The Empirical Grounds of the
SN-GRB Connection
M. Della Valle
INAF-Napoli
ICRANet-Pescara
Outline
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Supernova Taxonomy
GRB-SN properties
GRB-SN census à GRB 100316D / SN 2010bh
GRB and SN rates
Progenitors Properties
Supernova taxonomy
thermonuclear < 8M¤
core-collapse > 8M¤
H
II
I
Si
IIL IIP IIn
He
Ia
Ib
Ic
bright
faint
very
bright
à High KE SNe-Ic à Hypernovaeà GRB-SNe
GRB-SN census (z < 0.2)
GRB
SN
z
Ref.
GRB 980425
SN 1998bw
0.0085
Galama et al. 1998
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 060218
SN 2006aj
0.033
Campana et al. 2006
GRB 080109
SN 2008D
0.007
Soderberg et al. 2008
Mazzali et al. 2008
GRB 100316D
SN 2010bh
0.06
Chornoch et al., Bufano
et al., Starling et al. 2011
Properties of GRB-SNe (broad-lined SNe-Ic)
Lack of H and He in the ejecta: SNe-Ic
Very broad features: large expansion
velocity (0.1c)
Very large luminosity: large 56Ni mass
( ~ 0.5±0.2 M)
Energy (non-relativistic ejecta) ~ 1052 erg
≳ 10 larger than usual CC-SNe
Explosions are aspherical (profiles of
nebular lines O vs. Fe and Polarization)
SN 1998bw
SN 1987A
Maeda et al. 2006
2008
GRB-SNe are very
energetic events
=
E ~ 30×1051ergs
Aspherical
explosion
E ~ 1×1051ergs
Interpreting spectra: position
of elements
Immediately after explosion SNe go into
homologous expansion, i.e. vel is proportional
to the radius:
i) Relative positions of elements do not change
ii) Inner elements move slower than the outer ones
Late time spectra of SN1998bw
Fe lines broader than O lines
O
FWHM
[FeII]
5200A
[OI]
6300A
Observation
Fe
Expansion
Observer
Never in Spherical Model
Maeda et al. 2002
Spherical
FeII]
5200A
[OI] 6300A
Observed
Aspherical
Orientation
15 deg
II à IIb à Ib à Ic
1% ……………. 4%
Maeda et al. 2002
The new “baby”
GRB 100316D/SN 2010bh
Discovered by Swift;
T90 ≥ 1300s, similar to GRB 060218
z = 0.059 or 250 Mpc
Chornock et al. 2010 Bufano et al. 2011 Starling et al. 2011 Cano et al. 2011
GRB021211/SN 2002lt
Bufano et al. 2011
Rising time 8d (rest-frame).
The steepest rise ever observed.
Della Valle et al. 2003
GRB 050525A/SN 2005nc
Della Valle et al. 2006
rising time ~ 10d.
Maeda et al. (2005)
showed that asymmetric
SNe peak earlier if
observed close to their
polar axis.
INTENSIVE VLT
FOLLOW-UP with
X-shooter
Bufano et al. 2011
He I has been
detected !
5876 Å at ~ 5200 Å
1.083µm at ~ 9500 Å
Possible detection of
2.058 µm
CC-SNà Ib
[O I] bump is much fainter than observed in 1998bw. This indicates
a very small amount of oxygen ejected and consequently a less
massive progenitors than for SN 1998bw.
2010bh would be produced by the core collapse explosion of a
20-25M¤ and EK ~1052 erg, Mejc ~ 3 (± 50%). Fast magnetar?
(Fan et al. 2011); BH?)
GRB-SN census (z > 0.2)
GRB
SN
z
Ref.
GRB 021202
SN 2002lt
1.002
Della Valle et al. 2003
GRB 050525A
SN 2005nc
0.606
Della Valle et al. 2006
GRB 081007
SN 2008hw
0.53
Della Valle et al. 2008
GRB 091127
SN 2009nz
0.49
Cobb et al. 2010
Berger et al. 2011
GRB 101219B
SN 2010ma
0.55
Sparre et al. 2011
GRB 060729
SN ?
0.54
Cano et al. 2011
GRB 090618
SN ?
