the igc grb-sn family: the cases of grb 130427a and grb...

The IGC GRB-SN family:The IGC GRB-SN family:the cases of GRB 130427A and GRB 060614the cases of GRB 130427A and GRB 060614

Giovanni B. PisaniGiovanni B. Pisanisupported by the Erasmus Mundus Joint Doctorate Programsupported by the Erasmus Mundus Joint Doctorate Program

by Grant Number 2011-1640 from the EACEA of the European Commissionby Grant Number 2011-1640 from the EACEA of the European Commission

in collaboration with C.L. Bianco, M. Enderli, L. Izzo,in collaboration with C.L. Bianco, M. Enderli, L. Izzo,M. Kovacevic, M. Muccino, A.V. Penacchioni, J.A. Rueda and Y. WangM. Kovacevic, M. Muccino, A.V. Penacchioni, J.A. Rueda and Y. Wang

under the supervision of R. Ruffiniunder the supervision of R. Ruffini

2727thth Texas Symposium on Relativistic Astrophysics, 8-13 Dec 2013 Texas Symposium on Relativistic Astrophysics, 8-13 Dec 2013

GRB - supernova associationGRB - supernova association

GRB 980425 / SN 1998bw (Type Ic)GRB 980425 / SN 1998bw (Type Ic)

z = 0.0085

Galama et al. 1998Galama et al. 1998

GRB 030329 / SN 2003dhGRB 030329 / SN 2003dh

Hjorth et al. 2003Hjorth et al. 2003

Malesani et al. 2004Malesani et al. 2004

GRB 031203 / SN 2003lwGRB 031203 / SN 2003lw““smoking-gun”smoking-gun”

GRB - supernova associationGRB - supernova association

Izzo et al. 2012Izzo et al. 2012

Cano et al. 2010Cano et al. 2010

Eiso = 2.8 1053 erg

z = 0.54

The IGC GRB - SN source prototype: GRB 090618The IGC GRB - SN source prototype: GRB 090618

- Binary system in its f- Binary system in its f inal evolution inal evolution stage, composed of an evolved stage, composed of an evolved massive star and a neutron star (NS)massive star and a neutron star (NS)

- The evolved star, - The evolved star, likely a Carbon-likely a Carbon-Oxygen (CO) star or an evolved Wolf-Oxygen (CO) star or an evolved Wolf-Rayet star, explodes as a SN Ib/cRayet star, explodes as a SN Ib/c

- The SN explosion leads to a - The SN explosion leads to a subrelativistic expansion of its outer subrelativistic expansion of its outer layerslayers

- Part of the expelled material is - Part of the expelled material is accreted by the NS accreted by the NS companion, that companion, that very fast reaches the critical mass very fast reaches the critical mass and and collapses to a Black Hole (BH)collapses to a Black Hole (BH)

- During this gravitational collapse a - During this gravitational collapse a canonical GRB is emittedcanonical GRB is emitted

- The SN core collapses into a newly-- The SN core collapses into a newly-born NSborn NS

Induced Gravitational Collapse (IGC) scenarioInduced Gravitational Collapse (IGC) scenario

IGC GRB - SN eventsIGC GRB - SN events

Rueda & Ruffini 2012Rueda & Ruffini 2012

Ruffini et al. 2001, 2007Ruffini et al. 2001, 2007

Nonrelativistic Nonrelativistic expansion of the expansion of the

outer layers of the outer layers of the exploding SNexploding SN

Emission of the Emission of the GRB in coincidence GRB in coincidence with the formation with the formation of the BH from of the BH from the the collapse of the NScollapse of the NS

Emission of the newly-Emission of the newly-born NS generated by born NS generated by the SN core collapsingthe SN core collapsing

Optical Optical emissionemissionof the SNof the SN~~10 days 10 days

after the burstafter the burst

EPISODE 1

EPISODE 2

EPISODE 4

EPISODE 3

The IGC GRB - SN source prototype: GRB 090618The IGC GRB - SN source prototype: GRB 090618

