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Using the AKARI, Wide-field Infrared Survey Explorer (WISE), InfraredAstronomical Satellite (IRAS), Sloan Digital Sky Survey (SDSS) and Hubble SpaceTelescope (HST) data, we investigated the relation of polycyclic aromatichydrocarbon (PAH) mass ($M_{\rm PAH}$), very small grain mass ($M_{\rm VSG}$),big grain mass ($M_{\rm BG}$) and stellar mass ($M_{\rm star}$) with galaxymerger for 55 star-forming galaxies at redshift $z<0.2$. Using the SDSS imageat $z<0.1$ and the HST image at $z>0.1$, we divided the galaxies into mergergalaxies and non-merger galaxies with the morphological parameter asymmetry$A$, and quantified merging stages of galaxies based on the morphologicalindicators, the second-order momentum of the brightest 20$\%$ region $M_{20}$and the Gini coefficient. We find that $M_{\rm PAH}/M_{\rm BG}$ of mergergalaxies tend to be lower than that of non-merger galaxies and there are nosystematic differences of $M_{\rm VSG}/M_{\rm BG}$ and $M_{\rm BG}/M_{\rmstar}$ between merger galaxies and non-merger galaxies. We find that galaxieswith very low $M_{\rm PAH}/M_{\rm BG}$ seem to be merger galaxies at latestages. These results suggest that PAHs are partly destroyed at late stages ofmerging processes. Furthermore, we investigated $M_{\rm PAH}/M_{\rm BG}$variations in radiation field intensity strength $G_0$ and the emission lineratio of $[{\rm O\,{\scriptsize I}}]\lambda 6300/{\rm H}\alpha$ which is ashock tracer for merger galaxies and find that $M_{\rm PAH}/M_{\rm BG}$decreases with increasing both $G_0$ and $[{\rm O\,{\scriptsize I}}]/{\rmH}\alpha$. PAH destruction is likely to be caused by two processes; strongradiation fields and large-scale shocks during merging processes of galaxies.

A Relationship of Polycyclic Aromatic Hydrocarbon Features with Galaxy Merger in Star-forming Galaxies at $z<0.2$