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arXiv 2108.08575astro-ph.GAastro-ph.HE
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光学鉴定的超新星遗迹G107 .0+9.0的射电性质

Radio properties of the optically identified supernova remnant G107.0+9.0

Wolfgang Reich, Xuyang Gao, Patricia Reich

备注：
8 pages, 12 figures, accepted by Astronomy & Astrophysics
发表信息：
A&A 655, A10 (2021)
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摘要：

绝大多数的银河系超新星遗迹（SNRs）都是通过它们的同步辐射来探测的。最近，光学探测到直径约为3度或75 - 100 μ c的演化的SNR G107.0+9.0，并显示出微弱的相关射电发射。此SNR需要进行详细的无线电研究。我们的目标是通过分析来自Effelsberg 100米和乌鲁木齐25米射电望远镜的新数据，以及现有的无线电调查，寻找SNR G107.0+9.0的无线电发射。银河系以外的无线电信噪比，在那里混乱是罕见的，必须非常微弱，如果他们还没有被确定到目前为止。以G107.0+9.0的H $α$辐射为指导，将其射电辐射与银河系大尺度辐射分离。在22 MHz和4.8 GHz之间检测到SNR G107.0+9.0的无线电发射，具有陡峭的非热谱，这确认G107.0+9.0为SNR。它的表面亮度是已知的银河系信噪比最低的。极化发射在1.4~GHz处被清楚地检测到，但在4.8~GHz处较弱。我们解释的偏振发射所造成的法拉第屏幕与G107.0+9.0及其周围环境。其沿视线方向的有序磁场小于1~ $μ$ G。在4.8~GHz处，我们确定了沿着G107.0+9.0的西部外围的去极化细丝，其磁场强度沿着视线$B{_{||}} \sim 15~μ$ G，这需要磁场压缩。G107.0+9.0增加了目前已知的少数，进化的，大直径，低表面亮度的银河系SNR。我们已经表明，这样的对象可以成功地提取无线电连续谱调查，尽管占主导地位的大规模弥漫银河系的排放。

英文摘要：

The vast majority of Galactic supernova remnants (SNRs) were detected by their synchrotron radio emission. Recently, the evolved SNR G107.0+9.0 with a diameter of about 3~deg or 75~pc up to 100~pc in size was optically detected with an indication of faint associated radio emission. This SNR requires a detailed radio study. We aim to search for radio emission from SNR G107.0+9.0 by analysing new data from the Effelsberg 100-m and the Urumqi 25-m radio telescopes in addition to available radio surveys. Radio SNRs outside of the Galactic plane, where confusion is rare, must be very faint if they have not been identified so far. Guided by the H$α$ emission of G107.0+9.0, we separated its radio emission from the Galactic large-scale emission. Radio emission from SNR G107.0+9.0 is detected between 22~MHz and 4.8~GHz with a steep non-thermal spectrum, which confirms G107.0+9.0 as an SNR. Its surface brightness is among the lowest known for Galactic SNRs. Polarised emission is clearly detected at 1.4~GHz but is fainter at 4.8~GHz. We interpret the polarised emission as being caused by a Faraday screen associated with G107.0+9.0 and its surroundings. Its ordered magnetic field along the line of sight is below 1~$μ$G. At 4.8~GHz, we identified a depolarised filament along the western periphery of G107.0+9.0 with a magnetic field strength along the line of sight $B{_{||}} \sim 15~μ$G, which requires magnetic field compression. G107.0+9.0 adds to the currently small number of known, evolved, large-diameter, low-surface-brightness Galactic SNRs. We have shown that such objects can be successfully extracted from radio-continuum surveys despite the dominating large-scale diffuse Galactic emission.

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