Introduction
The Fireshell model
The Induced Gravitational Collapse model
Multiwavelength study of
Gamma-Ray Bursts emission
Ana Virginia Penacchioni
Instituto Nacional de Pesquisas Espaciais (INPE)
São José dos Campos, Brazil
GRACO II
Buenos Aires, April 2014
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Conclusions
Introduction
The Fireshell model
The Induced Gravitational Collapse model
1
Introduction
2
The Fireshell model
3
The Induced Gravitational Collapse model
4
Conclusions
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Conclusions
Introduction
The Fireshell model
The Induced Gravitational Collapse model
What are GRBs?
Intense flashes of
gamma-ray radiation.
Duration: from a fraction of
a second to a few minutes.
Extremely bright.
Extragalactic origin.
Isotropic distribution in the
sky.
Detected through the
orbiting satellites.
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Conclusions
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
Collapsing))
core)
→
Vacuum)polariza/on)
• )e;)
• )e+)
• )e;)
• )e+)
E
→
€
Electric)field)
• )e;)
• )e+)
• )e;)
• )e+)
• )e+)• )e
;)
Op>cally)thick)
e;;e+)plasma)
Some)pairs)annihilate)
to)form)photons)
100
Plasma*
reaches*
outer*shells*III
4
•
IV
II
•
I
10
Transparency*
point*(P2GRB)*
3
A=erglow*
E
m 2c 3
E >€ E c =
e
Expanding)outer)shells)
(baryonic)remnant)of)the)
progenitor)star))
Thermal)equilibrium))
and)accellera/on))
5•
10
Re2accelera'on*
•
1
V
6•
1
8
10
10
12
14
10
10
Radial coordinate (r) (cm)
Ruffini et al. 2001c, 2003b
Ana Virginia Penacchioni
PA
PL
Coas'ng*phase*
2
Accelera'on* •
Lorentz factor
Progenitor)asympto/cally)
collapsing)to)a)BH)
Multi-wavelength study of GRBs emission
10
16
10
18
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
Long, genuine short and disguised-short GRBs
1
P-GRB
Afterglow
Genuine Short: P-GRB
predominant. No afterglow.
Thermal spectrum.
±
Energy/Etot
e
0.8
0.6
Long: Afterglow
predominant. CMB density
∼ 1 part/cm3 .
0.4
Etot
1.44x1049 erg
e
±
0.2
tot
51
Ee 1.68x10 erg
Etot
1.77x1053 erg
e
Etot
1.22x1055 erg
e
±
±
±
0
10-8
10-7
10-6
Genuine&Short&
B"<"10&5"
10-5
B
10-4
10-3
10-2
Long&and&disguised1short&
3"x"10&4"<"B"<"10&2"
10−2
Disguised Short: Afterglow
predominant but with lower
peak luminosity. CMB
density ∼ 10−3 part/cm3 .
B>
⇒ no relativistic expansion.
B → 0 ⇒ genuine short GRB.
Ruffini et al. 2001c, 2003b
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
Long GRBs
GRB 090618
GRB 101023
EPISODE 2 EPISODE 1 Detected by Swift (BAT, XRT,
UVOT), Fermi, AGILE, Konus-Wind,
Coronas-Photon, Suzaku-WAM, VLA.
z = 0.54
Ep1 ∼ 50 s
Ep2 ∼ 100 s
Detected by Swift (BAT,XRT),
Fermi-GBM, Konus-Wind and Gemini.
Unknown redshift.
Ep1 ∼ 45 s
Ep2 ∼ 44 s
Izzo et al. (2012)
Penacchioni et al. 2012, A&A, 538, A58
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
The Fireshell model
GRB 090618: Episode 1
Band
BB+PO
α = −0.7(+0.4, −0.3)
β = −2.3 ± 0.3
Ep = 128(+109, −56)
Red χ2 = 1.11
kT = 32 ± 1 keV
γ = −1.75 ± 0.04
Red χ2 = 1.21
(Physical meaning)
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Conclusions
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
GRB 090618: Episode 1
Radius'of'the'emi.ng'region'
radius!km"
100 000
α='40.33'±'0.07'
70 000
50 000
30 000
20 000
15 000
β='40.5'±'0.1'
10 000
1.0
1.5 2.0
2 σT 4 = 4πr 2 σT 4 (1 + z)4
L = 4πrem
em
em
obs
φobs =
L
4πdL2
dL (z) =
c
H0
=
Rz
0
2 σT 4 (1+z)4
rem
obs
dL2
√
dz 0
Ωm (1+z)3 +Ωk (1+z)2 +ΩΛ
Ana Virginia Penacchioni
3.0
5.0
7.0
10.0
15.0 20.0
r
rem =
30.0
Time!s"
φBB
obs dL
4 (1+z)2
σTobs
Expansion at
NON-relativistic velocities!
