Table B.1
Point-like Fermi-LAT excesses found in the analysis above 1 GeV. Those excesses could be either new sources or diffuse emission not accounted for in our Galactic diffuse model.
| Source | (l, b) | Offset (°) | TS | Integrated flux (ph/cm2/s) | Γ |
|---|---|---|---|---|---|
| PS J1051.2-5931 | (288.224, -0.127) | 3.4 | 41.5 | (8.16 ± 1.50) · 10−10 | 2.68 ± 0.18 |
| PS J1111.5-5751a | (289.939, +2.463) | 3.4 | 29.2 | (5.89 ± 2.41) · 10−11 | 1.31 ± 0.17 |
| PS J1047.9-5943 | (287.943, -0.495) | 3.7 | 39.7 | (8.64 ± 1.74) · 10−10 | 2.40 ± 0.21b |
| PS J1046.1-5950 | (287.793, -0.710) | 3.8 | 90.0 | (1.75 ± 0.28) · 10−9 | 2.45 ± 0.12 |
| PS J1044.1-5922 | (287.353, -0.417) | 4.3 | 46.6 | (1.06 ± 0.20) · 10−9 | 2.51 ± 0.16 |
| PS J1043.1-5936 | (287.346, -0.682) | 4.3 | 113.4 | (1.97 ± 0.25) · 10−9 | 2.61 ± 0.11 |
| PS J1043.7-5851 | (287.060, +0.028) | 4.6 | 26.3 | (4.73 ± 1.16) · 10−10 | 2.27 ± 0.27b |
Notes. aAlthough we do not discuss associations with respect to the excesses, given the hardness of PS J1111.5-5751 we note that it is spatially consistent with the X-ray sources 1eRASS J111126.6-575208 and 1eRASS J111113.9-574927 (Merloni et al. 2024). bThese excesses were initially detected between 4σ and 5σ, therefore Γ is a fixed parameter in the ROI refit. The error provided is derived during the initial excess localization and not the final fit.
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