tokens: with ) based on their line properties alone. We compare the results from the simulations to what is expected when using the negative image FDR as reference. For the latter, we estimate the probability of an emission line with of being false by taking , where is the number of emission lines with found in the negative data, while is the number found in the positive (“real”) data. This means that for equal numbers, there is a 100% probability that the line is produced by noise. Alternatively, if there there are twice as many positive lines as negative ones, we assume that there is a 50% probability that each positive line is real. A comparison between simulations and negative image FDR probabilities for each cluster is shown in Fig. 4 . We see that using the negative image FDR as a reference for estimating the probability of a line being false returns a much noisier and sharper probability distribution for all of the clusters. At a given S/N value, it can strongly under- or overestimate the probability since it is dominated by small number statistics. Using simulations allows us to more accurately assign probabilities and understand the true detection rate at low . To confirm weaker real emission lines, we investigate the NIR and 1.1 mm counterparts of all of our candidates. Fig. 4 Probability of an emission line with a given of being produced by noise for the five clusters. Solid curves correspond to the probabilities given by the simulations, while dashed curves correspond to the probabilities estimated from the negative data. 3.3. Association with optical/NIR counterparts Clearly galaxies with high SFRs are likely to be detectable both with HST and/or ALMA in continuum and in molecular emission lines. Because of this, we expect that an emission line candidate co-spatial to a NIR detected galaxy should increase the probability of this candidate being real and thus use the NIR images for this purpose. However, the lack of a NIR or 1.1 mm counterpart does not necessarily imply that the emission line is noise. A galaxy that remains undetected both in HST/160 and ALMA continuum at could still have a at and at , based on spectral energy distribution fitting. In such cases, it should still be possible to detect CO, [NII], or [CII]lines. For instance, we find that CO can be detected at from CO lines when a high CO excitation level () is present in combination with strong dust extinction (). Detections of [NII]and [CII]lines can be made to lower SFRs and extinctions () at . Thus, some weak line candidates that lack NIR counterparts could still be real. Unfortunately, in such cases, confirmation and identification of line candidates will only be possible with deeper mm observations, which is beyond the scope of this study. Thus, we restrict our analysis of weak emission line candidates to those with nearby optical/NIR detected sources. Based on the number and spatial distribution of NIR detections in the FFs, a given random position within any of
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