Magnetic fields are ubiquitous and essential in star formation. In particular, their role in regulating formation of stars across diverse environments like H ii regions needs to be well understood. In this study, we present magnetic field properties toward the S235 complex using near-infrared (NIR) H-band polarimetric observations, obtained with the Mimir and POLICAN instruments. We selected 375 background stars in the field through combination of Gaia distances and extinctions from NIR colors. The plane-of-sky (POS) magnetic field orientations inferred from starlight polarization angles reveal a curved morphology tracing the spherical shell of the H ii region. The large-scale magnetic field traced by Planck is parallel to the Galactic plane. We identified 11 dense clumps using 1.1 mm dust emission, with masses between 33 and 525 M _⊙. The clump-averaged POS magnetic field strengths were estimated to be between 36 and 121 μG, with a mean of ∼65 μG. The mass-to-flux ratios for the clumps are found to be subcritical with turbulent Alfvn Mach numbers less than 1, indicating a strongly magnetized region. The clumps show scaling of magnetic field strength versus density with a power-law index of 0.52 0.07, similar to ambipolar diffusion models. Our results indicate that the S235 complex is a region where stellar feedback triggers new stars, and the magnetic fields regulate the rate of new star formation.

磁场无处不在，在恒星形成过程中必不可少。特别是，需要很好地理解它们在调节跨不同环境（如 H ii区域）的恒星形成中的作用。在这项研究中，我们使用Mimir 和 POLICAN 仪器获得的近红外 (NIR) H波段极化观测来展示 S235 复合体的磁场特性。我们通过结合盖亚距离和 NIR 颜色的消光在现场选择了 375 颗背景恒星。从星光偏振角推断出的天空平面 (POS) 磁场方向揭示了跟踪 H ii球壳的弯曲形态地区。普朗克追踪的大尺度磁场平行于银河平面。我们使用 1.1 毫米的尘埃发射确定了 11 个密集团块，质量在 33 到 525 M _{⊙ 之间}。团块平均 POS 磁场强度估计在 36 到 121 μ G 之间，平均值约为 65 μG. 发现团块的质量与通量比处于亚临界状态，湍流 Alfvn 马赫数小于 1，表明存在强磁化区域。团块显示磁场强度与密度的比例关系，幂律指数为 0.52 0.07，类似于双极扩散模型。我们的结果表明，S235 复合体是一个恒星反馈触发新恒星的区域，磁场调节新恒星形成的速度。