The IGC GRB-SN family: the cases of GRB 130427A and GRB...
Transcript of 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
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
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 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
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 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
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 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
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!
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
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!
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