ALMA一氧化碳超新星（ACOS）巡天II. 核心坍缩超新星位置处的湍流巨分子云
The ALMA carbon monoxide supernova (ACOS) survey II. Turbulent giant molecular clouds at the positions of core-collapse supernovae
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中文总结 AI 辅助
该研究通过ALMA观测33个邻近核心坍缩超新星位置的一氧化碳谱线，发现这类超新星偏好高速度弥散的分子气体区域，为其前身星的性质提供了观测约束。
中文摘要 AI 辅助
背景：对冷分子氢气体（以下简称分子气体）的研究为其与恒星形成区的相互作用提供了关键线索，但分子气体湍流与大质量恒星（质量>8倍太阳质量）作为核心坍缩超新星（CCSNe）爆发的位置之间的关联仍未被探索。目标：我们首次测量CCSNe环境中分子气体的湍流，旨在限定其前身星的性质。方法：为达到巨分子云（GMC）的空间分辨率（约100秒差距），我们收集了ALMA观测的一氧化碳J=2→1谱线（约230.54吉赫兹，作为分子气体的示踪物），观测对象为33个邻近CCSNe（距离<100兆秒差距）的位置。结果：我们发现，与宿主星系的平均水平相比，CCSNe更倾向于处于具有高速度弥散的分子气体区域。结论：对于CCSNe前身星，该观测证据支持它们在高密度区域的形成增加，或具有双星性质。
英文摘要
Context. Study of cold molecular hydrogen gas (hereafter molecular gas) provides crucial insights into its interplay with star-forming regions. However, the connection between molecular gas turbulence and the sites of massive star ($> 8~\rm{M}_{\odot}$) explosions as core-collapse supernovae (CCSNe) remains unexplored. Aims. We measure for the first time the turbulence of molecular gas in environments of CCSNe, with the aim to constrain the nature of their progenitors. Methods. In order to reach spatial resolutions of giant molecular cloud (GMC) sizes ($\sim 100~\rm{pc}$), we collected ALMA carbon monoxide $J = 2 \rightarrow 1$ spectral line ($\sim 230.54~\rm{GHz}$) observations (as a tracer of molecular gas) at the locations of 33 nearby CCSNe ($< 100~\rm{Mpc}$). Results. We found that CCSNe prefer molecular gas regions with high velocity dispersion compared to the average of their host galaxies. Conclusions. For CCSN progenitors, this observational evidence supports their increased formation in regions of high densities and/or their binary nature.