v ∼ 1000 km/s, Γ ∼ 1.
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
GRB 090618: Episode 2, P-GRB spectrum BB+PO
Eiso (Ep2 ) = (2.49 ± 0.02) × 1053 erg
EP−GRB = (4.3 ± 0.2) × 1051 erg
∆tP−GRB = 4s
kT = 29.22 ± 2.21 keV
NormBB = 3.5 ± 0.4
γ = 1.85 ± 0.06
normPL = 46 ± 10
Redχ2 = 1.15
A&A 543, A10 (2012)
Table 2. Time-resolved spectral analysis (8 keV–10 MeV) of the second episode in GRB 090618.
The remaining part is best fit by a Band model:
A
B
C
D
E
F
Time interval (s)
0–50
50–59
59–69
69–78
78–105
105–151
↵
–0.74 ± 0.10
–1.07 ± 0.06
–0.99 ± 0.02
–1.04 ± 0.03
–1.06 ± 0.03
–2.63 ± –1
–2.32 ± 0.16
–3.18 ± 0.97
–2.60 ± 0.09
–2.42 ± 0.06
–2.62 ± 0.09
–2.06 ± 0.02
E0 (keV)
118.99 ± 21.71
195.01 ± 30.94
321.74 ± 14.60
161.53 ± 11.64
124.51 ± 7.93
unconstrained
Ana Virginia Penacchioni
˜ 2BAND
1.12
1.23
2.09
1.55
1.20
1.74
kT (keV)
32.07 ± 1.85
31.22 ± 1.49
47.29 ± 0.68
29.29 ± 0.57
24.42 ± 0.43
16.24 ± 0.84
1.75 ± 0.04
1.78 ± 0.03
1.67 ± 0.08
1.78 ± 0.01
1.86 ± 0.01
2.23 ± 0.05
˜ 2BB+po
1.21
1.52
7.05
3.05
2.28
1.15
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
GRB 101023: Redshift determination
1) Amati relation
2) NH column density
Grupe, D. et al. (2007),AJ,133,2216
0.3$<$z$<$1.0$
Eiso =
4πdL2
(1+z) Sbol
Ep,i = Ep (1 + z)
R 104 /(1+z)
Sbol = Sobs
1/(1+z)
R Emax
Emin
E φ(E )dE
E φ(E )dE
∗ Get NH,gal from the coordinates of the
burst. Lab Survey: http://www.astro.unibonn.de/?webaiub/english/tools
labsurvey.php
∗ Fit the XRT spectrum with an absorbed
Power-law (phabs*po in XSPEC), fixing
NH,gal to get NH,fit.
∗ Compute ∆NH = NH,fit − NH,gal
∗ Put it in the formula
log (1 + z) < 1.3 − 0.5[log (1 + ∆NH )]
∗ z < 3.8
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
GRB 101023: Redshift determination
4) Overlapping of the light curves
∗ 0.3 − 10 keV Swift-XRT observed flux
light curve of GRB 101023 and GRB
090618.
∗ Transform the flux from the observer
frame to the rest frame: Frf = Cf Fobs .
∗ Transform the time from the observer
to the rest frame: trf = tobs /(1 + z).
∗ Calculate L in the rest frame:
L = 4πdL2 Frf .
