We present a 0.″15 resolution (21 au) ALMA 870 μm continuum survey of 25 pointings containing 31 young stellar objects in the Ophiuchus molecular clouds. Using the dust continuum as a proxy for dust mass and circumstellar disk radius in our sample, we report mean masses of and M _⊕ and mean radii of and au, for Class I and Flat spectrum protostars, respectively. In addition, we calculate the multiplicity statistics of the dust surrounding young stellar objects in Ophiuchus. The multiplicity fraction and companion star fraction of the combined Class I and Flats based solely on this work are 0.25 0.09 and 0.33 0.10, respectively, which are consistent with the values for Perseus and Orion. While we see clear differences in mass and radius between the Ophiuchus and Perseus/Orion protostellar surveys, we do not see any significant differences in the multiplicities of the various regions. We posit that there are some differences in the conditions for star formation in Ophiuchus that strongly affect disk size (and consequently disk mass), but does not affect system multiplicity, which could imply important variation in planet formation processes.

我们提出了一个0“。15分辨率（21 AU）ALMA 870 μ的含有在蛇夫分子云31个年轻星体25个勾缝连续调查。使用粉尘连续的粉尘量和周盘半径我们的样本中的代理，我们报告的均值群众和 中号 _⊕和平均半径和au，分别用于 I 类和平谱原星。此外，我们计算了蛇夫座中年轻恒星周围尘埃的多重统计。仅基于这项工作的 I 类和扁平星组合的重数分数和伴星分数分别为 0.25 0.09 和 0.33 0.10，这与英仙座和猎户座的值一致。虽然我们看到蛇夫座和英仙座/猎户座原恒星巡天之间的质量和半径存在明显差异，但我们没有看到不同区域的多样性有任何显着差异。我们假设蛇夫座恒星形成的条件存在一些差异，它们强烈影响盘的大小（以及盘的质量），但不影响系统的多样性，这可能意味着行星形成过程的重要变化。