SN-GRB Connection: Observations and Questions

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SN-GRB Connection: SN-GRB Connection: Observations and Observations and

QuestionsQuestions

Massimo Della ValleINAF-Osservatorio Astrofisico di

Arcetri, FirenzeBologna, 1 Giugno, 2006

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Outline

• Introduction

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Outline

• Introduction• SN 1998bw/GRB 980425, SN 2003dh/GRB 030329,

SN 2003lw/GRB 031203

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Outline


SN 2003lw/GRB 031203• Bumps (SN 2002lt & SN 2005nc)

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Outline



• SNe-Ibc & Hypernova & GRBs rates

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Outline



• SNe-Ibc & Hypernova & GRBs rates • Time lag SN-GRBs

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Outline



• SNe-Ibc & Hypernova & GRBs rates • Time lag SN-GRBs• GRB hosts

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Outline



• SNe-Ibc & Hypernova & GRBs rates • Time lag SN-GRBs• GRB hosts• Discussion & Conclusions

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Outline



• SNe-Ibc & Hypernova & GRBs rates • Time lag SN-GRBs• GRB hosts• Discussion & Conclusions• Recent (exciting) Results

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Gamma-ray bursts: prompt emission

“Brief (< 100 sec) and intense (~10-6 erg/cm2/s) flashes ofsoft (~100 keV) gamma-ray radiation”

Temporal beahviour: wide variety

Highly structured Single pulse

t << T

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Long and short GRBs

GRBs duration: (0.01 ÷ 100) s

The distribution is bimodal

Hardness/duration correlation:

short bursts are harder

All the results I will presentconcern the long-durationclass of GRBs!

Paciesas et al. 2000

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Afterglows

Long-lived counterparts at X-ray, optical, IR and radio wavelengths

Discovery: GRB 970228 by the BeppoSAX satellite

Optical counterpartssoon after

Costa et al. 1997

van Paradijs et al. 1999

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Jakobsson et al. 2005

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Clues about progenitors

The distance is ~ a few Gpc 3.11015 cm Observed flux 105/-6 erg cm2 s1

luminosity: 1051-54 erg

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Energetic Scale: Jets or Sphere

• GRB 990123 has been detected by the robotic telescope ROTSE, 22s and 47s after the -ray trigger at V~11.7 and 8.9, respectively. At z=1.6, the isotropic energy release implies MV ~-35 and a global energetic budget comparable to >Mc2

• All GRBs could be collimated events, with opening angles ~ 5-10 degrees (break in the power law decay of the afterglows, polarization)

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And in fact the jet effect on the light curve was observed in several GRBs. Here is an example. Due to its nature the jet break time measured from the observations (i.e. monitoring) of the burst afterglow allows to estimate the physical aperture of the GRB jet.

“Jet break”

Jet break time tbreak

Jet opening angle

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““True” energetics: True” energetics: correcting the energyes derived with the assumption that GRBs are correcting the energyes derived with the assumption that GRBs are isotropic the energy crisis is relaxed. Moreover the typical energetics clusters around a isotropic the energy crisis is relaxed. Moreover the typical energetics clusters around a similar value of 10^51 erg which is by far more standard also in comparison to other similar value of 10^51 erg which is by far more standard also in comparison to other

astro sources.astro sources.Fra

il e

t al.

2001

Isotropic equivalent Isotropic equivalent energyenergy

Etrue = Eiso (1 – cos )

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X-ray Flashes

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Probable Sequence of GRB Events

• The central engine emits a large amount of energy.

• Most of that energy accelerates a small mass (~10-5 M) to speeds > 99.99% of lightspeed (~100/500)

• Collisions between different shells of ejected debris creates the gamma rays.

• Collisions between ejected debris and interstellar gas create the afterglow.

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The progenitors collapses or coalesceces,

forming a spinning BH

Progenitor location:<108 cm

…and the colliding

shells give rise

to the GRB

GRB location

<1014 cm

The energy escapes in the form of jets…

observer

Afterglow location <1018

cm

Kinetic Energy

Shock dissipatio

n

Afterglow

Dense cloud

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SNe & GRBs Facts

• ‘Early Gamma-Rays from Supernovae’ (Colgate 1968 & 1974)

• GRB 980425 SN 1998bw (Galama et al. 1998)

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• SN 1998bw was discovered on NTT images of ESO 184 G82 at z=0.0085

• The GRB and the SN appeared spatially (P~10-4/-5) and temporally coincident t= +0.7d -2.0d (Iwamoto et al. 1998)

• SN 1998bw rivals with SN 1991T: MB =-19.5

To achieve such a luminosity about 0.5-0.7 M of Ni have to be synthesized in the explosion. This is unprecedented for Core Collapse events (less than 0.1 M )

