GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) GRB Science with Next Generation Instrument Abe Falcone, David Williams, Brenda Dingus and GRB group

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Science Group Members: Buckley Dingus Falcone (Chair) Horan Krawczynski Meszaros Razzaque Williams (Associate Chair) (Other contributions will be welcomed)

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Direct GRB Studies 3 basic categories –<10 s (bulk of nominal prompt emission) – s (extended prompt & injection phase & early afterglow & flares) –>1000 s (afterglow & flares) Other Studies Lorentz invariance violation GRB remnants Cosmic Ray acceleration

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Nominal prompt emission Initial prompt emission is generally thought to be from internal shocks IC of MeV-keV emission should create GeV/TeV emission Can measure VHE cutoff energy and bulk Lorentz factor GLAST will beat us to this for GeV (~1 burst/year); Current ACTs << 1/year Wide range of Lorentz factors expected (~ ) Ground-based needed for GRBs with very high (>500) Lorentz factor All sky or VERY fast slewing needed to even look at many, AND probably need sensitivity >10x VERITAS (of course, with a low threshold)

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) sec ~4 Mechanisms: –More prompt emission; thought to be from internal shocks –external shock blast wave (i.e. nominal afterglow) –prolonged energy injection –Flares Again: IC of MeV-keV emission should create GeV/TeV emission; can measure VHE cutoff energy and bulk Lorentz factor Can map out jet/shock parameters --> refute/confirm current model NEED sens. >10x VERITAS to have a hope of seeing many bursts and to get a lightcurve Requirements on FOV and slew speed are somewhat relaxed

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Pre-Swift Anticipated X-ray Afterglow Behavior (GRB C, XRT observation) Simple power law decay Expected interesting behavior in spectra

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Typical XRT afterglow (Nousek et al. 2006, ApJ) Steep decline common (>60% of afterglows) Temporal break around 1000 s

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) The Canonical GRB “Afterglow” (Zhang et al. 2005) t -3 t –0.5 t –1 t –2

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Giant X-ray Flare: GRB B 500x increase! GRB Fluence: 8E-7 ergs/cm 2 Flare Fluence: 9E-7 ergs/cm 2 Falcone et al. 2006, ApJ Burrows et al. 2005, Science

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) sec ~4 Mechanisms: –More prompt emission; thought to be from internal shocks –external shock blast wave (i.e. nominal afterglow) –prolonged energy injection –Flares Again: IC of MeV-keV emission should create GeV/TeV emission; can measure VHE cutoff energy and bulk Lorentz factor Can map out jet/shock parameters --> refute/confirm current model NEED sens. >10x VERITAS to have a hope of seeing many bursts and to get a lightcurve Requirements on FOV and slew speed are somewhat relaxed, but bigger/faster gives more detections

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) >1000 s ~2 Mechanisms –More late flares –external shock blast wave IC still dominant, but pion decay could be significant Less flux, but higher likelihood that slewing instrument will react fast enough Probably need sensitivity >10 VERITAS; slewing at ~1deg/s would be good enough High duty factor from something like HAWC+ would help catch more but HAWC sensitivity would likely be insufficient Definitely need low threshold

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Lorentz Invariance Violation Energy dependent delays of simultaneously emitted photons can limit (or measure) Lorentz invariance Best lower limits to-date are from GRBs at keV/MeV energies; –0.0066E pl ~ 0.66×10 17 GeV Our major disadvantage: we can't see the distant GRBs due to IR absorption Our major advantage: High and broad energy range, especially if we measure a delay between GLAST - TeV Everyone's disadvantage: Inherent energy dependent delays With a detection of ~1 TeV photons by a >10x V/H/M sensitivity instrument and a detection by GLAST, the limit could be increased by ~100x (to ~E pl ), asumming a GRB like B at z=0.5 !!! (caveat: I need to check this calculation in more detail) Need a very sensitive (>10x VERITAS) instrument to create light curves

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) GRB remnants Could be unique science to ground-based gamma ray VERITAS will answer some of these questions first Problem: Not many of these are expected to be local (only 1-2) However, increased spatial and energy resolution could provide new science from Atoyan, Buckley, Krawczynski 2005

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Cosmic Ray Source While most GeV/TeV emission is expected to be IC, there is some component from p + synchrotron, p+γ initiated cascades, and inelastic n+p initiated cascades. The latter is thought to be dominant. If there is significant UHECR acceleration, then we could detect these BUT, like blazars, it will be difficult to break degeneracy between IC and hadronic –Have the advantage of better constraints on Lorentz factor and smaller timescales/regions May still need neutrinos

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Conclusions Most agree that we need more than just a single GRB detection to make a big science impact; a reasonable goal is ~10 GRBs/year Nearly all science goals require >10x VERITAS sensitivity AND low thresh. Nominal impulsive emission can only be captured with all sky (such as HAWC-like) or with a very fast (5-10 o /s) slewing ACT There are many possible sources of IC emission after the nominal prompt emission; not just the afterglow Detection after the first 10 sec is best served by a very sensitive (>10 x VERITAS) low threshold instrument CR acceleration can be addressed by the future, but firm conclusions may be hindered by IC/hadronic ambiguity Lorentz Invariance violation can be addressed at ~E pl by catching time variable emission with a >10x VERITAS sensitive instrument GRBRs have potential to be a unique source type that can be mapped out and spectrally characterized by a high sensitivity instrument

GRBs, Falcone et al.Next Generation Gamma White Paper Mtg. (St. Louis 2006) Status The actual writing has been stalled due to the overwhelming schedule of the Chair (Falcone), who admits to trying to do too much of the work himself Two solutions to get things moving: –David Williams has been enlisted share responsibilities of Chair with Falcone –More writing tasks to other members of group (Both of these solutions have been set in motion)