tokens: we study (i) a constant 29% contamination and (ii) the stellar mass and redshift-dependent [N ii ]/H α flux ratios predicted by our model (Equation ( 3 )). To derive the intrinsic H α LF using our model [N ii ] contamination (Φ model ), we start with the observed ([N ii ]+H α ) tot LF (Φ obs ( L )) measured by Colbert et al. ( 2013 ) at 0.9 z 1.5. We obtain this LF from their published H α LF (, , and α = −1.43) by dividing the luminosities by a factor of (1–0.29) to undo the constant total [N ii ] flux contamination fraction correction of 29%, which the authors applied. In the following, we treat Φ obs as the true observed LF. Importantly, this LF is not corrected for [N ii ] contamination and dust. Because of the evolution of the star-forming main sequence, Φ obs is redshift-dependent, but here we do not model this dependence across z = 1–2, as we are only interested in the effects of [N ii ] contamination and not the absolute number of galaxies. On the other hand, the stellar mass and redshift-dependent [N ii ] contamination correction will change the intrinsic H α LF across the redshift range studied here. To obtain Φ model , we choose an approach that only uses the measured ([N ii ]+H α ) tot luminosities as input and assumes the most likely underlying stellar mass distribution (robustly determined from other studies), from which we obtain the [N ii ] contamination from our model. This approach has the advantage that it enables an easy implementation and propagation of a variety of uncertainties into the final results. Furthermore, this method results in reliable intrinsic H α LFs even if the mass distribution is poorly measured due to the lack of sufficient multiwavelength data, as long as the selection function of the galaxy sample is known. Here we make use of the Schreiber et al. ( 2015 ) parameterization of the star-forming main sequence to derive the underlying stellar mass distribution (we comment below on possible shortcomings). We note that the choice of different parameterizations (e.g., Tomczak et al. 2016 ) should not change the following results. We start with a distribution of ([N ii ]+H α ) tot , which we sample from Φ obs . To obtain stellar masses for these galaxies, we use a “backward-engineering” technique. First, we convert the SFRs of the Schreiber et al. ( 2015 ) parameterization into H α luminosities using the Kennicutt ( 1998 ) prescription. Thereby, we include a dispersion of 0.3 dex measured on the SFR–versus–stellar mass main sequence. Second, we redden the H α luminosities according to the relation between A H α (H α extinction) and stellar mass robustly derived from the spectra of local galaxy samples in SDSS (Garn Best 2010 ). This relation holds for the WISPS sample at 0.8 z 1.5, as shown in Domínguez et al. ( 2013 ). Third, we add the contribution of [N ii ] to the H α luminosity by using our model. Finally, this translation between dust-reddened ([N ii ]+H α ) tot luminosities and stellar masses allows us
ner_tags: O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Formula I-Formula I-Formula O O O O O O O B-Wavelength I-Wavelength O B-TextGarbage I-TextGarbage O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O B-Wavelength I-Wavelength B-Wavelength I-Wavelength O O O O O O O O O O O O O O B-Survey B-Citation I-Citation I-Citation O O O O O O B-Dataset I-Dataset O B-Formula I-Formula I-Formula O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O