• The radio emitting shell was expanding at (mildly) relativistic velocities ~1.8 (Kulkarni et al. 1998; Weiler et al. 1999)

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Patat et al. 2001

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Patat et al. 2001

Mg I

O I

[Ca II]

[O I]

Na I

Ca II

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Patat et al. 2001

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Pec Type Ic SNe

Broad lines

Large Kinetic Energy

“Hypernovae”

(only SN1998bw was associated with a GRB)

Narrow lines

“normal” KE (1051)

Normal SN Ic

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Pec Type Ic SNe = Hypernovae

Broad lines

Large Kinetic Energy

“Hypernovae”

(only SN1998bw was associated with a GRB)

Narrow lines

“normal” KE (1051)

Normal SN Ic

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Light Curves of Supernovae & Hypernovae

Brightness alone Brightness alone should not be should not be used to define a used to define a hypernova, hypernova, whose main whose main characteristic is characteristic is the high Ethe high Ekk~10~105252 ergs (see broad ergs (see broad spectral spectral feauturesfeautures))

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SN 1998bw

=

SN 1987A

E ~ 30×1051ergs E ~ 1×1051ergs

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Circumstantial evidence: The Bumps 1999-2003 (Bloom et al. 1999)

Della Valle et al. 2006

Della Valle et al. 2003 (MISTICI Collaboration)

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Are the bumps representative of signatures of incipient SNe?

Or they 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)

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Ca

The spectrum of the afterglow associated with GRB 021211, obtained during the bump, reveals the presence of a broad absorption feature (FWHM~150 A), blueshifted by ~15000 km/s, which has been identified with CaII H+K SUPERNOVA 2002ltSUPERNOVA 2002lt


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SN 1994I

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SN 1998bw was a peculiar Ic associated with a peculiar GRB energy budget about a few x 1047 ergs)

Evidence for the existence of a SN/GRB connection was circumstantial before March 2003

SN bumps were only suggestive for the existence of a SN/GRB connection. The spectroscopic confirmation was obtained only in one case (SN 2002lt/GRB 021211) and based on one spectrum (z=1). In addition the lightcurve was different from SN 1998bw

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The Smoking Gun (part 1)

2003dh /GRB 0303292003dh /GRB 030329

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GRB 030329/SN 2003dh = Smoking GRB 030329/SN 2003dh = Smoking Gun IGun I Stanek et al.2003; Stanek et al.2003;

Hjorth et al. 2003Hjorth et al. 2003 8 Apr 8 Apr

SpectrumSpectrum

--1 Apr 1 Apr

SpectrumSpectrum

= ?= ?

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Matheson et al. 2003

z=0.16

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The spectrum is very similar to the one exhibited by the type Ic SN 1998bw

GRB and SN events are spatial coincident and coeval

SN 2003dh was not so bright as 1998bw (0.3-0.5 M 56Ni)

Modelling (Deng et al. 2005): Mej ~ 7±3M; Prog = 25-40 M; MBH ~ 3 M

Fe II lines broader than [O I] (Maeda et al. 2005, 2006) aspherical explosion

The -energy associated with GRB 030329 is ‘’standard’’ (6.9 x 1051 erg) Sakamoto et al. 2004

GRB 030329/SN 2003dh: facts

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GRB 031203 & SN 2003lwMalesani et al. 2004

The Smoking Gun (part 2)

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GRB 031203/2003lw =Smoking Gun II

• Trigger from INTEGRAL

• Observations:ESO NTT & VLT

• Afterglow: X-ray (XMM) & radio (VLA)

• Low redshift host galaxy (z = 0.1) Very faint: E 1049 erg

Götz et al. 2003

Watson et al. 2004, Soderberg et al. 2004

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Spectroscopic ObservationsVLT + FORS Bright star-forming

host galaxy

SFR 10 M/yr

Z 0.1Z

AV 1.1

Prochaska et al. 2004 Chincarini et al. 2014

Broad undulations in the continuum close to the maximum

Malesani et al. 2004

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Spectra of SN 2003lw

Host galaxy subtracted

Tagliaferri et al. 2004


EK = 6 x 1052 ergM 56Ni = 0.55 M

Mej = 13 M

Mprg = 40-50 M Mazzali et al. 2006

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The very bright supernova 2003lw

SN 2003lwvs

SN 1998bw

With E(B–V) = 1.1:

* 0.5 mag brighter

* Same colors

* Slower evolution

Overall similar

See also Bersier et al. 2004; Thomsen et al. 2004, Cobb et al. 2004, Gal-Yam et al. 2004


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Conclusions

The discovery of the types Ic SNe 2003dh(Stanek et al. 2003; Hjorth et al. 2003) and SN 2003lw (Malesani et al. 2004) in the AGs of GRB 030329 and GRB 031203 has conclusively linked long duration GRBs

with the death of massive stars Particularly with a subclass of SNe-Ibc, the bright tail of HYPs

Is the game over?

