CAMPOS：Corona australis、Aquila、chaMaeleon、oPhiuchus north、Ophiuchus、Serpens中0/I类原恒星盘的ALMA遗产巡天。I. 原恒星盘半径的演化
The ALMA Legacy survey of Class 0/I disks in Corona australis, Aquila, chaMaeleon, oPhiuchus north, Ophiuchus, Serpens (CAMPOS). I. Evolution of Protostellar disk radii
AI总结：
本研究利用ALMA对七个附近分子云中的184个原恒星盘进行高分辨率1.3mm观测，发现盘半径随演化存在变异性，且Class 0盘半径分布与现有盘形成模型存在矛盾。
摘要：
我们使用Atacama Large Millimeter/submillimeter Array在1.3mm波段以0.1角秒的分辨率对七个附近分子云（Corona Australis、Aquila、Chamaeleon I和II、Ophiuchus North、Ophiuchus、Serpens）中几乎所有的嵌入式原恒星进行了巡天观测。本次巡天探测到184个原恒星盘，其中90个以14-18 au的分辨率进行了观测，使其成为迄今为止跨越各种原恒星演化阶段的最全面的高分辨率盘样本之一。我们的主要发现包括在两个Class I和两个平谱源中探测到新的环形子结构，同时21个嵌入式原恒星在其盘中表现出明显的不对称性或子结构。我们发现，原恒星盘在所有演化类别中的半径都存在极大的变异性。特别是，尺寸大于60 au的大盘比例随着原恒星从Class 0演化到Class I而减少。通过汇编文献数据，我们发现气体盘半径与尘埃盘半径之比（$R_{\ m gas,Kep}/R_{\ m mm}$）随着辐射温度（${\ m T}_{\ m bol}$）的增加呈上升趋势。我们的结果表明，尘埃盘和气体盘半径在Class I早期阶段发生解耦。然而，在Class 0阶段，尘埃盘和气体盘的尺寸相似，这使得能够在原恒星演化的最早阶段直接对模型和观测数据进行比较。我们表明，我们样本中52个Class 0盘的半径分布与各种盘形成模型存在高度矛盾，表明原恒星盘的形成仍然是一个未解的问题。
英文摘要：
We surveyed nearly all the embedded protostars in seven nearby clouds (Corona Australis, Aquila, Chamaeleon I & II, Ophiuchus North, Ophiuchus, Serpens) with the Atacama Large Millimeter/submillimeter Array at 1.3mm observations with a resolution of 0.1$"$. This survey detected 184 protostellar disks, 90 of which were observed at a resolution of 14-18 au, making it one of the most comprehensive high-resolution disk samples across various protostellar evolutionary stages to date. Our key findings include the detection of new annular substructures in two Class I and two flat-spectrum sources, while 21 embedded protostars exhibit distinct asymmetries or substructures in their disks. We find that protostellar disks have a substantially large variability in their radii across all evolutionary classes. In particular, the fraction of large disks with sizes above 60\,au decreases as the protostar evolves from Class 0 to Class I. Compiling the literature data, we discovered an increasing trend of the gas disk radii to dust disk radii ratio ($R_{\rm gas,Kep}/R_{\rm mm}$) with increasing bolometric temperature (${\rm T}_{\rm bol}$). Our results indicate that the dust and gas disk radii decouple during the early Class I stage. However, in the Class 0 stage, the dust and gas disk sizes are similar, which allows a direct comparison between models and observational data at the earliest stages of protostellar evolution. We show that the distribution of radii in the 52 Class 0 disks in our sample is in high tension with various disk formation models, indicating that protostellar disk formation remains an unsolved question.
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