For GRB 0901618, z = 0.54. z varies
for GRB 101023 until the light curves
overlap. z = 0.9
GRB$090618$
GRB$090618$
GRB$101023$
Penacchioni et al. 2012, A&A, 538, A58
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
The Fireshell model
GRB 101023: Episode 1
BB+PO
kT = 14 ± 6 keV
γ = 1.7 ± 0.1
Redχ2 = 0.98
Band
α = −1.3 ± 0.08
β = −1.9 ± 0.2
E0 = unc, Norm = unc
Redχ2 = 0.98
Eiso (Ep1 ) = 4.03 × 1053 erg
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Conclusions
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
GRB 101023: Episode 2
BB+PO
Band
α = −0.9 ± 0.1
β = −2.0 ± 0.1
E0 = 151 ± 24 keV
Norm = 0.043 ± 0.008
Redχ2 = 1.09
P-GRB
∆tP−GRB = 5 s
kTobs = 28.46 keV (14.96
keV after cosmological
correction).
EP−GRB = 2.51 × 1051 erg
Ana Virginia Penacchioni
kT = 26 ± 1
keV
γ = 1.58 ± 0.03
Redχ2 = 1.12
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
GRB 101023: Episode 1
Radius'of'the'emi.ng'region'
k T!keV"
50
Radius!km"
α='40.4'±'0.3'
1 ! 106
30
5 ! 105
20
2 ! 105
15
1 ! 105
10
5 ! 104
β='1.4'±'1.1'
1.5
2.0
3.0
5.0
7.0
10.0
2 ! 104
t!s"
15.0 20.0
r
rem =
1.5
2.0
3.0
5.0
7.0
10.0
15.0 20.0
Time!s"
φBB
obs dL
4 (1+z)2
σTobs
Expansion at NON-relativistic velocities! v ∼ 104 km/s, Γ ∼ 1.
Episode 1: Proto-Black hole
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Fireshell model
Simulation of the light curves and spectra
fit of the light curve of GRB 090618
Fermi-GBM light curve counts data of GRB 090618
60
’lc_sub_101023.txt’ u 1:2:3
’GRB101023.GRBsim7LCct’ u ($1+48):3
40
35
50
30
Counts/s
40
25
30
20
15
20
10
10
5
0
0
2012)
0
50
100
Timefireshell
(s)
ble 3. Final results of the simulation of GRB 090618 in the
nario.
0
kT th
EP GRB,th
n
n
Value
40
theoretical simulation
Fermi GBM count spectrum 8-1000 keV
60
80
0.1
0.01
10
ble 4. Physical properties of the three clouds surrounding the burst
.
Cloud
Distance (cm)
r (cm)
⇢ (#/cm3 )
First
Second
4.0 ⇥ 1016
7.4 ⇥ 1016
1 ⇥ 1016
5 ⇥ 1015
1
1
0.01
0.001
0.001
100
Energy (keV)
120
140
1e-04
10
100
Energy(keV)
M (g)
2.5 ⇥ 1024
3.1 ⇥ 1023
Ana
Virginia Penacchioni
160
B = 3.8 × 10−3
Lab radius:
r = 1.34 × 1014 cm
Γ ∼ 260
kTth = 13.26 keV
EP−GRB = 1.89 × 1052 erg
0.1
2.49 ± 0.02 ⇥ 1053 erg
1.98 ± 0.15 ⇥ 10 3
495 ± 40
29.22 ± 2.21 keV
4.33 ± 0.28 ⇥ 1051 erg
0.6 part/cm3
2 part/cm3
100
Spectrum Fermi GBM (8-440 keV)
Simulation of the spectrum
1
Photons/keV/cm2/s
+
e e
Etot
B
counts/cm2/s/keV
Parameter
150
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
The Induced Gravitational Collapse model
Progenitor: close binary system composed of
an evolved massive star in the latest phases of
its thermonuclear evolution and a NS
companion.
Time sequence:
1) the massive star undergoes a SN explosion;
2) part of the early-SN material is accreted
onto the NS companion;
3) the NS companion reaches its critical mass
Mcrit = 2.67M and it gravitationally collapses
to form a BH;
4) a canonical GRB is emitted.
Outcome: binary system formed by a NS and
a BH.
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Conclusions
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Induced Gravitational Collapse model
GRB 110709B
1st trigger
2nd trigger
Unknown redshift.
Optically dark GRB
0.4
Episode(1(
Counts/s
0.3
Episode(2(
Zauderer et al (2012).
Contemporaneous data from BAT
and XRT.
