标题： JCMT BISTRO调查：IC 348成星区域的磁场 显示英文标题

标题： The JCMT BISTRO Survey: The Magnetic Fields of the IC 348 Star-forming Region

摘要： 我们介绍了850$\mu$微米极化观测结果，这是Perseus分子云中IC 348恒星形成区域的一部分，属于B-fields In STar-forming Region Observation (BISTRO)调查。 我们研究了两个核（HH 211 MMS和IC 348 MMS）以及IC 348的丝状结构的磁场特性。 我们发现该区域的整体磁场倾向于比丝状结构更垂直。 极化分数随着强度的增加而减少，我们通过幂律和Rice分布拟合的平均值估计了这一趋势。 这些核的幂指数远小于1，表明这些核中可能存在微米大小的颗粒增长。 我们还分别应用Davis-Chandrasekhar-Fermi方法及其用于压缩介质的替代版本，测量了这两个核和丝状区域的磁场强度。 估计的质量-通量比分别为0.45-2.20和0.63-2.76，分别对应于HH 211 MMS和IC 348 MMS，而丝状结构的比值为0.33-1.50。 这一结果可能表明，在该区域的核尺度（$\sim$0.05 pc）发生了从亚临界到超临界条件的转变。 此外，我们研究了核的能量平衡，发现与磁场相比，湍流的相对强度对于IC 348 MMS比HH 211 MMS更强。 这一结果可能可以解释这两个核内部的不同配置：HH 211 MMS中的单个原恒星系统和IC 348 MMS中的多个原恒星。 显示英文摘要

摘要： We present 850 $\mu$m polarization observations of the IC 348 star-forming region in the Perseus molecular cloud as part of the B-fields In STar-forming Region Observation (BISTRO) survey. We study the magnetic properties of two cores (HH 211 MMS and IC 348 MMS) and a filamentary structure of IC 348. We find that the overall field tends to be more perpendicular than parallel to the filamentary structure of the region. The polarization fraction decreases with intensity, and we estimate the trend by power-law and the mean of the Rice distribution fittings. The power indices for the cores are much smaller than 1, indicative of possible grain growth to micron size in the cores. We also measure the magnetic field strengths of the two cores and the filamentary area separately by applying the Davis-Chandrasekhar-Fermi method and its alternative version for compressed medium. The estimated mass-to-flux ratios are 0.45-2.20 and 0.63-2.76 for HH 211 MMS and IC 348 MMS, respectively, while the ratios for the filament is 0.33-1.50. This result may suggest that the transition from subcritical to supercritical conditions occurs at the core scale ($\sim$ 0.05 pc) in the region. In addition, we study the energy balance of the cores and find that the relative strength of turbulence to the magnetic field tends to be stronger for IC 348 MMS than HH 211 MMS. The result could potentially explain the different configurations inside the two cores: a single protostellar system in HH 211 MMS and multiple protostars in IC 348 MMS.