We present a study of ultra-diffuse galaxies (UDGs) in the Virgo Cluster based on deep imaging from the Next Generation Virgo Cluster Survey (NGVS). Applying a new definition for the UDG class based on galaxy scaling relations, we define samples of 44 and 26 UDGs using expansive and restrictive selection criteria, respectively. Our UDG sample includes objects that are significantly fainter than previously known UDGs: i.e., more than half are fainter than $\langle\mu\rangle_e \sim27.5$ mag arcsec$^{-2}$. The UDGs in Virgo's core region show some evidence for being structurally distinct from "normal" dwarf galaxies, but this separation disappears when considering the full sample of galaxies throughout the cluster. UDGs are more centrally concentrated in their spatial distribution than other Virgo galaxies of similar luminosity, while their morphologies demonstrate that at least some UDGs owe their diffuse nature to physical processes---such as tidal interactions or low-mass mergers---that are at play within the cluster environment. The globular cluster (GC) systems of Virgo UDGs have a wide range in specific frequency ($S_N$), with a higher mean $S_N$ than "normal" Virgo dwarfs, but a lower mean $S_N$ than Coma UDGs at fixed luminosity. Their GCs are predominantly blue, with a small contribution from red clusters in the more massive UDGs. The combined GC luminosity function is consistent with those observed in dwarf galaxies, showing no evidence of being anomalously luminous. The diversity in their morphologies and their GC properties suggests no single process has given rise to all objects within the UDG class. Based on the available evidence, we conclude that UDGs are simply those systems that occupy the extended tails of the galaxy size and surface brightness distributions.

中文翻译：

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下一代处女座集群调查（NGVS）。XXX。超扩散星系及其球状星团系统

我们基于下一代室女座星团巡天 (NGVS) 的深度成像，对处女座星团中的超扩散星系 (UDG) 进行了研究。应用基于星系比例关系的 UDG 类的新定义，我们分别使用扩展和限制性选择标准定义了 44 个和 26 个 UDG 的样本。我们的 UDG 样本包括比以前已知的 UDG 明显更暗的物体：即，超过一半的物体比 $\langle\mu\rangle_e\sim27.5$ mag arcsec$^{-2}$ 更暗。处女座核心区域的 UDG 显示出一些在结构上与“正常”矮星系不同的证据，但是当考虑整个星团的完整星系样本时，这种分离就消失了。UDG 的空间分布比其他类似光度的室女座星系更集中，而它们的形态表明，至少一些 UDG 的扩散性质归功于物理过程——例如潮汐相互作用或低质量合并——在集群环境中发挥作用。处女座 UDG 的球状星团 (GC) 系统在特定频率 ($S_N$) 上的范围很广，平均 $S_N$ 高于“正常”处女座矮星，但在固定光度下的平均 $S_N$ 低于彗发 UDGs . 它们的 GC 主要是蓝色的，在更大的 UDG 中，红色簇的贡献很小。组合的 GC 光度函数与在矮星系中观察到的一致，没有显示异常光度的证据。它们的形态和 GC 特性的多样性表明，没有一个过程产生了 UDG 类中的所有对象。根据现有证据，