Constraints on the binary fraction of massive young stellar objects (mYSOs) are important for binary and massive star formation theory. Here, we present speckle imaging of 34 mYSOs located in the Large Magellanic Cloud (1/2 Z _⊙) and Small Magellanic Cloud (∼1/5 Z _⊙), probing projected separations in the 2000 to 20,000 au (at angular scales of 0.″02–0.″2) range, for stars above 8 M _⊙. We find two wide binaries in the Large Magellanic Cloud (from a sample of 23 targets), but none in a sample of 11 in the Small Magellanic Cloud, leading us to adopt a wide binary fraction of 9% ± 5% and <5%, respectively. We rule out a wide binary fraction greater than 35% in the Large Magellanic Cloud and 38% in the Small Magellanic Cloud at the 99% confidence level. This is in contrast to the wide binary fraction of mYSOs in the Milky Way (presumed to be 1 Z _⊙), which within the physical parameter space probed by this study is ∼15%–60% from the literature. We argue that while selection effects could be responsible for the lower binary fraction observed, it is more likely that there are underlying physical mechanisms responsible for the observed properties. This indicates that metallicity and environmental effects may influence the formation of wide binaries among massive stars. Future larger, more statistically significant samples of high-mass systems in low-metallicity environments for comparison to the Milky Way, are essential to confirm or repudiate our claim.

中文翻译：

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麦哲伦星云中大质量年轻恒星物体的高分辨率成像巡天


对大质量年轻恒星（mYSO）的双星部分的约束对于双星和大质量恒星形成理论非常重要。在这里，我们展示了位于大麦哲伦星云 (1/2 Z _⊙ ) 和小麦哲伦星云 (∼1/5 Z _⊙ ) 中的 34 个 mYSO 的散斑成像，探测了 2000 至 20,000 au 范围内的预计间隔（角尺度为 0 .″02–0.″2) 范围，对于8 M 以上的恒星_⊙ 。我们在大麦哲伦星云中发现了两个宽双星（来自 23 个目标的样本），但在小麦哲伦云中的 11 个目标样本中没有找到，这导致我们采用 9% ± 5% 和 <5% 的宽双星分数， 分别。在 99% 的置信水平下，我们排除了大麦哲伦云中大于 35% 和小麦哲伦云中大于 38% 的宽二元分数。这与银河系中 mYSO 的宽二元部分（假定为 1 Z _⊙ ）形成鲜明对比，在本研究探测的物理参数空间内，mYSO 在文献中占 ∼15%–60%。我们认为，虽然选择效应可能是观察到的较低二元分数的原因，但更可能的是存在导致观察到的特性的潜在物理机制。这表明金属丰度和环境影响可能会影响大质量恒星中宽双星的形成。未来在低金属丰度环境中获得更大、更具统计意义的高质量系统样本，以便与银河系进行比较，对于证实或否定我们的主张至关重要。