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Fig. 6


Combined 3σ upper limit on the non-detection of the electromagnetic counterpart of LVT151012 derived by using the all sky observations of SPI-ACS, IBIS/Veto, IBIS/PICsIT, and IBIS/ISGRI. The color map indicates the upper limit values in different sky regions. We assumed here the case of a 1 s impulsive event with a spectral energy distribution described by the Comptonized model introduced in Sect. 2. The model parameters are α = −0.5 and Epeak = 600 keV. Black contours represent the most accurate localization of LVT151012 obtained from the LALInference (Abbott et al. 2016c) at both the 50% and 90% confidence level. Red, green, and blue contours indicate the regions covered by the INTEGRAL imaging FoV observations performed with IBIS/ISGRI, SPI, and the two JEM-X modules, respectively (the larger bounds of all these FoVs has been set to the point where a worsening of the instrument sensitivity by a factor of 20 compared to the on-axis value is reached), see also Fig. 9. During this observation the Earth’s shadow was near its maximum size for INTEGRAL (about 10 deg diameter) and did not occult the region of non-negligible LIGO probability.

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