0.54
Cano et al. 2011
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
Bumps can be produced by different phenomena as
dust echoes or thermal re-emission of the afterglow
or thermal radiation from a pre-existing SN remnant
(e.g. Esin & Blandfors 2000; Waxman & Draine 2000; Dermer 2003)
At higher redshift secure SN identification
becomes difficult because the SN gets
fainter, which leads to problems of obtaining
sufficient signal-to-noise in
the spectra, a problem that is aggravated by
contamination of the host galaxy and the
afterglow
Time consuming observations Della
àValle
single
et al. 2003epoch
spectrum
GRB 081007
A GRB-SN at z=0.5
06/09/11
20
SN 2008hw vs. SN 1997ef
21
2008hw vs. SN 2004aw
22
2008hw vs. SN 1998bw
23
Cobb et al. 2010
Berger et al. 2011
GRB 091127/SN 2009nz
These observations allow us to use the rebrightenings
observed in the AGs as tracers of SNe.
Since rebrightenings are observed up to z ~ 1, then
the connection between GRBs and SNe can be
confidently extended up to z ~ 1 (~8 Gyr)
Della Valle et al. 2003
GRBs and SNe are coeval
GRB
SN
+Δt(d)
-Δt(d)
Ref.
Iwamoto et
980425
1998bw
0.7
2
The near simultaneity of non thermal (GRB)
al. and
thermalBump
(SN) X-ray1.5
emissions 7indicates that
the
SN
Lazzati
et al.
000911
and GRB are coeval events within ~ a few
x Valle
102set
Della
021211
2002lt
1.5
3
al.
030329
2003dh
2
0
8
2
Kawabata et al
Matheson et al
031203
2003lw
0
2
Malesani et
al.
041006
Bump
2
0
Stanek et al.
050525A 2005nc
0
2
Della Valle et
al.
060218
2006aj
~0.003
--
Campana et al.
080109
2008D
~0.06
--
Mazzali et al.
Soderberg et al.
What is the fraction of SNe-Ib/c which
produces (long)GRBs ?
Rate for Ib/c: 0.2 SNu
1.2 x 108 LB, Mpc-3 à 2 x 104 SNe-Ibc Gpc-3 yr-1
GRB rate: 0.5-1.1 GRB Gpc-3 yr-1
<fb-1> ~500
<fb-1> ~75
<fb-1> < 10
<fb-1> ~ 1
(Frail et al. 2001)
(~ 4°)
(Guetta, Piran & Waxman 2004)
(~ 10°)
(Guetta & DV 2007 for sub-lum GRBs)
(> 25°)
(Ruffini et al. 2006)
GRB/SNe-I(b)c: 3%-0.01%
(~ 4 π)
Radio survey on nearby
Guetta and
DV 2007 à GRB/SNe
SNe-Ibc
<3% (Berger et al. 2003)
27
GRB/SNe-Ibc ~ 1/146
GRB/SNe-Ibc ~ 0.7%
< 4.5% at 99%
GRB/SNe-I(b)c: 3%-0.01%
Grieco, Matteucci + 2011
Matsubayashi et al. 2005
Wandeman & Piran 2009
the ratio GRB/SNeIbc ~ 10-3/-4 à0.1-0.01%
GRB/SNe-Ibc ~ 0.7% (<5%) SN Radio Observations
GRB/SNe-I(b)c: 3%-0.01% (GRB vs SN observed rates)
GRBs are very rare phenomena
(compared to SN explosions)
GRB/SNe-I(b)c: 3%-0.01%
Ibc/CC ~ 0.25
GRB/CC-SN < 1% or << 1%
What causes some small fraction of CC-SNe to
produce observable GRBs, while the majority do not?
Special conditions are requested to stars
to be GRB progenitors:
i) to be massive ~ 30-50 M¤
Kelly et al. 2008 find that local SNe-Ic erupt in the brightest regions of
their hosts (like GRBs, see Fruchter et al. 2006)
Long-GRBs have ~ 40 M
Raskin et al. 2008
Modeling lightcurves and spectra
1998bw
40 M
2003dh
2003lw
2006aj
2008D
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.
