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The weak transient detected by the Fermi Gamma-ray Burst Monitor (GBM) 0.4 safter GW150914 has generated much speculation regarding its possibleassociation with the black-hole binary merger. Investigation of the GBM data byConnaughton et al. (2016) revealed a source location consistent with GW150914and a spectrum consistent with a weak, short Gamma-Ray Burst.  Greiner et al. (2016) present an alternative technique for fittingbackground-limited data in the low-count regime, and call into question thespectral analysis and the significance of the detection of GW150914-GBMpresented in Connaughton et al. (2016). The spectral analysis of Connaughton etal. (2016) is not subject to the limitations of the low-count regime noted byGreiner et al. (2016). We find Greiner et al. (2016) used an inconsistentsource position and did not follow the steps taken in Connaughton et al. (2016)to mitigate the statistical shortcomings of their software when analyzing thisweak event. We use the approach of Greiner et al. (2016) to verify that ouroriginal spectral analysis is not biased.  The detection significance of GW150914-GBM is established empirically, with aFalse Alarm Rate (FAR) of $\sim 10^{-4}$~Hz. A post-trials False AlarmProbability (FAP) of $2.2 \times 10^{-3}$ ($2.9 \sigma$) of this transientbeing associated with GW150914 is based on the proximity in time to the GWevent of a transient with that FAR. The FAR and the FAP are unaffected by thespectral analysis that is the focus of Greiner et al. (2016).

On the interpretation of the Fermi GBM transient observed in coincidence with LIGO Gravitational Wave Event GW150914