We present high angular resolution observations of OH maser emission towards the high-mass star forming region IRAS 06056+2131. The observations were carried out using the UK radio interferometer array, Multi-Element Radio Linked Interferometer Network (MERLIN) in the OH main lines at 1665and 1667-MHz, in addition to the OH satellite line at 1720-MHz. The results of this study reveal the small upper limit to the size of emission in the 1665-MHz line with an estimated total intensity of ∼ 4 Jy. We did not detect any emission from the 1667-MHz and 1720-MHz lines. The full polarization mode of MERLIN enables us to investigate the magnetic field in the OH maser region. In this transition, a Zeeman pair is identified from which a magnetic strength of ∼ −1.5 mG is inferred. Our results show that IRAS 06056+2131 is highly polarized, with ∼ 96 % circular polarization and ∼ 6 % linear polarization. The linear polarization angle is ∼ 29◦, implying a magnetic field which could be aligned with the outflow direction detected toward this region, but the actual magnetic field direction has an uncertainty of up to 110◦ due to the possible effects of Faraday rotation. The star forming evolutionary status of the embedded proto-stellar object is discussed.

中文翻译：

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面向 IRAS 06056+2131 的 OH 脉泽：极化参数和演化状态

我们展示了对大质量恒星形成区 IRAS 06056+2131 的 OH 脉泽发射的高角分辨率观测。除了 1720-MHz 的 OH 卫星线路外，这些观测是使用英国无线电干涉仪阵列、多元素无线电链接干涉仪网络 (MERLIN) 在 1665 和 1667-MHz 的 OH 干线上进行的。这项研究的结果揭示了 1665-MHz 线中发射大小的小上限，估计总强度约为 4 Jy。我们没有检测到来自 1667-MHz 和 1720-MHz 线路的任何发射。MERLIN 的全极化模式使我们能够研究 OH 脉泽区域的磁场。在这个转变中，确定了一个塞曼对，从中推断出大约 -1.5 mG​​ 的磁场强度。我们的结果表明 IRAS 06056+2131 是高度极化的，〜 96 % 圆极化和〜 6 % 线极化。线性极化角约为 29°，这意味着磁场可以与朝向该区域检测到的流出方向对齐，但由于法拉第旋转的可能影响，实际磁场方向具有高达 110° 的不确定性。讨论了嵌入的原恒星天体的恒星形成演化状况。