对蛇夫座-A恒星形成区域的詹姆斯·韦布空间望远镜、阿塔卡马大型毫米/亚毫米波阵列和甚大阵巡天：揭示隐藏的尘埃质量并将红外外流与其射电起源联系起来
A JWST, ALMA and VLA survey of the Ophiuchus-A star-forming region: Unveiling hidden dust mass and connecting infrared outflows to their radio origins
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中文总结 AI 辅助
对蛇夫座A恒星形成区域进行多波段巡天，结合高分辨率观测数据，用基于物理的模型推导尘埃和电离气体性质等，揭示星周尘埃盘质量，联系外流与起源，解决“缺失盘质量”问题，为相关研究提供潜在方案，但受现有分辨率和灵敏度限制。
中文摘要 AI 辅助
我们对蛇夫座A L1688恒星形成星团中的20个0-III类年轻恒星天体进行了红外、毫米波和射电巡天，将高分辨率（7-25天文单位）的甚大阵和詹姆斯·韦布空间望远镜观测与存档的阿塔卡马大型毫米/亚毫米波阵列数据相结合。我们采用基于物理的模型，通过毫米-厘米射电频谱能量分布来推导尘埃和电离气体的性质、光谱行为及其相对贡献。我们的模型揭示了星周尘埃盘，其平均质量比仅基于毫米波估计的质量大数十至数百倍（受尘埃不透明度选择产生的不确定性影响），甚至在0类阶段就包含毫米大小的颗粒。由于甚大阵的高分辨率，我们能够将外流与其起源联系起来，在10-1000天文单位的尺度上探测到原恒星喷流发射。我们的结果代表了对蛇夫座尘埃和电离气体性质的均匀表征，并为长期存在的“缺失盘质量”问题提供了一个潜在解决方案。然而，我们的理解仍受频率<40吉赫兹时的分辨率和灵敏度限制。未来需要像平方公里阵列和下一代甚大阵这样的设施，以提供必要能力，即使在最接近的恒星形成区域之一，也能完全在空间上分辨这种发射（<0.18
英文摘要
We present an infrared, millimetre, and radio survey of 20 Class 0-III young stellar objects in the Ophiuchus A L1688 star-forming cluster, combining high-resolution (7-25 au) VLA and JWST observations with archival ALMA data. We implement physically motivated models to derive dust and ionised gas properties, spectral behaviour and their relative contributions through the millimetre-centimetre radio spectral energy distribution. Our models reveal circumstellar dust disks that are, on average, tens to hundreds of times more massive than millimetre-only estimates (subject to uncertainties arising from the choice of dust opacity) and contain millimetre-sized grains even at the Class 0 stage. Owing to the VLA's high resolution we are able to connect outflows to their origins, detecting protostellar jet emission on scales of 10s-1000s au. Our results represent a homogeneous characterisation of the dust and ionised gas properties in Ophiuchus and present a potential solution to the long-standing 'missing disk mass' problem. However, our understanding is still limited by resolution and sensitivity at frequencies <40 GHz. Future facilities like the SKA and ngVLA are needed to provide the necessary capabilities to fully spatially resolve this emission (<0.18") even in one of the closest star-forming regions.
