 10-3
N(40M¤-120M¤)
N(8M¤-120M¤)~ 0.1 (Salpeter IMF)

What causes some small fraction of CC-SNe toproduce observable GRBs, while the majority do not?

Special conditions are requested to stars
to be GRB progenitors:i) to be massive ~ 30-50 M¤ (Maeda et al. 2006; Raskin et al.
2008; Tanaka et al. 2008)ii) H/He envelopes to be lost before the collapse ofthe core, i.e. the GRB progenitor is a WR star(Campana et al. 2006)

GRB 060218/SN 2006aj

3 x104 km/s
Campana et al. 2006s56

SNe-CC size progenitors
Red Supergiant
R~4x1013 cm

The radius of theprogenitor of SN2006aj à
W-R StarBlue Supergiant
R~4x1012 cmR~4x1011 cm57

Special conditions are requested to stars
to be GRB progenitors:i) to be massive ~ 30-50 M¤ (Maeda et al. 2006; Raskin et al.
2008; Tanaka et al. 2008)ii) H/He envelopes to be lost before the collapse of
the core, i.e. the GRB progenitor is a WR star(Campana et al. 2006)iii) low metallicity and star forming environments(Modjaz et al. 2008, Fruchter et al. 2006)

Levesque et al. 2012
See also Modjaz et al. 2011

Special conditions are requested to stars
to be GRB progenitors:i) to be massive ~ 30-50 M¤ (Maeda et al. 2006; Raskin et al.
2008; Tanaka et al. 2008)ii) H/He envelopes to be lost before the collapse ofthe core, i.e. the GRB progenitor is a WR star(Campana et al. 2006)iii) low metallicity and star forming environments(Modjaz et al. 2008, Fruchter et al. 2006)iv) binarity (Panagia 1988 and Smartt et al. 2008 à a significant

fraction of SNe-Ibc progenitors are binaries)

Special conditions are requested to stars
to be GRB progenitors:i) to be massive ~ 30-50 M¤ (Maeda et al. 2006; Raskin et al.
2008; Tanaka et al. 2008)ii) H/He envelopes to be lost before the collapse ofthe core, i.e. the GRB progenitor is a WR star(Campana et al. 2006)iii) low metallicity and star forming environments(Modjaz et al. 2008, Fruchter et al. 2006)iv) binarity (Panagia 1988 and Smartt et al. 2008 à a significant

fraction of SNe-Ibc progenitors are binaries)v) high rotation (Yoon et Langer 2005; Campana et al. 2008,
Yoon et al. 2012)Special conditions are requested to stars
to be GRB progenitors:i) to be massive ~ 30-50 M¤ (Maeda et al. 2006; Raskin et al.
2008; Tanaka et al. 2008)ii) H/He envelopes to be lost before the collapse ofthe core, i.e. the GRB progenitor is a WR star(Campana et al. 2006)iii) low metallicity and star forming environments(Modjaz et al. 2008, Fruchter et al. 2006)iv) binarity (Panagia 1988 and Smartt et al. 2008 à a significant

fraction of SNe-Ibc progenitors are binaries)v) high rotation (Yoon et Langer 2005; Campana et al. 2008,
Yoon et al. 2012)vi) asimmetryc explosion ( Taubenberger et al. 2009;
Maeda et al. 2008)

Within Virgo Circle, in 5 years àwe should observe ~ 5 SNe-Ibc, about half of them
useful for GWs hunting. Only ~ 0.3 HNeWithin 30 Mpc Circle, in 5 years à we should observe
about 1 HN and ~ 15 SNe-Ibc, about half of them
useful for GWs hunting.

Open Issues

“Much ado about nothing": GRB 060614
Low redshift:z = 0.125
SN search?
Gehrels et al. 2006
Mangano et al. 2007

0s

50s

100s

Late time:
host galaxy
contribution(no variation)
Upper limit:
MV > -13.5 (3σ)
Della Valle et al. 2006 (see also Gal-Yam et al. 2006 – Fynbo et al. 2006)

Factor >100

What is the rate of GRB 060614-like events ?

Scenarios without Supernova
1. Supranova à SN occurs (months, years)
before the GRB (Vietri & Stella 1998)
2. NSà QS (Berezhiani et al. 2003; Drago et al. 2008)
3. Vacuum Polarization around Kerr-BH (Ruffini1998; Caito et al. 2008)

4. Binary merging mechanisms similar to those
proposed to power short GRBs (Gehrels et al. 2006)

Scenarios with Supernova-13.5

Pastorello et al. 2007

SN 2008ha is the first faint,hydrogen deficient, lowenergy core-collapse
supernovae ever detected.
Potential “dark SN” (GRBprogenitor) ?

Nomoto et al. 2005
See also Smartt et al. 2008

GRB 060614: SN with small explosion energy à lowexpansion velocity à most 56Ni falls back into the BHà small 56Ni mass in the ejectaà < 10-4/-5 M 56Ni à“Dark Supernovae” (see DV et al. 2006, Nomoto et al. 2007 andTominaga et al. 2007)