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…there is an expanding frontier of ignorance…

(R. Feynman, Six Easy Pieces)

Not at all...

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There is growing evidence that GRBs can be associated with SNe which are different from SN 1998bw, both in the peak of luminosity and in spectroscopic type(SN 2002lt/GRB 021211 SN 1994 I normal Ibc 1994I)

What SN types are connected with GRBs? (only 1998bw-like?)

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SN in XRF 030723

LC Fits: a normal SN Ic or a low-E Hyp like SN2002ap at z~0.6

Fynbo et al. 2004;

Tominaga et al.2004

Lg (Fx/F) > 0 XRF

>-0.5 XRR

<-0.5 GRB

GRB021211/SN 2002lt

67Levan et al. 2005

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Garnavich et al. 2003

GRB 011121 IIn?

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Soderberg et al. 2005

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XRF 040701 fainter than 2002ap/SN 1994I by 3-6 mag (i.e. MV ~ -13/-15)

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1. It is not clear whether or not only Hypernovae are capable to produce GRBs or also “standard” Ib/c events can do it (IIn??)

2. The distributions of the absolute mag at max of GRB/SNe and standard Ibc are statistically indistinguishable effect of scanty statistic? they derive from the same SN population? (very heterogeneous class of objects)

• All GRB-SNe which have received a spectroscopic confirmation belong to the bright tail of Ibc distribution observational bias ?

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

• Rate for Ib/c: 0.22 SNu (Cappellaro et al. 1999)

1.2 x 108 LB, Mpc-3 (Madau, Della Valle & Panagia 1998)

2.6 x 104 SNe-Ibc Gpc-3 yr-1

• HYPs/Ibc ? (No absolute rate from controlled time surveys) 5-10% Podsiadlowski et al. 2004, Della Valle 2005

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Rates of GRBs Local rate:

0.5-1 GRB Gpc-3 yr-1 (Schmidt 2001, Guetta et al. 2004)

0.04-0.4 Gpc-3 yr-1 (Firmani et al. 2004)

0.01 Gpc-3 yr-1 (Matsubayashi et al. 2005)

2.6x104 SNe-Ibc Gpc-3 yr-1

<fb-1> ~500 (Frail et al. 2001)

<fb-1> ~75 (Guetta, Piran & Waxman 2004)

GRB/Hyp: 25%-4%

GRB/SNe-Ibc: 2%-0.3%

GRB/Hyp ~ 0.1, IF <fb-1> ~ 200

GRB/Hyp ~ 1, IF <fb-1> ~ 2000

GRB+XRR+XRF/SNe-Ibc ~ 1, IF <fb-1> ~30000

Soderberg, Nakar & Kulkarni 2005

Radio survey on 74 Ibc+Optical Rau et al. 2006

Podsiadlowski et al. 2004

GRB/Hyp ~1

< 1200

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Radio light curves of HNe

Soderberg et al.2006

Only GRB-SNe show strong radio emission.

No-GRB-HNe, like 2002ap, do not.

Either no jets or low-density environments.

The presence of relativistic jets is the mark between GRB/XRF-HNe and ordinary SNe/HNe

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Discussion and Conclusions

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1. Long duration GRBs are closely connected with the death of massive stars. Spectroscopic observations have been carried out over a large range of redshifts (z=0.008 1998bw; z=0.03 2006aj z=0.1 2003lw; z=0.16 2003dh; z=0.23 XRF 020903; z=0.6 GRB 050525a and possibly up to z~1, 2002lt).

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2. Only a very small fraction of all massive stars appears capable to produce GRBs. SNe-Ib/c are the natural candidates because of the lack of H envelope. However, this does not seem to be sufficient: only ~ 1% of SNe-Ibc (~10% of Hyps) produce GRBs. Some special circumstances are requested to the GRB star progenitor besides being “only” a massive star (Rotation, e.g. Woosley & Hegel 2006, Binarity, e.g. Podsiadlowski et al. 2004; Mirabel et al. 2003, Asymmetry Maeda et al. 2006). This point is not well understood (yet).

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3. The unification scheme where every SNe-Ibc is producing a GRB, XRR or XRF according to different viewed angles (e.g. Lamb et

al. 2005), is not favored by current estimates of SN/GRB rates and radio observations.

