Uncovering low-level Fermi/GBM emission using orbital background subtraction

2011/11/16 by Gerard Fitzpatrick, Fitzpatrick, Gerard, Valerie Connaughton +5 · 2 citations
Physics and Astronomy · #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #Instrumentation and Methods for Astrophysics (astro-ph.IM) #astro-ph.HE #astro-ph.IM

paper · pdf · doi:10.48550/arxiv.1111.3779

2011 Fermi Symposium proceedings - eConf C110509

arxiv created 2011/11/16 · arxiv updated 2011/11/17

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.

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