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We present 2D-spectroscopic observations from Centro Astron\'omico HispanoAlem\'an (CAHA) 3.5 m telescope and the millimetre observation from NOrthernExtended Millimeter Array (NOEMA) of the nearby S0 galaxy PGC 26218, whichshows central star-formation activity and post-starburst outside in the disk.We estimate the star formation rate (SFR = $0.28\pm0.01$ $M_{\odot} \rmyr^{-1}$) and molecular gas mass ($\rm log\ $$M_{\rm H_{2}}=7.60\pm0.15\M_{\odot}$) of PGC 26218 based on the extinction-corrected H$\alpha$ emissionline and the CO-$\rm H_{2}$ conversion factor ($\alpha_{\rm CO}$) of the MilkyWay, respectively. We find that PGC 26218 follows the star forming mainsequence (SFMS) and the Kennicutt-Schmidt law. Comparing the kinematics ofCO($J$=1-0), stars and H$\alpha$, we find that the rotational axis ofCO($J$=1-0) is 45$^{\circ}$ different from that of H$\alpha$. In addition, theprofile of the CO($J$=1-0) emission line shows asymmetry and has an inflowcomponent of $\sim$ 46 $\rm km\ s^{-1}$. With the decomposition of the opticalimage, we confirm that PGC 26218 shows multiple nuclear structures. Theprojected offset between the most luminous optical center and the center ofCO($J$=1-0) is $5.2\arcsec$ ($\sim$ 0.6 kpc) and the latter overlaps with oneof the optical cores. These results support that PGC 26218 may have experienceda gas-rich minor merger, extending its star formation and locating it in theSFMS.

The physical properties of S0 galaxy PGC 26218: the origin of starburst and star formation