0.2
0.1
200
400
600
800
1000
Time (s)
Detected By Swift, Suzaku,
Konus, GROND, APEX, EVLA,
Gemini-South, etc.
Ep1 ∼ 100 s
Separation: 611s ∼ 10 minutes
Ep2 ∼ 135 s
Penacchioni et al. 2013, A&A, 551, A133
Ana Virginia Penacchioni
10−8
10−9
10−10
10−11
10−12
10−13
3
Γ
0
0.3−10 keV flux (erg cm−2 s−1)
XRT data of GRB 110709B
Cyan: WT setting; Blue: WT; Red: PC
0
2
1
100
1000
104
105
Time since BAT trigger (s)
Multi-wavelength study of GRBs emission
106
107
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Induced Gravitational Collapse model
GRB 110709B
Episode 1: BB+PO
kT = 22 ± 5 keV
NormBB = 0.2 ± 0.1
γ = 1.4 ± 0.1
Normpo = 2.2 ± 0.8
Redχ2 = 1.049, DOF = 54
Flux = 8.96 × 10−8 erg/cm2 /s
(15 − 150 keV)
Ana Virginia Penacchioni
Episode 2: Cutoffpl
γ = 1.0 ± 0.1
E0 = 132 ± 31
K = 0.5 ± 0.1
Redχ2 = 0.77, DOF = 55
Flux = 2.43 × 10−8 erg/cm2 /s
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Induced Gravitational Collapse model
GRB 110709B: Redshift estimation
Yonetoku Relation:
Amati Relation
700
Ep,i !keV"
500
z">"0.4"
300
X
X X
200
X
Yonetoku (2004)
z">"0.6"
X
X
X
X
X
X
X
X
XXX
X
X
X
XXX
XX
XX
XX
150
100
1051
1052
Eiso !erg"
1053
Amati, L., 2006, MNRAS 372, 233
NH column density:
z < 1.35
Grupe, D. et al. (2007),AJ,133,2216
Ana Virginia Penacchioni
L
1052 erg /s
−5
= (2.34+2.29
−1.76 ) × 10
L = 4πdL2 Fbol
Fbol = Pobs
Ep (1+z) 2.0±0.2
1keV
R 10000/(1+z)
EN(E )dE
1/(1+z)
R Emax
N(E )dE
Emin
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Induced Gravitational Collapse model
GRB 110709B: Redshift estimation
Overlapping of the X-ray light curves
Ana Virginia Penacchioni
10-8
Flux @erg cm-2 s -1 D
Procedure:
1) Convert the observed energy
range to the rest-frame.
2) Assume that the late X-ray
decay is well fit by a simple PL.
3) Convert the observed flux fobs
to the rest-frame.
4) Calculate the luminosity in the
rest-frame: Lrf = 4πdL2 (z)frf
5) Convert the time to the
rest-frame: trf = tobs /(1 + z)
10-10
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
OO
O O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
OO O
O
O
O
O
O
O
O O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
O
10-12
OO
O
O
O
O
O
O
OO
O
O
O
O
O
O
O
O
O
O
O
O
O
OO
O
O
O
O
O
O
O
O
O
O
O
O
O
O
OO
OO
OO
O
O
O
O
O
O
O
O
OO
O
O
O
O
O
O
O
O
O
O
O
OO
O
O
O
OO
O
O
O
O
O
O
O
OO
OO
O
O
O
OOO
OO
O
O
OOO
O
OOOOO
OO O
10-14
100
1000
104
Time @sD
z = 0.75
Multi-wavelength study of GRBs emission
105
106
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Induced Gravitational Collapse model
GRB 110709B: Episode 1
E(Ep1)&=&1.42&×&1053&erg&
20
200 000
150 000
α&=&0&&
100 000
5
rem !Km"
kT !keV"
70 000
10
β&=&−4±2&
2
1
1
50 000
30 000
20 000
15 000
10 000
2
5
10
tobs !s"
20
50
1.0
1.5 2.0
r
BB → expansion of the ejected
material.
PL → accretion of part of this material
onto the NS companion.
