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Non-thermal emission from Gamma-Ray Burst SNe

Non-thermal emission from Gamma-Ray Burst SNe. X-rays. RADIO. …the Science across the rainbow…. Raffaella Margutti Harvard University. GRB- SNe. Non-thermal emission: --Tracks the fastest ejecta --Properties of the jet. --Tracks the slow ejecta

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Non-thermal emission from Gamma-Ray Burst SNe

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  1. Non-thermal emission from Gamma-Ray Burst SNe X-rays RADIO …the Science across the rainbow… Raffaella Margutti Harvard University

  2. GRB-SNe Non-thermal emission: --Tracks the fastest ejecta --Properties of the jet --Tracks the slow ejecta -- Properties of the progenitor (Mej, M_Ni) γ-rays Log (Lum) X-rays RADIO Optical-UV OPTICAL AFTERGLOW Log (Time) 40 days 10-20 days 5-1000 s 0.1 d 1 d

  3. CE SN Isotropic emission GRB-jet Early-time X-rays Jet deceleration Optical - X-ray + RADIO afterglow

  4. GRB-SNe NON THERMAL EMISSION --Tracks the fastest ejecta --Properties of the jet γ-rays Log (Lum) RADIO X-rays CE Optical-UV 40 days 10-20 days 1 d

  5. What’s peculiar about GRB-SNe? Hypernovae (Type Ic) Relativistic (Soderberg 2010) SN2009bb SN2002ap SN1994I Broad Line SN

  6. Hydrogen Poor Super Luminous SNe (e.g. Gal-Yam 2012) 7x1043 erg/s PS1-10kw PS1-10awh 2007bi Hypernovae (Type Ic) Relativistic ejecta (Soderberg ref) SN2009bb SN2002ap SN1994I Broad Line SN (ref)

  7. Asymmetric MNi Mazzali 2005 Sanders 2012 Large vphot Hjorth 2011

  8. Energy partitioning Relativistic Soderberg 2006

  9. γ-rays OPTICAL 980425 (1998bw) 120422A (2012bz) 20 0 100316D (2010bh) 060218 (2006aj)

  10. X-rays 980425/1998bw 030329/2003dh 031203/2003lw 060218/2006aj 091127/2009nz 100316D/2010bh 120422A/2012bz 0.001 Cosmological 0.01 t-(1.5or 2) t-1 t-0.2 Sub-luminous

  11. X-rays 12bz Mildly Relativistic (Soderberg 2010) Non-GRB

  12. SUPERNOVAE Radio GAMMA-RAY BURSTS 030329(2003dh) 031203 (2003lw) 980425(1998bw) 060218 (2006aj) Sanders 2012 100316D (2010bh)

  13. Xrays-Radio X-rays Cosmological GRBs (including 030329/2003dh) 2009bb Relativistic 100316D (2010bh) Radio 060218 (2006aj) 2008D Common Ibc Explosions

  14. Take-away list: 1. Late-time X-rays clearly distinguish GRB/SNe also from relativistic SNe with much brighter radio emission

  15. Xrays Late time (0.5-10 days) temporal DECAY RATE <1 keV dN ≈ ν-Γ Average decay= 1.5 SPECTRUM 060218 (2006aj) 100316D (2010bh) 060218 (2006aj) 100316D (2010bh) • SLOW late-time decay Typical Index= 2 • EXCEPTIONALLY SOFT X-ray emission

  16. EngineOFF EngineON MILD decay + Extremely SOFT emission 100316D/2010bh Ambient medium interaction Slower blob Collision Faster blob EXTERNAL SHOCK Central engine STANDARD GRB MODEL Synchrotron Pre Burst Prompt Emission Afterglow

  17. Synchrotron emission Fireball Dynamics 060218 (2006aj) 100316D (2010bh) WIND, slow cooling ISM, slow cooling ISM, WIND Jet Spreading Not synchrotron Granot 2002

  18. Take-away list: 1. Late-time X-rays clearly distinguish GRB/SNe also from relativistic SNe with much brighter radio emission … 2. …BUT they are NOT consistent with synchrotron emission from the deceleration of the GRB jet in the ambient medium (different from GRBs)

  19. 100316D/ 2010bh Synchrotron X-rays Radio Radio SED, t=36 days X-rays

  20. Take-away list: 1. Late-time X-rays clearly distinguish GRB/SNe also from relativistic SNe with much brighter radio emission … 2. …BUT they are NOT consistent with synchrotron emission from the deceleration of the GRB jet in the ambient medium (different from GRBs) 3. There is evidence for an EXCESS of X-ray emission with respect to the synchrotron model

  21. Inverse Compton:: ρ 100316D/2010bh Donor Star X-rays SN EXPLOSION X-rays 1014 1015 e- 1016 R Inverse Compton emission e- 10 days e- Shock 37 days e- X-rays Photosphere e- X-rays 37 days

  22. Take-away list: 1. Late-time X-rays clearly distinguish GRB/SNe also from relativistic SNe with much brighter radio emission … 2. …BUT they are NOT consistent with synchrotron emission from the deceleration of the GRB jet in the ambient medium (different from GRBs) 3. There is evidence for an EXCESS of X-ray emission with respect to the synchrotron model 4. The X-ray EXCESS of emission is not consistent with IC (up-scattering of the SN optical photons by the SN shock )

  23. Accretion on BH 100316D/2010bh CE Inverse Compton emission 10 days 37 days Magnetar spin-down

  24. Take-away list: 1. Late-time X-rays clearly distinguish GRB/SNe also from relativistic SNe with much brighter radio emission … 2. …BUT they are NOT consistent with synchrotron emission from the deceleration of the GRB jet in the ambient medium (different from GRBs) 3. There is evidence for an EXCESS of X-ray emission with respect to the synchrotron model 4. The X-ray EXCESS of emission is not consistent with IC (up-scattering of the SN optical photons by the SN shock ) 5. We suggest that this is emission from the CE (Magnetar or BH). Whatever is the physical source, our analysis indicates that this emission is NOT strongly beamed

  25. Very nearby GRB/SN Cosmological GRBs GRB jet Jet Jet CE X-rays CE CE Thanks! -- Nearby -- Less powerful jets

  26. Take-away list: 1. Late-time X-rays clearly distinguish GRB/SNe also from relativistic SNe with much brighter radio emission … 2. …BUT they are NOT consistent with synchrotron emission from the deceleration of the GRB jet in the ambient medium (different from GRBs) 3. There is evidence for an EXCESS of X-ray emission with respect to the synchrotron model 4. The X-ray EXCESS of emission is not consistent with IC (up-scattering of the SN optical photons by the SN shock ) 5. We suggest that this is emission from the CE (Magnetar or BH). Whatever is the physical source, our analysis indicates that this emission is NOT strongly beamed

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