Unification works for <fb-1> ~ 30000 ( ~ 0o.5 )

HYP & GRB Rates give <fb-1> ~ 200 ( ~ 6o ) Radio Obs SNe-Ibc give <fb-1> < 1200 (or >

2o .5)

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Recent Results

GRB 050525A/SN 2005cn (Della Valle et al. 2006)

GRB060218/SN 2006aj (Campana et al. 2006)

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GRB 050525a: a new SN connection

Discovered by Swift

solid = 15-25 keV

dots = 25-50 keV

short dashed = 50-100 keV

long dashed = 100-350 keV

Blustin et al. 2005

z=0.606 Della Valle et al. 2006

E(B-V)=0.1 Blustin et al. 2005

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Follow-up at TNG, NTT and VLT+FORS2


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Hyp with short rising time on axis event (Maeda et al. 2006)

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+5 days

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+ 10 days

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Host galaxy of XRF060218/SN2006aj (DSS2)

z = 0.033

Mv (host) = -16

Host has brightnessSimilar to SMC

Z/Z ~ 0.3

Associated with SN 2006aj

(Masetti et al. 2006)

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Steep decline common

Gets shallower around here

Examples of Swift-XRT light curves

Nousek et al. 2005

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Campana et al. 2006

…in any type of SN triggered by core collapse, a shock is generated which propagates through the progenitor star and ejects the envelope. Accompanying the emergence of the shock wave through the surface of the star is a very bright UV/X burst of radiation… (A. Burrows 1992)

…the internal energy following an adiabatic expansion of the envelope leads to a luminosity peak at 1 day and 1% of the observed luminosity… (Colgate & White 1964)

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3 x104 km/s

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We have observed for the first time in a GRB a thermal

component which we have interpreted as signature of the

shock break-out (Colgate 60s)

We have caught a SN in the act of exploding (about 100s

after the collapse of the core)

We have definitely proved that SN and GRB are coeval

events

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Summary of SN-GRB time lag

GRB SN +t -t Ref.980425 1998bw +0.7 -2 Iwamoto et

al.

000911 Bump +1.5 -7 Lazzati et al.

011121 2001ke 0 -5 Bloom et al. + Garnavich et al

021211 2002lt +1.5 -3 Della Valle et

al.

030329 2003dh +2 0

-8-2

Kawabata et alMatheson

031203 2003lw 0 -2 Malesani et al.

041006 Bump 2 0 Stanek et al.

050525A 2005nc 2 0 Della Valle et al.

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Observations of SNe and bumps connected with GRBs imply that SNe and gamma bursts are

simultaneous events. This favors the collapsar model (Woosley 1993, Paczynski 1998, MacFadyen

& Woosley 1999) over competing theories (e.g. Supranova, Vietri & Stella 1998)

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We have observed for the first time in a GRB a thermal component which we have interpreted as signature of

the shock break-out (Colgate 60s)

We have caught a SN in the act of exploding (about 100s

after the collapse of the core)

We have definitely proved that SN and GRB are coeval events

We have measured the radius of the progenitor star, to be about 4 x 1011 cm which is typical of a W-R star.

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Jupiter

Red Supergiant

R~3x1013 cm

Blue Supergiant

R~4x1012 cm

Wolf-Rayet Star

R~4x1011 cm

SNe C-C (II, Ib, Ic)

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The properties of the 4 closest SNe associated with GRBs vary by at most 30%. The -budget covers about 4 order of magnitudes.

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a) we may be seeing intrinsically similar phenomena under different angles. GRB 030329/SN 2003dh may be viewed ~pole-on, GRB 980425/SN 1998bw considerably off-axis (15-30°, Maeda et al. 2005). GRB 031203/SN 2003lw may lie in between (Ramirez-Ruiz et al. 2005)

In this scenario the -properties are a strong function of the angle (E whereas the optical properties are not much influenced by this relative small spread in viewing angles.

b) GRB 060218/SN 2006aj there is an intrinsic dispersion in the properties of the relativistic ejecta for SNe with similar optical characteristics. relativistic energies at play in (local) GRB phenomenon (~ 1047- 1050 erg) are small compared to the KE involved in the “standard” SN-Ibc (1051 erg) or Hyp (1052 erg) explosions.

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HL-GRBs vs. LL-GRBs• HL-GRBs (-ray budget of 1051-52erg ~ SN/HN KE)• LL-GRBs (intrinsically faint 1047-49erg ~ 10-4/-2 SN KE)• Sampled volume 104-6 smaller Rate LL-GRBs: 20-500

x HL-GRBs rate (Della Valle 2006, Pian et al. 2006, Soderberg et al. 2006, Liang et al. 2006)

• LL-GRBs vs HL-GRBs properties of SN explosions?? • Different properties in the central engine (=compact

stellar remnant NS vs BH)?• Lack of tbreak implies (cfr. 5o-10o)• GRBs occur in star forming and low metallicity galaxies.

If they are sensitive to metallicity, we can expect systematic differences between nearby and cosmological GRBs (the latter produced in low-metallicity environments). e.g. GRB 050904 at z=6.3 (Kawai et al. 2005, Tagliaferri et al. 2005) is quite atypical (duration energy content, variability).

Nomoto et al. 2003

2006aj

SN-GRB Connection: Observations and Questions

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