tokens: near T 0 . Figure 1. Results of the AGILE -GRID standard analysis for the three Sources A (upper panel), B (middle panel) and C (lower panel) of Table 1 . Left panels: gamma-ray lightcurves above 100 MeV around the IceCube T 0 . Right panels: maps in equatorial coordinates (J2000) of gamma-ray intensity above 100 MeV in (ph cm −2 s −1 sr −1 ) corresponding to the gamma-ray detection before T 0 shown on the left. The AGILE 95% confidence level (c.l.) location contours are shown in white; the IceCube error boxes or circles are shown in yellow. A systematic error of 01 should be added to each AGILE source determination. The positions of the classified AGNs from the BZCAT Catalog (Massaro et al. 2015 ) and the FERMI -LAT 3FGL gamma-ray sources (Acero et al. 2015 ) are shown in cyan and red, respectively. The standard AGILE data analysis indicates that in all cases the peak gamma-ray emission is similarly observed within 1–2 days from T 0 . For Sources B (IC-170321) and C (IC-170922), weak gamma-ray emission is also observed over longer integration timescales that include T 0 . In particular, for the new Source B an integration of 15 days, starting from 2017 March 15 (12:00 UT), shows a detection above 4 σ with a flux . The AGILE centroid has Galactic coordinates ( l , b ) = (224.59, −10.53) ± 0.42 (deg) (95% stat. c.l.) ± 0.1 (deg) (syst.) (R.A., decl. (J2000) = (98.58, −15.08) (deg)), and is fully compatible with the IceCube centroid (see Figure 2 ). Figure 2. Left panel: AGILE -GRID intensity maps, in (ph cm −2 s −1 sr −1 ) and equatorial coordinates (J2000), centered at the position of the IceCube event IC-170321, over a long integration time of 15 days around T 0 (( T 0 − 6; T 0 + 11) days). The AGILE 95% c.l. location contour obtained with the AGILE standard analysis is shown in white, the IceCube error box in yellow. Right panel: AGILE -GRID 7 day time bin gamma-ray lightcurve ( E > 100 MeV) around T 0 , obtained from the AGILE standard analysis performed at the IC-170321 position. 2.1. Post-trial False Alarm Probability To evaluate the probability that each of these three gamma-ray sources is associated with the neutrino events by chance, we first evaluated the FAR for an AGILE QL detection per unit time δt and per unit solid angle δ Ω. As the unit time δt , we assumed the standard integration time of the QL maps ( δt = 2 days). For δ Ω, we assumed the solid angle subtended by a cone with half-aperture matching the standard circular radius of 15 used in the database search ( δ Ω ≃ 2.15 × 10 −3 sr). 22 22 See Appendix A for details of the FAR computation. We then estimated the post-trial false alarm probability P i of a random occurrence in space and time of a neutrino and a gamma-ray transient event separated by an interval Δ t and by the solid angle ΔΩ (corresponding to the angular distance Δ θ ) as (Connaughton et al. 2016 )where N i is the number of trials for a symmetric time window, is the FAR per 2 day map and per unit solid angle for
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