Electromagnetic Counterparts I M. Benacquista ICE Summer School: Gravitational Wave Astronomy July 3, 2018
What is an electromagnetic counterpart? • Source of gravitational waves • Source of electromagnetic waves • Coincident in time (Events) • Mergers Today • Supernovae • Coincident in space (Continuous) • Compact Binaries • Pulsars • Statistically correlated (Long Delay) • Binary SMBH Thursday • Tidal Disruptions ICE Summer School: Gravitational Wave Astronomy � 2 July 3, 2018
・ ・ ✓ “ hree generic phases” ✓ ✓ Electromagnetic Counterparts of Supernovae especially when convection dominates over SASI. ✓ The horizon of LIGO is limited to nearby events. Kei Kotake: LVC Workshop on CCSN: wiki.ligo.org/LSC/2017SupernovaeWorkshop × Anisotropic instabilities can generate time varying quadrupole moments R s ∼ 3 km ( M ⊙ ) 2 v R ( c ) M h ij ∼ ϵ R s v c ∼ 0.1 degree of anisotropy ϵ ∼ 10 − 4 − 10 − 12 ICE Summer School: Gravitational Wave Astronomy � 3 July 3, 2018
• Unmodeled signal detection • Coherent analysis over network of detectors • Typical best distance is a few 100 pc • How many are there? Mukherjee et al. PRD 96 104033 (2017) ICE Summer School: Gravitational Wave Astronomy � 4 July 3, 2018
ICE Summer School: Gravitational Wave Astronomy � 5 July 3, 2018
Core Collapse Supernovae • Neutrino burst coincident with gravitational wave burst • EM burst due to shock break out ~ hours/days later • Signal detection limits to only nearby events ~ 200 pc • Very rare events at this distance (1 per 1000yrs) • Unlikely to have to search for EM counterparts • Probably a good thing ICE Summer School: Gravitational Wave Astronomy � 6 July 3, 2018
Electromagnetic Counterparts of Mergers Needs: • Matter to couple to photons • Neutron star • Ejection of matter • Energy source to generate those photons • Accretion • Disk shocking • Radioactive decay (r-process) • Prompt emission • Jet breakout — γ -ray burst • Sustained afterglow • Radioactive decay • Disk opacities • Jet expansion ICE Summer School: Gravitational Wave Astronomy � 7 July 3, 2018
Rosswog+Ramirez-Ruiz(2002) M unbound ∼ 5 × 10 − 3 − 5 × 10 − 2 M ⊙ v unbound ∼ 0.1 − 0.3 c ICE Summer School: Gravitational Wave Astronomy � 8 July 3, 2018
• Neutron rich material and heavy nuclei • Nucleus can absorb a neutron • Probability (time-scale) depends on the density of neutrons τ absorb • Nucleus can decay through β -decay • Probability (time-scale) depends on the nucleus τ decay • r-process: τ absorb < τ decay • s-process τ absorb > τ decay ICE Summer School: Gravitational Wave Astronomy � 9 July 3, 2018
120 e c n a d n u b a s s e c o r 100 p - r 0 0 2 0 8 1 80 Proton number ( Z ) 160 1 0 1 ) A ( r 140 e b m N r , (Si = 10 6 ) u 0 0 n 1 s 0 s 60 2 a 1 M –1 log( T s –1 ) 0 0 0 1 1 1.0 0 –2 8 0 1 40 0.5 0.0 –0.5 –1.0 20 –1.5 –2.0 –2.5 00 20 40 60 80 100 120 140 160 Neutron number ( N ) ICE Summer School: Gravitational Wave Astronomy � 10 July 3, 2018
Nuclear Evolution of the Debris r-process network: neutron captures, photo-dissociations, alpha- and beta-decays, fission reactions Lattimer+Schramm1976, Freiberghaus+99, Goriely+2011, Metzgert+2010, Roberts+2011, Korobkin+2012 ICE Summer School: Gravitational Wave Astronomy � 11 July 3, 2018
Lightcurves Change in internal energy of the debris dU dt = − U t − U + L heat τ d nuclear decay adiabatic 1 ) radiation 41 10 Luminosity (erg s τ d = ( 1/2 ( v unbound ) 1/2 4 π c ) M unbound 3 κ 40 10 diffusion timescale 39 10 0 0 1 1 2 2 3 3 4 4 5 5 6 6 7 7 8 8 9 9 Time (days) ∼ 1 day rise ( v unbound ∼ 0 . 1 c , M unbound ∼ 10 � 2 M � , κ ∼ 0 . 1 cm 2 g � 1 ) ICE Summer School: Gravitational Wave Astronomy � 12 July 3, 2018
ICE Summer School: Gravitational Wave Astronomy � 13 July 3, 2018
Spectral Lines ICE Summer School: Gravitational Wave Astronomy � 14 July 3, 2018
Finding the counterpart ~ 30 square degrees ICE Summer School: Gravitational Wave Astronomy � 15 July 3, 2018
DECam Image—9 square degrees ICE Summer School: Gravitational Wave Astronomy � 16 July 3, 2018
Catalog of galaxies (GWGC) out to ~100 Mpc ICE Summer School: Gravitational Wave Astronomy � 17 July 3, 2018
ICE Summer School: Gravitational Wave Astronomy � 18 July 3, 2018
ICE Summer School: Gravitational Wave Astronomy � 19 July 3, 2018
1M2H team (UCSC+Carnegie) ICE Summer School: Gravitational Wave Astronomy � 20 July 3, 2018
ICE Summer School: Gravitational Wave Astronomy � 21 July 3, 2018
kilonova SSS17a bolometric light curve radioactivity: Lippuner & Roberts 2015 Q(t) of 0.02 M sun ICE Summer School: Gravitational Wave Astronomy � 22 July 3, 2018
What was our viewing angle? ICE Summer School: Gravitational Wave Astronomy � 23 July 3, 2018
Margutti et al. 2018 Figure 8. Evolution of the X-ray emission from GW170817 as seen by the CXO . ICE Summer School: Gravitational Wave Astronomy � 24 July 3, 2018
O ff -axis view of jet breakout into interstellar medium leads to late-time brightening across all wavelengths Margutti et al. 2018 ICE Summer School: Gravitational Wave Astronomy � 25 July 3, 2018 a - q q µ t r k � - = » - k » - - - = � ´ - - - �
Further detections: • Learn about the r-process and s-process development. • Learn about the disk opacities of Lanthanides. • Learn about the jet break-out mechanism • Learn about the angle of opening of the jet • Gives us the rate of "invisible" GRBs ICE Summer School: Gravitational Wave Astronomy July 3, 2018
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