SN1987A的残留物在（亚）mm波长处显示
The remnant of SN1987A revealed at (sub-)mm wavelengths
摘要：
超新星1987 A（SN 1987 A）在大麦云（LMC）中爆炸。它的邻近性和快速演化使其成为超新星遗迹发展早期阶段的独特案例研究。一个特别令人感兴趣的方面是SN 1987 A中可能形成的尘埃，因为SNe可能对高红移的尘埃有显着贡献。目的：我们探讨了SN 1987 A及其环暴介质的属性，在毫米和亚毫米波长，弥合现有的无线电和红外（IR）观测的同步辐射和尘埃发射之间的差距。研究方法：SN 1987 A于2005年7月由澳大利亚望远镜紧凑阵列（ATCA）以3.2毫米观测，并于2007年5月由阿塔卡马探路者实验（APEX）以0.87毫米观测。本文首次给出了SN 1987 A在这些波长下的图像和亮度测量结果。结果：SN 1987 A在3.2 mm（5”射束）和0.87 mm（18”射束）处被检测为11.2 +/- 2.0 mJy和21 +/- 4 mJy的未分辨点源。这些通量密度与幂律无线电频谱和修正黑体尘埃排放的外推完全一致。这限制了自由-自由发射的存在，这与SN 1987 A电离喷出物的预期自由-自由发射相似。在0.87 mm处观察到邻近的较暗发射，向西南方向延伸约0.5'。这可能是超新星前身的风的影响，当它仍然是一个红色的超巨星在致密的介质。结论：我们已经建立了一个连续的光谱能量分布从SN 1987 A和它的周围环境，连接红外和无线电数据。这限制了来自电离等离子体的贡献。我们的亚毫米图像揭示了SN 1987 A周围冷尘埃分布的复杂性，但为SN喷出物中的新合成尘埃留下了空间。
英文摘要：
Context: Supernova 1987A (SN1987A) exploded in the Large Magellanic Cloud (LMC). Its proximity and rapid evolution makes it a unique case study of the early phases in the development of a supernova remnant. One particular aspect of interest is the possible formation of dust in SN1987A, as SNe could contribute significantly to the dust seen at high redshifts. Aims: We explore the properties of SN1987A and its circumburst medium as seen at mm and sub-mm wavelengths, bridging the gap between extant radio and infrared (IR) observations of respectively the synchrotron and dust emission. Methods: SN1987A was observed with the Australia Telescope Compact Array (ATCA) at 3.2 mm in July 2005, and with the Atacama Pathfinder EXperiment (APEX) at 0.87 mm in May 2007. We present the images and brightness measurements of SN1987A at these wavelengths for the first time. Results: SN1987A is detected as an unresolved point source of 11.2 +/- 2.0 mJy at 3.2 mm (5" beam) and 21 +/- 4 mJy at 0.87 mm (18" beam). These flux densities are in perfect agreement with extrapolations of the powerlaw radio spectrum and modified-blackbody dust emission, respectively. This places limits on the presence of free-free emission, which is similar to the expected free-free emission from the ionized ejecta from SN1987A. Adjacent, fainter emission is observed at 0.87 mm extending ~0.5' towards the south-west. This could be the impact of the supernova progenitor's wind when it was still a red supergiant upon a dense medium. Conclusions: We have established a continuous spectral energy distribution for the emission from SN1987A and its immediate surroundings, linking the IR and radio data. This places limits on the contribution from ionized plasma. Our sub-mm image reveals complexity in the distribution of cold dust surrounding SN1987A, but leaves room for freshly synthesized dust in the SN ejecta.
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