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Fig. 11.

image

Distribution of the peak magnitudes of the validated events in the I-band (left panel) and in the R-band (right panel). For comparison we have plotted the distribution of the events observed by Suggs et al. (2014) in the R-band (black-line histogram in the right panel). It is evident that the NELIOTA campaign is detecting flashes about two magnitudes fainter than what was previously detected by Suggs et al. (2014), a result of the use of a larger aperture telescope (see text for details). The difference in the number of the events is mainly due to the different campaign periods (one year of NELIOTA observations versus five years of observations in Suggs et al. 2014).

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