GRB 101023GRB 101023GRB 101023GRB 101023

EPISODE 1EPISODE 1

EPISODE 2EPISODE 2

z = 0.9

Penacchioni et al. 2012Penacchioni et al. 2012

GRB 110709BGRB 110709B

EPISODE 1EPISODE 1 EPISODE 2EPISODE 2

GRB 110709BGRB 110709B

z = 0.75

Penacchioni et al. 2013Penacchioni et al. 2013

Sample of IGC GRB-SN sourcesSample of IGC GRB-SN sources

GRBGRB zz Eiso (erg)Eiso (erg) SNSN Episode 1Episode 1

060729 0.54 1.6 ∙ 1052 photometric possible

061007 1.261 1.2 ∙ 1054 too far yes

080913B 0.937 1.4 ∙ 1054 photometric possible

090618 0.54 2.8 ∙ 1053 photometric yes

091127 0.49 1.4 ∙ 1052 SN 2009nz possible

111228 0.713 2.3 ∙ 1052 photometric yes

101023 0.9 * 1.3 ∙ 1053 no data yes

110709B 0.75 * 2.7 ∙ 1053 no data yes

Pisani et al. 2013Pisani et al. 2013

THE GOLDEN SAMPLETHE GOLDEN SAMPLE

An universal behavior of rest-frame X-ray luminosity after 20An universal behavior of rest-frame X-ray luminosity after 20 000 s000 s

THE GOLDEN SAMPLETHE GOLDEN SAMPLE

Pisani et al. (submitted)Pisani et al. (submitted)

Pisani et al. 2013Pisani et al. 2013

We are currently testing the predictive power of this result in 3 different cases:We are currently testing the predictive power of this result in 3 different cases:

1)1) GRBs at redshift z > 1 GRBs at redshift z > 1in this case we can predict the existence of a SN in such a system, expected to in this case we can predict the existence of a SN in such a system, expected to emerge after a time of emerge after a time of ~~ 10 ( 1 + z ) days, the canonical time sequence of a SN 10 ( 1 + z ) days, the canonical time sequence of a SN explosion. This offers a new challenge to detect SNe at high redshiftexplosion. This offers a new challenge to detect SNe at high redshift

2)2) GRBs at redshift z < 1 GRBs at redshift z < 1we can indicate in advance, from the X-ray luminosity light curve observed by we can indicate in advance, from the X-ray luminosity light curve observed by XRT, the expected time for the observations of a SN and alert direct XRT, the expected time for the observations of a SN and alert direct observations from on-ground and space telescopesobservations from on-ground and space telescopes

3) GRBs with no measured redshift3) GRBs with no measured redshiftwe can infer the redshift of the GRBs as done for GRB 110709B andwe can infer the redshift of the GRBs as done for GRB 110709B andGRB 101023AGRB 101023A

GRB 130427A: a monster just around the cornerGRB 130427A: a monster just around the corner

z = 0.34

Levan et al. 2013Levan et al. 2013

Xu et al. 2013Xu et al. 2013

Flores et al. 2013Flores et al. 2013

Eiso ~ 1054 erg

Golenetskii et al. 2013Golenetskii et al. 2013

GRB 130427A: late X-ray luminosity overlap with GRB 060729GRB 130427A: late X-ray luminosity overlap with GRB 060729

Ruffini et al. (in preparation)Ruffini et al. (in preparation)

GRB 130427A / SN 2013cq

z = 0.34

Eiso ~ 1054 erg

GRB 060729

z = 0.54

Eiso = 1.6 · 1052 erg

Ruffini et al., GCN 14526Ruffini et al., GCN 14526

22ndnd May 2013 May 2013

GRB 130427AGRB 130427A

Episode 1 Episode 2

Initially indicated isotropic energy

Eiso = 2.4x1051 erg

for redshift z = 0.125, determined from the host galaxy

Episode 3

GRB 060614: the puzzling absence of an associated SNGRB 060614: the puzzling absence of an associated SN

Price et al. 2006, GCN 5275Price et al. 2006, GCN 5275

Fynbo et al. 2006Fynbo et al. 2006

Associated SN shouAssociated SN should be ~ 100 times less luminous tld be ~ 100 times less luminous than the typical one !han the typical one !

GRB 060614: the puzzling absence of an associated SNGRB 060614: the puzzling absence of an associated SN

Della Valle et al. 2007Della Valle et al. 2007

GRB 060614: is z = 0.125 the correct redshift?GRB 060614: is z = 0.125 the correct redshift?