Penacchioni et al., 2013, A&A, 551, A133
Ana Virginia Penacchioni
rem =
time !s"
3.0
5.0
7.0 10.0 15.0 20.0 30.0
φBB
obs dL
4 (1+z)2
σTobs
a = (1.5 ± 1.2) × 104 km s−b
b = 0.32 ± 0.27
Expansion at NON-relativistic
velocities
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
The Induced Gravitational Collapse model
GRB 110709B: Simulation of the light curve and spectrum of Episode 2
GRB 110709B light curve
Simulation of the light curve
3.5
Swift BAT spectrum of GRB 110709B (15 -150 keV)
Swift XRT spectrum of GRB 110709B (0.3 - 10 keV)
Simulated count spectrum of GRB 110709B
1
3
0.1
Photons/(cm s keV)
2
2
Counts/(cm2 s)
2.5
1.5
0.01
1
0.001
0.5
A&A 551, A133 (
0
-40
-20
0
20
40
Time [s]
60
80
100
120
1
10
Energy [keV]
100
Table 3. Fit of the P-GRB and the afterglow of GRB 110709B,
episode 2.
Spectral)fit)of)Episode)2)
B = 5.7 × 10−3
r = 6.04 × 1013 cm
Γ = 1.73 × 102
P-GRB obs T(after cosmological correction):
kT = 12.36 keV
< nCBM >= 76 part/cm3
P-GRB → BB
EP−GRB = 3.44 × 1050 erg
Afterglow → Cutoffpl
E (Ep2 ) = 2.43 × 1052 erg
Ana Virginia Penacchioni
Parameter
kT [keV]
BB Amp
PL Amp
Red 2
Energy flux
(15 150 keV)
[erg cm 2 s 1 ]
Energy [erg]
P-GRB
14 ± 1
0.30 ± 0.02
P-GRB+afterglow
1.448 (56 D.O.F.)
2.413 ⇥ 10 8
1.03 ± 0.1
0.5 ± 0.1
0.77 (55 D.O.F.)
6.34 ⇥ 10 8
3.44 ⇥ 1050
2.43 ⇥ 1052
Notes. The P-GRB is well-fit with a BB model, while the whole
episode 2 is best fit bystudy
a cuto↵PL
model.emission
From this fit and the value
Multi-wavelength
of GRBs
Introduction
The Fireshell model
The Induced Gravitational Collapse model
Conclusions
Conclusions
The sources we studied present a standard behavior with different
episodes:
Episode 1: thermal (+ non-thermal) emission in γ-rays. kT
follows a broken-PL behavior. It corresponds to the onset of
the SN in the IGC model.
Episode 2: canonical GRB (P-GRB + Afterglow). Formation
of a BH from the NS companion.
Episode 3: late decay in the X-ray luminosity light curve.
Associated with the cooling of the newly-formed NS from the
SN explosion.
Episode 4: SN emission ∼ 10 days from the burst in the
cosmological rest-frame. It is observed as a bump in the
optical band.
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Introduction
The Fireshell model
Conclusions
The Induced Gravitational Collapse model
156
Conclusions
CHAPTER 6. THE SCALING
We created a sample of 8 GRBs following (some of) these
Table 6.1: Sample of GRBs belonging to the IGC family. The
requirements:
with an (*) were estimated by using the method described in
∗E > 1052 erg
the corresponding energies were calculated assuming these re
∗Episodes 1, 2, 3 and 4
GRB
z
Eiso (erg)
∗Measured cosmological z
060729
0.54 1.6 ⇥ 1052
061007
1.261 1.0 ⇥ 1054
∗Associated SN
080319B
090618
091127
111228
101023
110709B
0.937
0.54
0.49
0.713
0.9*
0.75*
1.3 ⇥ 1054
2.9 ⇥ 1053
1.1 ⇥ 1052
2.4 ⇥ 1052
1.8 ⇥ 1053
1.7 ⇥ 1053
We are looking for more
• they need to present
Episodes
1, 2, 3 and
with the
GRBs
belonging
to 4,
this
scribed above,
subclass.
• Pisani&et&al.&(2013)&
they need to have a measured cosmological redshift,
• they
Ana Virginia Penacchioni
haveMulti-wavelength
to present evidence
of an
associated SN.
study of GRBs
emission
Introduction
The Fireshell model
The Induced Gravitational Collapse model
THANK YOU!
Ana Virginia Penacchioni
Multi-wavelength study of GRBs emission
Conclusions