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

Abstract

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 = $0.28\pm 0.01$ $M_{\odot }\mathrm{y}{\mathrm{r}}^{-1}$) and molecular gas mass ($\log$$M_{{\mathrm{H}}_2}=7.60\pm 0.15M_{\odot }$) of PGC 26218 based on the extinction-corrected H$\alpha$ emission line and the CO-${\mathrm{H}}_2$ conversion factor (${\alpha }_{\mathrm{CO}}$) 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 $\mathrm{km}{\mathrm{s}}^{-1}$. 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.

accepted for publication in ApJ, 16 page, 12 figures

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