论文标题
S0 Galaxy PGC 26218的物理特性：Starburst和Star组的起源
The physical properties of S0 galaxy PGC 26218: the origin of starburst and star formation
论文作者
论文摘要
我们介绍了CentroAstroStroStroStrostroscotic的2D-SpectRospic观察结果，来自HispanoAlemán（CAHA）3.5 M望远镜和附近S0 Galaxy PGC 26218的Northern Extender Extender Extender毫米阵列（NOEMA）的毫米表观察，显示了中央星星拟合活性和后星堡外部和后星堡外的中央星星。我们估计恒星形成率（SFR = $ 0.28 \ PM0.01 $ $ $ M _ {\ odot} \ rm yr^{ - 1} $）和分子气体质量（$ \ rm log \ $ \ $ \ $ \ $ \ $ \ $ \ $ _ 26218基于灭绝校正的H $α$发射线和Co-$ \ rm H_ {2} $转换因子（$α_ {\ rm Co} $），分别是银河系的方式。我们发现PGC 26218遵循恒星形成主序列（SFM）和Kennicutt-Schmidt定律。比较CO的运动学（$ j $ = 1-0），星和H $α$，我们发现CO（$ J $ = 1-0）的旋转轴为45 $^{\ circ} $与H $α$不同。此外，CO（$ J $ = 1-0）发射线的配置文件显示不对称，并具有$ \ sim $ 46 $ \ rm \ rm \ rm \ s \ s^{ - 1} $的流入部分。随着光学图像的分解，我们确认PGC 26218显示了多个核结构。最发光的光学中心和CO中心（$ j $ = 1-0）之间的预计偏移量为$ 5.2 \ arcsec $（$ \ sim $ 0.6 kpc），而后者与其中一个光核重叠。这些结果支持PGC 26218可能经历了富含气体的小型合并，扩展了其恒星形成并将其定位在SFMS中。
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 = $0.28\pm0.01$ $M_{\odot} \rm yr^{-1}$) and molecular gas mass ($\rm log\ $$M_{\rm H_{2}}=7.60\pm0.15\ M_{\odot}$) of PGC 26218 based on the extinction-corrected H$α$ emission line and the CO-$\rm H_{2}$ conversion factor ($α_{\rm CO}$) 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$α$, we find that the rotational axis of CO($J$=1-0) is 45$^{\circ}$ different from that of H$α$. In addition, the profile of the CO($J$=1-0) emission line shows asymmetry and has an inflow component of $\sim$ 46 $\rm km\ s^{-1}$. 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.
