We present 2D-spectroscopic observations from Centro Astronómico Hispano Alemán ( CAHA ) 3.5 m telescope and the millimetre observation from NOrthern Extended Millimeter Array ( NOEMA ) of the nearby S0 galaxy PGC 26218 , which shows central star-formation activity and post-starburst outside in the disk .
We estimate the star formation rate ( SFR = 0.28 \pm 0.01 M _ { \odot } yr ^ { -1 } ) and molecular gas mass ( log M _ { H _ { 2 } } = 7.60 \pm 0.15 M _ { \odot } ) of PGC 26218 based on the extinction-corrected H \alpha emission line and the CO- H _ { 2 } conversion factor ( \alpha _ { CO } ) of the Milky Way , respectively .
We find that PGC 26218 follows the star forming main sequence ( SFMS ) and the Kennicutt-Schmidt law .
Comparing the kinematics of CO ( J =1-0 ) , stars and H \alpha , we find that the rotational axis of CO ( J =1-0 ) is 45 ^ { \circ } different from that of H \alpha .
In addition , the profile of the CO ( J =1-0 ) emission line shows asymmetry and has an inflow component of \sim 46 km s ^ { -1 } .
With the decomposition of the optical image , we confirm that PGC 26218 shows multiple nuclear structures .
The projected offset between the most luminous optical center and the center of CO ( J =1-0 ) is 5.2 \arcsec ( \sim 0.6 kpc ) and the latter overlaps with one of the optical cores .
These results support that PGC 26218 may have experienced a gas-rich minor merger , extending its star formation and locating it in the SFMS .