Magnetic field could play a role in the formation and early evolution of non-spherical planetary nebulae (PNe). The predominant source of information of the magnetic fields in PNe is the polarization observations of maser emission. To date, distinct and/or possible Zeeman pairs have only been reported towards four PNe by measuring the OH ground-state transitions at 1.6–1.7 GHz. With the C-band (4–8 GHz) receiving system of the Shanghai TianMa 65-m radio telescope, we aim to search for possible Zeeman pairs of the PNe towards which the OH excited-state 6.035 GHz maser lines have been detected. For the young PN K 3-35, a new emission component near V_LSR = 20.5 km s⁻¹, which is currently the strongest (I_peak ∼ 0.3 Jy) among the four components towards K 3-35 is detected. A clear S-shaped feature corresponding to this new emission component is observed in the Stokes V spectrum. Frequency shifts are seen between the fitted left-hand circular polarization and right-hand circular polarization emission peaks for the two emission components near V_LSR = 19.7 and 20.5 km s⁻¹. If the S-shaped profile and the frequency shifts are the results of Zeeman-splitting, the line-of-sight magnetic field strengths of +2.9 ± 0.6 and +4.5 ± 0.4 mG can be inferred for these two emission components, respectively.

中文翻译：

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在年轻的行星状星云K 3-35中搜索OH 6.035 GHz线的塞曼分裂

磁场可能在非球形行星状星云（PNe）的形成和早期演化中起作用。PNe中磁场的主要信息来源是maser发射的极化观测。迄今为止，通过测量1.6–1.7 GHz的OH基态跃迁，仅报告了四个PNe不同和/或可能的Zeeman对。利用上海天马65米射电望远镜的C波段（4–8 GHz）接收系统，我们旨在搜索可能被检测到的OH激发态6.035 GHz maser线的PNe的塞曼对。对于年轻的PN K 3-35，在V _LSR  = 20.5 km s ^-1附近有一个新的发射分量，这是目前最强的（I_峰值 在朝向K 3-35的四个分量中检测到〜0.3 Jy）。在斯托克斯V光谱中观察到了与该新发射分量相对应的清晰S形特征。在V _LSR  = 19.7和20.5 km s ^-1附近，两个发射分量的拟合左旋圆极化和右旋圆极化发射峰之间出现了频移。如果S形轮廓和频移是塞曼分裂的结果，则对于这两个发射分量，可以分别得出+2.9±0.6和+4.5±0.4 mG的视线磁场强度。