The GLAST Burst Monitor (GBM) will enhance LAT observations of GRBs by extending the spectral coverage from the LAT threshold down to ∼8keV, and will provide a trigger for re-orienting the spacecraft to observe delayed emission from selected bursts outside the LAT field of view. GBM consists of twelve NaI scintillation detectors operating in the 8 keV to 1 MeV energy range and two BGO scintillation detectors operating in the 150 keV to 30 MeV energy range. Detector resolution, effective area, and angular response have been determined by calibrations. Analyses indicate that the on-board burst threshold will be ∼0.7photonscm-2s-1 and the on-board burst localization accuracy will typically be better than 8°. © 2008 American Institute of Physics.
Expected performance of the glast burst monitor / Meegan, Charles; Bhat, Narayana; Bissaldi, Elisabetta; Briggs, Michael; Connaughton, Valerie; Diehl, Roland; Fishman, Gerald; Greiner, Jochen; von Kienlin, Andreas; Kippen, R. Marc; Kouveliotou, Chryssa; Lichti, Giselher; Paciesas, William; Preece, Robert; Steinle, Helmut; Wilson-Hodge, Colleen. - ELETTRONICO. - 1000:(2008), pp. 573-576. (Intervento presentato al convegno Santa Fe Conference on Gamma-Ray Bursts 2007, GRB 2007 tenutosi a Santa Fe, NM nel November 5-9, 2007) [10.1063/1.2943535].
Expected performance of the glast burst monitor
Bissaldi, Elisabetta;
2008-01-01
Abstract
The GLAST Burst Monitor (GBM) will enhance LAT observations of GRBs by extending the spectral coverage from the LAT threshold down to ∼8keV, and will provide a trigger for re-orienting the spacecraft to observe delayed emission from selected bursts outside the LAT field of view. GBM consists of twelve NaI scintillation detectors operating in the 8 keV to 1 MeV energy range and two BGO scintillation detectors operating in the 150 keV to 30 MeV energy range. Detector resolution, effective area, and angular response have been determined by calibrations. Analyses indicate that the on-board burst threshold will be ∼0.7photonscm-2s-1 and the on-board burst localization accuracy will typically be better than 8°. © 2008 American Institute of Physics.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
