Coincident gray and gravitational wave observations Lee Samuel

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Coincident g-ray and gravitational wave observations Lee Samuel Finn Penn State University LIGO Scientific

Coincident g-ray and gravitational wave observations Lee Samuel Finn Penn State University LIGO Scientific Collaboration LIGO DCC G 020010 -Z 5 February 2002 SWIFT Science Team Meeting 1

Executive Summary • Principal g-ray burst models all involve violent formation of solar mass

Executive Summary • Principal g-ray burst models all involve violent formation of solar mass black hole – Progenitor uncertain (coalescence, collapse, …) – Where, when of g-ray producing shocks uncertain • Violent formation of black hole is a likely gravitational wave source – High-end LIGO band • f ~ 4 KHz (3 Msol/M) • Coincident grav. , g ray observations reveals details of burst model – Verify model, estimate gw conversion efficiency – From gravitational waves: nature of progenitor – From interval between grav. , g-ray burst: internal vs. external shocks • Impact – Observation scheduling to maximize overlap with LIGO antenna pattern LIGO DCC G 020010 -Z 5 February 2002 SWIFT Science Team Meeting 2

Science Impact • Observe association – Verify central feature of models – Estimate radiated

Science Impact • Observe association – Verify central feature of models – Estimate radiated gw power • Distinguish triggers via grav. rad. spectra Hypernovae; collapsars; NS/NS, NS/BH, He/BH, WD/BH mergers; AIC; … – Collapse: Peak grav. rad. spectral line l=2, m=0 – Coalescence: Peak spectral line l=2, m=+/– 2 g-rays generated by internal or external shocks • Internal vs. external shocks – Elapsed time between grav. , g-ray bursts ~0. 1 s for internal shocks, ~100 s for external Black hole + debris torus Relativistic fireball LIGO DCC G 020010 -Z 5 February 2002 SWIFT Science Team Meeting 3

Mission impact • Detector antenna pattern is quadrupolar – Earth doesn’t attenuate grav. waves

Mission impact • Detector antenna pattern is quadrupolar – Earth doesn’t attenuate grav. waves – Beam orthogonal to detector plane • In-beam more sensitive than uncoordinated observing – 10 x source rate at same threshold LIGO DCC G 020010 -Z 5 February 2002 SWIFT Science Team Meeting 4