Cobb et al. 2006Cobb et al. 2006

Atteia Relation z = 1.45 Atteia Relation z = 1.45 ±± 0.85 0.85

Combined X-ray UV O spectral analysis z < 1.3Combined X-ray UV O spectral analysis z < 1.3

Pelangeon & Atteia 2006, GCN 5265Pelangeon & Atteia 2006, GCN 5265

Gehrels et al. 2006Gehrels et al. 2006

Probability of a chance superpositionProbability of a chance superpositionof the purpoted host galaxy along the ~0.5%–1.9% of the of the purpoted host galaxy along the ~0.5%–1.9% of the SwifSwift GRB sample t GRB sample line of sight of GRB 060614 line of sight of GRB 060614

Current Current SwiftSwift sample counts ~700 GRBs between 3 and 13 of such occurrences! sample counts ~700 GRBs between 3 and 13 of such occurrences!

GRB 060614 z = 0.125

GRB 090618 z = 0.54

GRB 060614GRB 060614

Della Valle et al. 2006Della Valle et al. 2006Fynbo et al. 2006Fynbo et al. 2006

Gal-Yam et al. 2006Gal-Yam et al. 2006No supernova !No supernova !

GRB 060614 z = 0.125

GRB 090618 z = 0.54

GRB 060614: comparison with IGC X-ray luminosity prototypeGRB 060614: comparison with IGC X-ray luminosity prototype



GRB 060614 z = 0.125

GRB 060614 z = 1.2

GRB 090618 z = 0.54

GRB 060614 in the IGC paradigm: a higher redshiftGRB 060614 in the IGC paradigm: a higher redshift

Ruffini et al. GCN 15560Ruffini et al. GCN 15560



GRB 060614 z = 0.125

GRB 060614 z = 1.2

GRB 060614 in the Amati relationGRB 060614 in the Amati relation

Ruffini et al. GCN 15560Ruffini et al. GCN 15560

SummarySummary

We found a common late X-ray behaviour for energetic GRBs-SNeWe found a common late X-ray behaviour for energetic GRBs-SNe

Predictive power:Predictive power: the occurrence of SNe associated to near enough GRBsthe occurrence of SNe associated to near enough GRBs energetic GRBs-SNe distances when not measuredenergetic GRBs-SNe distances when not measured

Theoretical interpretation: Induced Gravitational Collapse paradigmTheoretical interpretation: Induced Gravitational Collapse paradigm energetic GRBs-SNe progenitors are binaries!energetic GRBs-SNe progenitors are binaries!

SummarySummary

Enlarge the sample in order to increase the statistical validity of this approach as Enlarge the sample in order to increase the statistical validity of this approach as well as its cosmological implicationswell as its cosmological implications

Look for other observational tests for the IGC scenarioLook for other observational tests for the IGC scenario

Clarify the mechanism behind the common late X-rays decayClarify the mechanism behind the common late X-rays decay




What still remains to do?What still remains to do?

SummarySummary

Enlarge the sample in order to increase the statistical validity of this approach as Enlarge the sample in order to increase the statistical validity of this approach as well as its cosmological implicationswell as its cosmological implications

Look for other observational tests for the IGC scenarioLook for other observational tests for the IGC scenario

Clarify the mechanism behind the common late X-rays decayClarify the mechanism behind the common late X-rays decay




What still remains to do?What still remains to do?

Thanks for your attentionThanks for your attention

optically thick plasma optically thick plasma of eof e±± at thermal at thermal

equilibrium withequilibrium withtotal energy Etotal energy Eee±±

gravitational gravitational collapse to a collapse to a Black HoleBlack Hole

gradual gradual annihilation annihilation

confined in a confined in a relativistically relativistically

expanding shellexpanding shell

engulfing of the engulfing of the left over barionsleft over barions

B = MB = Mbbcc2 2 / E/ Eee±±

at transparencyat transparencyP-GRBP-GRB is emitted is emitted

accelerated barions accelerated barions interact with the interact with the

circumburst medium circumburst medium giving rise to the giving rise to the

Extended AfterglowExtended Afterglow

Fireshell modelFireshell model

Fireshell modelFireshell model

Enlarging the family Enlarging the family (before (before SwiftSwift-XRT)-XRT)

GRB 030329 / SN 2003dhz = 0.168

Eiso ~ 2·1052 erg

GRB 970828z = 0.958Eiso = 1.60·1053 erg

Izzo et al. 2012Izzo et al. 2012

the igc grb-sn family: the cases of grb 130427a and grb...

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