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Dust attenuation of an inclined galaxy can cause additional asymmetries inobservations, even if the galaxy has a perfectly symmetric structure. {Takingadvantage of the integral field spectroscopic data observed by the SDSS-IVMaNGA survey, we investigate the asymmetries of the emission-line and continuummaps of star-forming disk galaxies.} We define new parameters, $A_a$ and $A_b$,to estimate the asymmetries of a galaxy about its major and minor axes,respectively. Comparing $A_a$ and $A_b$ in different inclination bins, weattempt to detect the asymmetries caused by dust. For the continuum images, wefind that $A_a$ increases with the inclination, while the $A_b$ is a constantas inclination changes. Similar trends are found for $g-r$, $g-i$ and $r-i$color images. The dependence of the asymmetry on inclination suggests a thindust layer with a scale height smaller than the stellar populations. For theH$\alpha$ and H$\beta$ images, neither $A_a$ nor $A_b$ shows a significantcorrelation with inclination. Also, we do not find any significant dependenceof the asymmetry of $E(B-V)_g$ on inclination, implying that the dust in thethick disk component is not significant. Compared to the SKIRT simulation, theresults suggest that the thin dust disk has an optical depth $\tau_V\sim0.2$.This is the first time that the asymmetries caused by the dust attenuation andthe inclination are probed statistically with a large sample. Our resultsindicate that the combination of the dust attenuation and the inclinationeffects is a potential indicator of the 3D disk orientation.

Asymmetry Revisited: The Effect of Dust Attenuation and Galaxy Inclination