March 2006 GLAST DC2 Kickoff — 1 Algorithm for LAT On-board / On-ground GRB Trigger and Localization Jay Norris

March 2006 GLAST DC2 Kickoff — 2 On-ground Detection: Near threshold: GRB signal (5-10  ’s, 40 s, > 50 MeV), with 2 Hz bckgnd rate  1/300 count  -1 (  = sq. deg.), or 2 counts in 15° radius. For extended emission (~ 10 3 s) in a bright burst, the corresponding bckgnd total is ~ 50 counts, perhaps comparable to the signal. Recourse: more severe cuts, probably removing more low-energy signal. Use Likelihood. Notes: “2 Hz bckgnd” means total sky rate: sources + extragalactic & galactic diffuse + residual particle bckgnd. (Possibly higher with looser cuts for maximum GRB signal.) The Detection Problems - 1

March 2006 GLAST DC2 Kickoff — 3 The Detection Problems - 2 On-board Triggering: At threshold, GRB signal ~ 5-10  ’s in s (>50 MeV) Bckgnd rate ~ 600 Hz  40 s / 41,253  ~ 0.6 count  -1 Suppose GBM 2  radius ~ 10°  190 bckgnd count  -1 total in 40 s. Knowing GBM position facilitates on-board ID’ing of LAT GRB photons, but clearly … A localization will require additional cleverly divined filters applied to a GRB event buffer, to reduce the rate to ~ 60 Hz  20 bckgnd counts (further reducible on-board). This is a “worthy goal” for the on-board GRB filter chore.

March 2006 GLAST DC2 Kickoff — 4 Straightforward LAT GRB Detection & Localization Algorithm Philosophy (On-ground analysis): Usually, negligible bckgnd and only one source (the GRB) High-energy  ’s provide accuracy, but are less numerous. More low-energy  ’s, and they are “bunched in time.”  Optimal algorithm should be unbinned in time (thereby exploit bunching) and in space (exploit high-energy  ’s).* Starting from all-sky sample, algorithm should be able to bootstrap GRB position with very few false positives. *This same conclusion applies for on-board trigger/localization, but it is constraint of GBM position (rather than ground filters) that lowers the bckgnd rate sufficiently, AND pinpoints GRB onset (thereby greatly reducing N trials ).

March 2006 GLAST DC2 Kickoff — 5 {  s} : distances {  t} : intervals Event with smallest  s Swift/BAT z = 0.547

March 2006 GLAST DC2 Kickoff — 6  An N-event sliding window is used as the bootstrap step in searching for significant temporal-spatial clustering. Compute the Log {Joint (spatial*temporal) likelihood} for the tightest spatial cluster of events in the temporal sliding window: Log(P) =  Log{ [1 – cos(d i )] / [1 – cos(  max )] } +  Log{ 1 – exp(-R  t i ) }  Log(P) is measured against the near real-time bckgnd rate ( R ). Trigger threshold is also set as a function of the bckgnd, such that high GRB trigger efficiency is realized (events w/ 5-10  ’s detected), and formal expectation for false positive < /day.  Localization algorithm collects all events between 1 st and last windows which trigger within a time limit, ~ 150 s; computes an energy-weighted centroid. Probable particle events are ID’ed— by virtue of difference between actual and predicted distances from centroid—and then deweighted. Convergence: one iteration. Algorithm

March 2006 GLAST DC2 Kickoff — 7 On-board Trigger and Localization Sequence: Send LAT telemetry event stream to GRB processor. Apply additional filters, reduce background rate to ~ 60 Hz. Run spatial/temporal sliding-window trigger/localization algorithm. Option to utilize GBM trigger time and position to reduce windows. Telemeter localization and other GRB information to ground. Option to send alert message with ~ 10 highest energy GRB events to ground for rapid localization analysis. Implementation Some Adjustable/Variable Parameters: On-board / On-ground filters Nevents in sliding window(s); Nmove events per trial GBM positional uncertainty Inclusion radius (  threshold energy) for GRB  ’s “This” trigger-active search interval Trigger threshold(s) Nsigma distance threshold for deweighting putative particle events

March 2006 GLAST DC2 Kickoff — 8 Burst 2 Bckgnd rate = 32 Hz, 60-event sliding window Localization from 10 events telemetered for ground analysis. Events ID’ed using pseudo on- board recon, and GBM position. Localization from all 129 events ID’ed on ground (results same, w/ or w/o GBM position):  Ground ~ 1/2  Alert Red Circle: 10   est

March 2006 GLAST DC2 Kickoff — 9 Burst 3 Bckgnd rate = 32 Hz, 60-event sliding window Localization from 10 events telemetered for ground analysis. Events ID’ed using pseudo on- board recon, and GBM position. Localization from all 27 events ID’ed on ground (results same, w/ or w/o GBM position):  Ground ~ 1/2  Alert Red Circle: 10   est

March 2006 GLAST DC2 Kickoff — 10 dumbck = where(distset gt 2.*photerrs, nbck) if (nbck gt 0) then photerrs (dumbck) = distset(dumbck) W = 1. / photerrs W2 = W^2 Y = W2 * thetaset X = W2 * phiset * sin(thetaset) W2tot = total(W2) Xavg = total(X) / W2tot Yavg = total(Y) / W2tot One = sqrt(Nphots / (Nphots-1)) Fact = sqrt(max(W) / total(W)) errX = One * sqrt( total( ((X/W2 - Xavg)*W2)^2) / W2tot^2 ) * Fact errY = One * sqrt( total( ((Y/W2 - Yavg)*W2)^2) / W2tot^2 ) * Fact avgtheta = Yavg avgphi = Xavg / sin(avgtheta) errtheta = errY errphi = errX / sin(avgtheta) errrho = sqrt(errX^2 + errY^2) Error Estimation: Energy Weighting

March 2006 GLAST DC2 Kickoff — 11 Comparison: Ground vs. Alert vs. On-board T min T max {Azi, Polar}  est  true N  N >10MeV N >100MeV N >1GeV (Ground Recon) , (Ground Alert) , , (Ground Recon) , (Ground Alert) , , (Ground Recon) , (Ground Alert) , , Ground  true ~  Alert  true ~ 0.5  On-board  true

March 2006 GLAST DC2 Kickoff — 12  Algorithm unbinned in {time, space} utilizes most of the available information — On-board or On-ground. Fast. Probably sufficient for ID’ing photons in bursts of <~ 100 s duration. Extended emission (~ 10 3 s): use Likelihood.  GBM position and additional on-board filters necessary to reduce bckgnd rate, enable a “clean” LAT localization.  Alert to ground — containing ~ 10 highest energy LAT  ’s for “quicklook” analysis — probably better accuracy than on-board.  Lest we forget: The smallest possible LAT localization, delivered quickly to the community, means that larger ground-based telescopes can participate in afterglow searches at earlier epochs. Even past the Swift era, it is likely that spectroscopic redshifts will still be superior to “pseudo” redshifts (presently very immature) obtained from burst prompt emission properties. Know redshift  Know energetics. Summary