标题： SAMI和MaNGA近邻星系中中心恒星面密度与恒星自旋的物理联系 显示英文标题

标题： The physical connection between central stellar surface density and stellar spin in SAMI and MaNGA nearby galaxies

摘要： 内核区 1 千秒差距（$\Sigma_{1}$）内的恒星面密度已成为理解星系增长及其与恒星形成熄灭之间联系的一种流行工具。 由此产生的图景表明，构建一个中心致密的核心是熄灭的必要条件。然而，目前尚不清楚$\Sigma_{1}$的变化是否可以追踪恒星运动学和弥散主导凸起的增长。 在本文中，我们结合了来自斯隆数字巡天的图像和来自悉尼-阿格顿天文台多目标积分场单元（SAMI）和阿帕奇点天文台近邻星系测绘（MaNGA）巡天的恒星运动学，量化了 1599 个附近星系在一有效半径（$\lambda_{re}$）内$\Sigma_{1}$和恒星自旋参数代理之间的相关性。 我们显示，在恒星形成主序上且在固定的恒星质量下，$\Sigma_{1}$的变化反映在$\lambda_{re}$的变化上。 在形成恒星时，主序列星系仍然是旋转主导的系统，其$\Sigma_{1}$增加，但恒星自旋保持不变或略有增加。 主序列以下的图像发生了变化，在这里 $\Sigma_{1}$ 和 $\lambda_{re}$ 不再相关。 被动系统显示出比形成恒星的星系更窄的 $\Sigma_{1}$ 范围，但 $\lambda_{re}$ 的范围更宽。 我们的结果表明，从结构角度来看，被动星系比形成恒星的系统具有更大的异质性，并且可能经历了各种各样的演化路径。 这也表明，如果在 $z\sim$0时分散主导的凸起仍然显著增长，这通常发生在熄灭阶段期间或之后。 显示英文摘要

摘要： The stellar surface density within the inner 1 kpc ($\Sigma_{1}$) has become a popular tool for understanding the growth of galaxies and its connection with the quenching of star formation. The emerging picture suggests that building a central dense core is a necessary condition for quenching. However, it is not clear whether changes in $\Sigma_{1}$ trace changes in stellar kinematics and the growth of dispersion-dominated bulges. In this paper, we combine imaging from the Sloan Digital Sky Survey with stellar kinematics from the Sydney-AAO Multi-object Integral-field unit (SAMI) and Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) surveys to quantify the correlation between $\Sigma_{1}$ and the proxy for stellar spin parameter within one effective radius ($\lambda_{re}$) for 1599 nearby galaxies. We show that, on the star-forming main sequence and at fixed stellar mass, changes in $\Sigma_{1}$ are mirrored by changes in $\lambda_{re}$. While forming stars, main sequence galaxies remain rotationally-dominated systems, with their $\Sigma_{1}$ increasing but their stellar spin staying either constant or slightly increasing. The picture changes below the main sequence, where $\Sigma_{1}$ and $\lambda_{re}$ are no longer correlated. Passive systems show a narrower range of $\Sigma_{1}$, but a wider range of $\lambda_{re}$ compared to star-forming galaxies. Our results indicate that, from a structural point of view, passive galaxies are a more heterogeneous population than star-forming systems, and may have followed a variety of evolutionary paths. This also suggests that, if dispersion-dominated bulges still grow significantly at $z\sim$0, this generally takes place during, or after, the quenching phase.