Uncovering low-level Fermi/GBM emission using orbital background subtraction
arXiv:1111.3779
Abstract
The secondary instrument onboard Fermi, the Gamma-ray Burst Monitor (GBM) is an all sky monitor consisting of 14 scintillation detectors. When analysing transient events such as Gamma-Ray Bursts (GRBs) and Solar Flares (SFs) the background is usually modelled as a polynomial (order 0-4). However, for long events the background may vary more than can be accounted for with a simple polynomial. In these cases a more accurate knowledge of GBM's background rates is required. Here we present an alternative method of both determining the background and distinguishing low-level emission from the instrumental background.
2011 Fermi Symposium proceedings - eConf C110509
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- A Low-latency Pipeline for GRB Light Curve and Spectrum using Fermi/GBM Near Real-time Data