Table 1.
Summary of data sets used to show the performance of the BG modelling method.
| Energy | Bin size | Nebins | Nobs | Texp | Type | BGRDB | Comments |
|---|---|---|---|---|---|---|---|
| 508–514 | 6.0 | 1 | 12 587 | 24.3 | Diffuse/line | o | Inner Galaxy / also weak point sources |
| 1795–1820 | 0.5 | 50 | 92 867 | 201.0 | Diffuse/line | a | Full sky |
| 2500–3500 | 1000.0 | 1 | 11 029 | 21.6 | Diffuse/continuum | a | Inner Galaxy |
| 50–100 | 2.0 | 25 | 3771 | 7.2 | Point-like/continuum | o | |
| 508–514 | 6.0 | 1 | 3771 | 7.2 | Point-like/continuum | o | Annihilation emission possible |
| 1790–1840 | 0.5 | 100 | 3771 | 7.2 | Point-like/continuum | o | No 26Al expected |
| 2500–3500 | 1000.0 | 1 | 3185 | 6.0 | Point-like/continuum | a | |
Notes. The first three columns define the analysed energy range, the chosen energy bin size in units of keV, and the resulting number of bins, Nebins. The fourth and fifth columns list the number of pointings, Nobs, and the resulting exposure time, Texp in units of Ms for a working detector, from the chosen observations. In the “Type” column, the expected emission types, diffuse vs. point-like and line vs. continuum emission, are listed. The “BGRDB” column shows which database was used to construct the background model, either per one INTEGRAL orbit (o) or per half a year (annealing, a). In the comments, additional characteristics of the data set or the expected emission are mentioned.
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