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We study the effect of inclination on the apparent brightness of star-forminggalaxies in spectral passbands that are commonly used as star-formationindicators. As diagnostics we use mass-to-light ratios in three passbands: theUV continuum at 280 nm, the H$\alpha$ emission line, and the FIR 24$\mu$-band.We include a study of inclination trends in the IR/UV ratio ("IRX") and theIR/H$\alpha$ ratio. Our sample comprises a few hundred galaxies from the regionaround the clusters Abell 901/902 with deep data and inclinations measured fromouter disks in Hubble Space Telescope images. As a novelty, the H$\alpha$- andseparately the NII-emission are measured by tunable-filter imaging andencompass galaxies in their entirety. At galaxy stellar masses above log$M_*/M_\odot > 10$ we find trends in the UV and H$\alpha$ mass-to-light ratiothat suggest an inclination-induced attenuation from face-on to edge-on of$\sim 1$ mag and $\sim 0.7$ mag in UV and H$\alpha$, respectively, implyingthat star-formation rates of edge-on galaxies would be underestimated by $\sim2.5\times$ in UV and $\sim 2\times$ in H$\alpha$. We find the luminosities inUV and H$\alpha$ to be well correlated, but the optical depth of diffuse dustthat causes inclination dependence appears to be lower for stars emitting at280 nm than for gas clouds emitting Balmer lines. For galaxies with log$M_*/M_\odot < 9.7$, we find no measurable effect at $>0.1$ mag. The absence ofan inclination dependence at 24$\mu$ confirms that the average galaxy isoptically thin in the FIR.

OMEGA - OSIRIS Mapping of Emission-line Galaxies in A901/2: IV. - Extinction of Star-Formation Estimators with Inclination