Required peak brightness of simulated laser lines, relative to the stellar continuum in each spectral order, for 80% to be detected, as determined by direct injection of mock laser lines and their recovery (or not) by the detection pipeline. Each panel represents a different stellar type observed without the “pollution” of iodine lines (left column) and with iodine lines (right column), which compromise the sensitivity to laser lines. Low luminosity M-dwarfs with their many atomic and molecular absorption features suffer from high detection thresholds in continuum units, yet due to their low overall flux allow the detection of faint lasers.