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We investigate whether strong molecular and atomic emission lines at far‐infrared wavelengths can influence the identification and derived properties of galaxies selected from broad‐band, far‐infrared or submillimetre observations. Several of these lines, for example, [C  ii ] 158  μ m, have been found to be very bright in some galaxies, with fluxes of ≳0.1–1 per cent of the total far‐infrared luminosity, and may be even brighter in certain populations at high redshifts. At redshifts where these lines fall in instrument passbands, they can significantly increase the broad‐band flux measurements. We estimate that the contributions from line emission could boost the apparent broad‐band flux by ≳20–40 per cent in the  Herschel  and SCUBA‐2 bands. Combined with the steep source counts in the submillimetre and far‐infrared bands, line contamination has potentially significant consequences for the properties of sources detected in flux‐limited continuum surveys, biasing the derived redshift distributions and bolometric luminosities. Indeed, it is possible that some  z  &gt; 4 sources found in 850‐ μ m surveys are being identified in part due to the line contamination from strong [C  ii ] emission. These biases may be even stronger for less‐luminous and lower metallicity populations at high redshifts, which are observable with the ALMA and which may have even stronger line‐to‐continuum ratios.

The potential influence of far‐infrared emission lines on the selection of high‐redshift galaxies