VERTICO V：室女座星系团星系内部冷气体盘的环境驱动演化
VERTICO V: The environmentally driven evolution of the inner cold gas discs of Virgo cluster galaxies
AI总结：
本研究利用VERTICO巡天和存档HI数据，分析室女座星系团星系光学盘内冷气体的空间分布，发现环境不仅剥离外围HI，还会降低中心区域气体面密度，且分子气体减少需用直接剥离解释。
摘要：
星系团卫星星系的恒星形成淬灭与环境机制对其冷星际介质（ISM）的抑制密不可分。尽管大半径处中性原子氢（HI）的剥离已得到充分研究，但环境如何影响星系中心以分子气体为主的剩余气体，目前仍不明确。利用CO示踪室女座环境巡天（VERTICO）的新观测数据和存档HI数据，我们以1.2千秒差距的分辨率研究了室女座星系团星系光学盘内的HI和分子气体，构建了恒星（$Σ_{\nstar}$）、HI（$Σ_\nHI$）和分子气体（$Σ_\nmol$）面密度的空间分辨标度关系。以HI缺失度作为环境影响的衡量指标，我们发现证据表明，星系团过程除了剥离大半径处的HI外，甚至在中心1.2千秒差距区域也会降低剩余气体的平均$Σ_\nHI$。环境对分子气体的影响相对弱于对HI的影响，且我们发现较低$Σ_\nmol$的气体会先被剥离。然而，在HI缺失最严重的星系中，我们发现证据表明环境过程使剩余气体的典型$Σ_\nmol$降低了近3倍。我们未在HI缺失星系中发现环境驱动$Σ_\nHI$或$Σ_\nmol$升高的证据。通过单个区域内$Σ_\nmol$与$Σ_\nHI$的比值，我们发现利用总气体面密度和中平面流体静压力估算的星际介质物理条件变化，无法解释观测到的分子气体含量减少。相反，我们认为需要分子气体的直接剥离来解释我们的结果。
英文摘要：
The quenching of cluster satellite galaxies is inextricably linked to the suppression of their cold interstellar medium (ISM) by environmental mechanisms. While the removal of neutral atomic hydrogen (HI) at large radii is well studied, how the environment impacts the remaining gas in the centres of galaxies, which are dominated by molecular gas, is less clear. Using new observations from the Virgo Environment traced in CO survey (VERTICO) and archival HI data, we study the HI and molecular gas within the optical discs of Virgo cluster galaxies on 1.2-kpc scales with spatially resolved scaling relations between stellar ($Σ_{\star}$), HI ($Σ_\mathrm{HI}$), and molecular gas ($Σ_\mathrm{mol}$) surface densities. Adopting HI deficiency as a measure of environmental impact, we find evidence that, in addition to removing the HI at large radii, the cluster processes also lower the average $Σ_\mathrm{HI}$ of the remaining gas even in the central 1.2 kpc. The impact on molecular gas is comparatively weaker than on the HI, and we show that the lower $Σ_\mathrm{mol}$ gas is removed first. In the most HI-deficient galaxies, however, we find evidence that environmental processes reduce the typical $Σ_\mathrm{mol}$ of the remaining gas by nearly a factor of 3. We find no evidence for environment-driven elevation of $Σ_\mathrm{HI}$ or $Σ_\mathrm{mol}$ in HI-deficient galaxies. Using the ratio of $Σ_\mathrm{mol}$-to-$Σ_\mathrm{HI}$ in individual regions, we show that changes in the ISM physical conditions, estimated using the total gas surface density and midplane hydrostatic pressure, cannot explain the observed reduction in molecular gas content. Instead, we suggest that direct stripping of the molecular gas is required to explain our results.
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