Table 3
Default parameters for built-in HE detectors.
| Detector | Energy range (keV) | Flux limit | FoV (percentage) | fc |
|---|---|---|---|---|
| Compton-BATSE | 50–300 | 0.3 phs cm−2 s−1 | 25% | 1 |
| Swift/BAT | 15–150 | 1.5 phs cm−2 s−1 | 10% | 2 |
| Fermi/GBM | 10–1000 | 2.28 phs cm−2 s−1 | 60% | 2 |
| Insight-HE(1) | 30–250 | 2 × 10−8 ergs s−1 cm−2 | 60% | 1 |
| GECAM(2) | 15–5000 | 1.8 × 10−8 ergs s−1 cm−2 | 30% | 1 |
Notes. The Swift/BAT and Fermi/GBM flux limits as well as the Fermi/GBM energy range differ from their theoretical specified values. We follow Coward et al. (2012) and realise that it is more difficult for a sGRB to be detected as it needs to produce a significant signal over a short amount of time. As such, we use the lowest value for the peak flux in the sGRB catalogues (Lien et al. 2016 for Swift/BAT, von Kienlin et al. 2014, von Kienlin et al. 2020; Gruber et al. 2014; Bhat et al. 2016 for Fermi/GBM) of each of these instruments, in the shortest time accumulation window (20 ms for Swift/BAT, and 64ms for Fermi/GBM where flux for the latter was given within 10–1000 keV). More HE detectors will be added to the GWToolbox in the future.(1) While we include Insight-HE in our list here, we leave this instrument out of our analysis; as its published GRB catalogue is currently incomplete, we are not able to extract an effective flux threshold at which it operates at the present time. Similarly to Fermi/GBM and Swift/BAT, using the theoretical threshold does not lead to accurate detection rates for sGRBs.(2) The designed FoV of GECAM is 100%, however, due to a power problem, the actual on-orbit FoV had been only about ~30% for the past year. During the preparation of this manuscript, we learnt that the FoV has been restored to ~60% recently from a private conversation.
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