2003
2006
2006
2008
Special conditions are requested to stars
to be GRB progenitors:
i) to be massive ~ 30-50 M¤ (Raskin 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)
What Stars are GRB Progenitors ?
z = 0.033
faint: Eγ ∼ 1049 erg
MV (host) = -16
Host has brightness
Similar to SMC
GRB 060218/SN 2006aj
Z/Z ~ 0.3
(Campana et al. 2006)
2006aj = SN-Ic
36
GRB 060218
37
Campana et al. 2006
3 x104 km/s
s
Campana et al. 2006
38
SNe-CC size progenitors
Red Supergiant
R~4x1013 cm
The radius of the
progenitor à
W-R Star
Blue Supergiant
R~4x1012 cm
R~4x1011 cm
39
ž
Special conditions are requested to stars
to be GRB progenitors:
i) to be massive ~ 30-50 M¤ (Raskin 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)
Modjaz et al. 2008
San Servolo, 2007
41
Special conditions are requested to stars
to be GRB progenitors:
i) to be massive ~ 30-50 M¤ (Raskin 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)
iv) binarity (Smartt et al. 2008 à a significant fraction of SNeIbc progenitors are binaries)
Special conditions are requested to stars
to be GRB progenitors:
i) to be massive ~ 30-50 M¤ (Raskin 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)
iv) binarity (Smartt et al. 2008 à a significant fraction of SNeIbc progenitors are binaries)
v) high rotation
(Yoon et Langer 2005; Campana et al. 2008)
LONG GRBs
*  Association with
bright (Ib/c)core-collapse
SNe
*  Star-forming host galaxies
SHORT GRBs
*  Differentiated host galaxies
(early types and spirals)
*  Not associated with recent
star formation (?)
*  Binary compact object
mergers?
44
Messing up matters: GRB 060614
Low redshift:
z = 0.125
SN search?
Gehrels et al. 2006
Long GRBs: T > 2 sMangano et al. 2007
Short GRBs: T < 2 s
0s
50s
100s
Late time:
host galaxy
contribution
(no variation)
Factor >100
Looking for a SN
Upper limit:
MV > -13.5 (3σ)
Della Valle et al. 2006 (see also Gal-Yam et al. 2006 – Fynbo et al. 2006, Caito et al. 2009)
What produces the observed variety in
long duration GRB phenomenology ?
i) HL-GRBs (≥ 1051 erg) + bright Ic (GRB 030323/ 2003dh)
ii) LL-GRBs (≤1049 erg) + bright Ic (GRB 060218/SN 2006aj)
iii) LL-GRBs (≤1049 erg) + faint Ib (GRB 100316D/SN 2010bh)
iv) vLL-GRB (≤1046 erg) + SN-Ibc (GRB 080109/SN 2008D)
v) HNe w/out GRBs (e.g. 2002ap)
vi) GRBs w/out (bright?) SN (GRB 060614)
Rate
Cosmological
HL-GRBs +HNe
(2003dh-like)
weak X-ray flashes
( failed GRBs) +
HNe (2008D-like)
Local LL-GRBs
+HNe (2006aj-like)
While the γ-budget covers about ~ 6 order of
magnitudes, the luminosity of the GRB-SNe vary
by at most a factor ~4
49
A simplified Scheme for a GRB-SN event
-  an almost isotropic
component carrying most
energy 1052 erg and mass
(~5-10M¤) à SN event
-highly collimated
component (4°-10° for
HL-GRBs and > 25° for
LL-GRBs) containing a
tiny fraction of the
mass (10 -4/-5 M)
moving at Γ ~ x 102-3
à GRB
30,000 km/s
à  The lack of a relation between Mag(max)
and E(iso) or E(peak) suggests that
γ-properties maybe a strong function of
the angle (Eγ ∼ ϑ-4 ) whereas the optical
properties are not much influenced by this
relative small spread in viewing angles.
line of sight
SN
line of sight
SN + GRB
Metallicity
~
55
Scenarios without Supernova
i) Merging of comapct objects + Vacuum
Polarization (Ruffini 1998)
ii) Binary merging mechanisms similar to
those proposed to power short GRBs (Gehrels
et al. 2006)
56
Light curves of SNe-Ic: GRB-SNe, broad-lined SNe, normal SNe
-13.5
57
A new class of transients?
Kulkarni et al. 2007
Nomoto et al. 2005
See also Smartt et al. 2008
GRB 060614: SN with small explosion energy à low expansion
velocity à most 56Ni falls back into the BH à small 56Ni mass
in the ejectaà ~ 10-4/-5 M 56Ni à “Dark Supernovae” (see DV et al.
2006, Nomoto et al. 2007 and Tominaga et al. 2007)
Massive star evolution
Zampieri et al. (2003)
060614: SN with small explosion energy à low expansion
velocity à most 56Ni falls back into the BH à small 56Ni mass
in the ejectaà ~ 10-4/-5 M 56Ni à “Dark Supernovae” (see DV et al.
2006, Nomoto et al. 2007 and Tominaga et al. 2007)