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We present the results of CO(1-0) observations of the host galaxy of a Type Isuperluminous supernova (SLSN-I), SN2017egm, one of the closest SLSNe-I at z =0.03063, by using the Atacama Large Millimeter/submillimeter Array. Themolecular gas mass of the host galaxy is $M_{\rm gas} = (4.8 \pm 0.3) \times10^9$ $M_{\odot}$, placing it on the sequence of normal star-forming galaxiesin an $M_{\rm gas}$-star-formation rate (SFR) plane. The molecular hydrogencolumn density at the location of SN2017egm is higher than that of the Type IISN PTF10bgl, which is also located in the same host galaxy, and those of otherType II and Ia SNe located in different galaxies, suggesting that SLSNe-I havea preference for a dense molecular gas environment. On the other hand, thecolumn density at the location of SN2017egm is comparable to those of Type IbcSNe. The surface densities of molecular gas and the SFR at the location ofSN2017egm are consistent with those of spatially resolved local star-forminggalaxies and follow the Schmidt-Kennicutt relation. These facts suggest thatSLSNe-I can occur in environments with the same star-formation mechanism as innormal star-forming galaxies.

Spatially Resolved Molecular Gas Properties of Host Galaxy of Type I Superluminous Supernova SN 2017egm