在PHANGS-MUSE星系中发现年轻、富氧的超新星遗迹
Discovery of young, oxygen-rich supernova remnants in PHANGS-MUSE galaxies
AI总结：
本文提出一种基于发射线形状的新方法，利用MUSE光谱仪在PHANGS-MUSE星系中发现307个超新星遗迹（含7个富氧SNRs），证明方法有效性并为研究富氧SNRs起源提供新样本。
摘要：
背景：超新星遗迹（SNRs）是超新星在与周围介质合并前的晚期阶段。富氧超新星遗迹是一种罕见的亚型，具有强烈的可见光氧发射。目的：我们提出一种利用现代可见光积分视场单元能力、基于SNR发射线形状的新方法来探测SNRs。方法：我们使用甚大望远镜上的中分辨率积分视场光谱仪MUSE，搜索具有加宽发射线的未解析激波区域。光谱分辨率使激波发射源能够根据线宽与光致电离源区分开。结果：我们发现了307个超新星遗迹，包括7个富氧SNRs。对于所有富氧SNRs，我们观测到[O III]λλ4959,5007发射双线。此外，我们不同程度地观测到[O I]λλ6300,6364、[O II]λλ7320,7330、Hα+[N II]λ6583和[S II]λλ6717,6731的发射。富氧SNRs的线宽通常比本文样本中的其他SNRs更宽。氧发射复合体让人联想到SNR 4449-1和一些持久的超新星。对于富氧SNRs，我们还在其他望远镜的档案数据中搜索对应体；我们检测到多个遗迹的X射线和中红外对应体。结论：我们证明了本文提出的探测SNRs方法的有效性。此外，该方法在探测罕见的富氧SNRs方面也有效，使文献中的样本量增加了一倍。富氧SNRs的起源及其与特定超新星类型或环境的联系仍不清楚，但对这个新样本的进一步研究无疑将帮助我们阐明这些罕见遗迹。
英文摘要：
Context. Supernova remnants (SNRs) are the late stages of supernovae before their merging into the surrounding medium. Oxygen-rich supernova remnants represent a rare subtype with strong visible light oxygen emission. Aims. We present a new method to detect SNRs exploiting the capabilities of modern visible-light integral-field units based on the shapes of the SNR emission lines. Methods. We search for unresolved shocked regions with broadened emission lines using the medium-resolution integral-field spectrograph MUSE on the Very Large Telescope. The spectral resolving power allows shocked emission sources to be differentiated from photoionised sources based on the linewidths. Results. We find 307 supernova remnants, including seven O-rich SNRs. For all O-rich SNRs, we observe the [O III]λλ4959,5007 emission doublet. In addition, we observe emissions from [O I]λλ6300,6364, [O II]λλ7320,7330, Hα+[N II]λ6583 and [S II]λλ6717,6731 to varying degrees. The linewidths for the O-rich SNRs are generally broader than the rest of the SNRs in the sample of this article. The oxygen emission complexes are reminiscient of SNR 4449-1 and some long-lasting SNe. For the O-rich SNRs, we also search for counterparts in archival data of other telescopes; we detect X-ray and mid-IR counterparts for a number of remnants. Conclusions. We have shown efficacy of the method to detect SNRs presented in this article. In addition, the method is also effective in detecting the rare O-rich SNRs, doubling the sample size in the literature. The origin of O-rich SNRs and their link to specific SN types or environments is still unclear, but further work into this new sample will unquestionably help us shed light on these rare remnants.
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