Stellar系统的大规模组装及其与SMA-1.3 mm微型数据发布的演变
Mass Assembly of Stellar Systems and their Evolution with the SMA - 1.3 mm Subcompact Data Release
摘要：
我们提出了恒星系统的质量组装及其演化与SMA（MASSES）调查，它使用亚毫米阵列（SMA）干涉仪映射的连续谱和分子线的所有74个已知的0/I类原恒星系统在英仙座分子云。调查的主要目标是在一个单一的分子云中观察年轻原恒星的无偏见样本，以便我们能够描述原恒星的演化。本文发布了来自次紧凑型配置（$\sim$ 4 $^{\prime\prime}$或$\sim$ 1000 au分辨率）的MASSES 1.3 mm数据，这是SMA最紧凑的阵列配置。我们发布了光谱线CO（2 - 1）、$^{13}$ CO（2 - 1）、C $^{18}$ O（2 - 1）和N $_2$ D $^+$（3 - 2）以及1.3 mm连续谱的$uv$可见度数据和成像数据。我们识别出在每个源中检测到的示踪剂。我们还展示了连续谱和CO（2 - 1）外流的示例图像，分析了C $^{18}$ O（2 - 1）光谱，并提供了SVS 13恒星形成区的数据。从连续计算的信封质量显示出减少的趋势与测热温度（年龄的代理）。典型的C $^{18}$ O（2 - 1）线宽为1.45 km/s $^{-1}$，这高于在英仙座灯丝和核心探测到的C $^{18}$ O线宽。我们发现，N $_2$ D $^+$（3 - 2）更有可能在年轻的原恒星中被探测到。我们证明了SVS 13中的原恒星包含在由C $^{18}$ O（2 - 1）和N $_2$ D $^+$（3 - 2）追踪的星系结构中。我们还提出了SVS13 A的高速度（绝对视线速度$>$ 150公里秒$^{-1}$）的红色和蓝色流出成分的位置。数据可从www.example.com下载。
英文摘要：
We present the Mass Assembly of Stellar Systems and their Evolution with the SMA (MASSES) survey, which uses the Submillimeter Array (SMA) interferometer to map the continuum and molecular lines for all 74 known Class 0/I protostellar systems in the Perseus molecular cloud. The primary goal of the survey is to observe an unbiased sample of young protostars in a single molecular cloud so that we can characterize the evolution of protostars. This paper releases the MASSES 1.3 mm data from the subcompact configuration ($\sim$4$^{\prime\prime}$ or $\sim$1000 au resolution), which is the SMA's most compact array configuration. We release both $uv$ visibility data and imaged data for the spectral lines CO(2-1),$^{13}$CO(2-1), C$^{18}$O(2-1), and N$_2$D$^+$(3-2), as well as for the 1.3 mm continuum. We identify the tracers that are detected toward each source. We also show example images of continuum and CO(2-1) outflows, analyze C$^{18}$O(2-1) spectra, and present data from the SVS 13 star-forming region. The calculated envelope masses from the continuum show a decreasing trend with bolometric temperature (a proxy for age). Typical C$^{18}$O(2-1) linewidths are 1.45 km s$^{-1}$, which is higher than the C$^{18}$O linewidths detected toward Perseus filaments and cores. We find that N$_2$D$^+$(3-2) is significantly more likely to be detected toward younger protostars. We show that the protostars in SVS 13 are contained within filamentary structures as traced by C$^{18}$O(2-1) and N$_2$D$^+$(3-2). We also present the locations of SVS 13A's high velocity (absolute line-of-sight velocities $>$150 km s$^{-1}$) red and blue outflow components. Data can be downloaded from https://dataverse.harvard.edu/dataverse/MASSES .
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
