标题： IllustrisTNG中超大质量盘的形成和演化 显示英文标题

标题： The formation and evolution of Supermassive disks in IllustrisTNG

摘要： 超大质量盘状星系是引人注目的星系，它们的形成和演化仍然知之甚少。 它们包括各种各样的天体，从大的低表面亮度星系，如马林1号，到最壮观的超亮螺旋星系。 然而，我们仍然不知道其形成的物理机制，以及它们是否会是长寿命的天体，或者它们的质量是否会在一定时间内摧毁它们。 我们旨在利用最先进的磁流体动力学模拟IllustrisTNG-100来研究这些星系的形成和演化。 我们将超大质量盘状星系定义为具有$\lambda / \sqrt{\varepsilon} \geq 0.31$或 0.71，并且恒星质量对数$_{10}M_\star/M_\odot > 10^{11}$的星系。 我们研究了这些星系所处的颜色、合并历史、活动星系核历史和环境。 超大质量盘状星系通常经历平静的合并历史，其中$48\%$在$z \leq 1$时没有经历显著的合并。 它们的恒星质量增长主要由恒星形成驱动，这与需要大量合并才能形成的椭圆星系不同。 此外，盘状星系经历的合并通常富含气体含量，无论它们是小规模还是大规模事件。 超大质量盘状星系存在于各种环境中，从孤立到星系团，其中$\sim 60\%$居住在孤立或低质量的星系群中，$\sim 25\%$居住在大质量的星系群中，而$\sim15\%$则位于星系团内部。 在研究在$z=0.5$选定的超大质量盘的演化时，我们发现当它们获得足够的质量时，它们保持盘状结构直到$z=0$的概率相对较高 ($\sim 60\%$)。 最后，尽管活动星系核显著影响星系中恒星形成的调节，但它不会直接改变它们的形态结构。 显示英文摘要

摘要： Supermassive disks are outstanding galaxies whose formation and evolution are still poorly understood. They comprise a large variety of objects, ranging from large, low-surface-brightness galaxies, such as Malin 1, to the most spectacular superluminous spirals. However, we still do not know the physical mechanisms behind its formation, and whether they will be long-lived objects or whether their mass could destroy them in time. We aim to investigate the formation and evolution of these galaxies using the magnetohydrodynamical state-of-the-art simulation IllustrisTNG-100. We defined supermassive disks as galaxies with $\lambda / \sqrt{\varepsilon} \geq 0.31$ or 0.71, and with stellar mass log$_{10}M_\star/M_\odot > 10^{11}$. We studied the color, merging history, AGN history, and environment in which these galaxies reside. Supermassive disk galaxies typically experience a quiescent merging history, with $48\%$ experiencing no significant mergers at $z \leq 1$. Their stellar mass growth is driven mainly by star formation, unlike spheroidal galaxies, which require a significant number of mergers to form. Moreover, the mergers experienced by disk galaxies are generally rich in gas content, irrespective of whether they are minor or major events. Supermassive disks exist across various environments, from isolation to clusters, with $\sim 60\%$ inhabiting in isolation or low-mass groups, $\sim 25\%$ residing in massive groups, and $\sim15\%$ residing within galaxy clusters. When studying the evolution of supermassive disks selected at $z=0.5$, we show that when they gain sufficient mass, the probability of them maintaining their disk-like structure up to $z=0$ is relatively high ($\sim 60\%$). Lastly, while AGN significantly influences the regulation of star formation in galaxies, it does not directly alter their morphological structure.