出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：Fermi Gamma-ray Burst Monitor (GBM) detects gamma-rays in the energy range 8 keV – 40MeV. Background fitting of the Fermi data is not trivial in some cases, especially when an Autonomous Repoint Request (ARR) is received. One good example is the burst 091030613 measured by the GBM, which cannot be fitted properly by a third-order polynomial of time. We present the background fitting of this burst for energy channels given in the CTIME data file. Our method is based on the motion of the satellite: we define three underlying parameters which depend on the actual position and orientation of the satellite and use them to fit the background. The main steps and results of this process are shown on the poster for the triggered NaI detector ’3’.
