中德$λ$ 6厘米银河面偏振巡天五.大型超新星遗迹
A Sino-German $λ$6\ cm polarization survey of the Galactic plane. V. Large supernova remnants
摘要：
以高频率观测大型超新星遗迹（SNRs）是罕见的，但提供了有关其物理性质的有价值的信息。利用乌鲁木齐$λ$ 6 cm银道面偏振巡天的观测资料，以9 $\farcm$ 5为角分辨率，研究了16个大信噪比的银道面偏振和总强度特性。我们提取了乌鲁木齐$λ$ 6 cm大信噪比的总强度图和线偏振图，得到了它们的积分通量密度，并结合以前公布的不同频率的通量密度推导了射电频谱。特别是，Effelsberg $λ$ 11 cm和$λ$ 21 cm测量数据用于计算积分通量密度。$λ$ 6\ cm极化数据还描绘了SNR的磁场结构。我们在$λ$ 6 cm处给出了SNR G106.3+2.7、G114.3+0.3、G116.5+1.1、G166.0+4.3的第一个总强度图（VRO 42.05.01），G205.5+0.5（麒麟座星云）和G206.9+2.3（PKS 0646+06）和在$λ$ 6 cm处的SNR G82.2+5.3（W 63），G106.3+2.7，G114.3+0.3，G116.5+1.1，G166.0+4.3（VRO 42.05.01）、G205.5+0.5（麒麟座星云）和G206.9+2.3（PKS 0646+06）。大多数新得到的积分射电谱与以前的结果是一致的。乌鲁木齐$λ$ 6 cm、Effelsberg $λ$ 11 cm和$λ$ 21 cm观测获得的新通量密度对确定SNR G65.1+0.6、G69.0+2.7（CTB 80）、G93.7-0.2和G114.3+0.3的光谱至关重要。我们发现G192.8 $-$ 1.1（PKS 0607+17）由背景源、\ion{H}{II}区和热性质的扩展漫发射组成，并得出G192.8 $-$ 1.1不是信噪比的结论。
英文摘要：
Observations of large supernova remnants (SNRs) at high frequencies are rare, but provide valuable information about their physical properties. The total intensity and polarization properties of 16 large SNRs in the Galactic plane were investigated based on observations of the Urumqi $λ$6\ cm polarization survey of the Galactic plane with an angular resolution of 9$\farcm$5. We extracted total intensity and linear polarization maps of large SNRs from the Urumqi $λ$6\ cm survey, obtained their integrated flux densities, and derived the radio spectra in context with previously published flux densities at various frequencies. In particular, Effelsberg $λ$11\ cm and $λ$21\ cm survey data were used for calculating integrated flux densities. The $λ$6\ cm polarization data also delineate the magnetic field structures of the SNRs. We present the first total intensity maps at $λ$6\ cm for SNRs G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula) and G206.9+2.3 (PKS 0646+06) and the first polarization measurements at $λ$6\ cm for SNRs G82.2+5.3 (W63), G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula) and G206.9+2.3 (PKS 0646+06). Most of the newly derived integrated radio spectra are consistent with previous results. The new flux densities obtained from the Urumqi $λ$6\ cm, Effelsberg $λ$11\ cm and $λ$21\ cm surveys are crucial to determine the spectra of SNR G65.1+0.6, G69.0+2.7 (CTB 80), G93.7-0.2 and G114.3+0.3. We find that G192.8$-$1.1 (PKS 0607+17) consists of background sources, \ion{H}{II} regions and the extended diffuse emission of thermal nature, and conclude that G192.8$-$1.1 is not a SNR.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
