Multi-frequency study of supernova remnants in the Large Magellanic Cloud Confirmation of the supernova remnant status of DEM L205
Multi-frequency study of supernova remnants in the Large Magellanic Cloud Confirmation of the supernova remnant status of DEM L205
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大麦哲伦星云中超新星遗迹的多频率研究 确认DEM L205超新星遗迹状态
DOI：
10.1051/0004-6361/201219708
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发表时间：
2012
影响因子：
6.5
通讯作者：
A. Horta
中科院分区：
文献类型：
--
作者：
P. Maggi;F. Haberl;L. Bozzetto;M. Filipović;S. Points;You;M. Sasaki;W. Pietsch;R. Gruendl;J. Dickel;R. Smith;R. Sturm;E. Crawford;A. Horta
语境。大麦哲伦星云 (LMC) 是研究超新星遗迹 (SNR) 的无偏且完整样本的理想目标。我们开始使用 XMM-Newton 对 LMC 进行 X 射线调查，结合其他波长的观测，我们将能够发现和研究比之前已知的更暗或更进化（或两者兼而有之）的遗迹。目标。我们展示了由 XMM-Newton 和 ATCA 获得的 LMC SNR 候选 DEM L205 的新 X 射线和无线电数据，以及档案光学和红外观测结果。方法。我们使用不同波长的数据来研究这个物体及其复杂的邻近区域，特别是在源周围过去和现在的恒星形成活动的背景下。我们分析 X 射线光谱，得出一些残余物的特性，例如年龄和爆炸能量。结果。在所有观察到的波长下都可以检测到超新星遗迹特征：观察到由温度 kT 在 0.2 keV 到 0.3 keV 之间的热等离子体产生的柔和且扩展的 X 射线发射。光线发射的特征是增强的[S ii]-Hα比率和壳状形态，与X射线发射相关。未或仅在近红外波长（短于 10 μm）处暂时检测到光源，但在中红外和远红外波长（24 和 70 μm）处检测到弧状发射，这可以明确地与残余物相关联。我们认为，恒星辐射和冲击波加热的尘埃的热发射是红外发射的主要贡献者。最后，扩展且微弱的非热射电发射与其他波长的残余物相关，我们发现射电光谱指数在-0.7和-0.9之间，在SNR范围内。遗迹的大小约为 79 × 64 pc，我们估计其动态年龄约为 35 000 年。结论。我们确实确认 DEM L205 作为新的 SNR。该物体是大麦哲伦地区已知最大的遗迹之一。众多的大质量恒星和最近在源头周围爆发的恒星形成强烈表明，核心塌缩超新星是该遗迹的前身。
Context. The Large Magellanic Cloud (LMC) is an ideal target for the study of an unbiased and complete sample of supernova remnants (SNRs). We started an X-ray survey of the LMC with XMM-Newton, which, in combination with observations at other wavelengths, will allow us to discover and study remnants that are either even fainter or more evolved (or both) than previously known. Aims. We present new X-ray and radio data of the LMC SNR candidate DEM L205, obtained by XMM-Newton and ATCA, along with archival optical and infrared observations. Methods. We use data at various wavelengths to study this object and its complex neighbourhood, in particular in the context of the star formation activity, past and present, around the source. We analyse the X-ray spectrum to derive some remnant’s properties, such as age and explosion energy. Results. Supernova remnant features are detected at all observed wavelengths : soft and extended X-ray emission is observed, arising from a thermal plasma with a temperature kT between 0.2 keV and 0.3 keV. Optical line emission is characterised by an enhanced [S ii]-to-Hα ratio and a shell-like morphology, correlating with the X-ray emission. The source is not or only tentatively detected at near-infrared wavelengths (shorter than 10 μm), but there is a detection of arc-like emission at mid and far-infrared wavelengths (24 and 70 μm) that can be unambiguously associated with the remnant. We suggest that thermal emission from dust heated by stellar radiation and shock waves is the main contributor to the infrared emission. Finally, an extended and faint non-thermal radio emission correlates with the remnant at other wavelengths and we find a radio spectral index between −0.7 and −0.9, within the range for SNRs. The size of the remnant is∼79 × 64 pc and we estimate a dynamical age of about 35 000 years. Conclusions. We definitely confirm DEM L205 as a new SNR. This object ranks amongst the largest remnants known in the LMC. The numerous massive stars and the recent outburst in star formation around the source strongly suggest that a core-collapse supernova is the progenitor of this remnant.
DOI：
10.1088/0004-6256/136/3/919
发表时间：
2005-06
期刊：
The Astronomical Journal
影响因子：
--
作者：
M. Meixner;K. Gordon;R. Indebetouw;J. Hora;B. Whitney;R. Blum;W. Reach;J. Bernard;M. Meade;B. Babler;C. Engelbracht;B. For;K. Misselt;U. Vijh;C. Leitherer;M. Cohen;E. Churchwell;F. Boulanger;J. Frogel;Y. Fukui;J. Gallagher;V. Gorjian;J. Harris;D. Kelly;A. Kawamura;Soyoung Kim;W. Latter;S. Madden;Ciska Markwick-Kemper;A. Mizuno;N. Mizuno;J. Mould;A. Nota;M. Oey;K. Olsen;T. Onishi;R. Paladini;N. Panagia;P. Pérez-González;H. Shibai;Sato Shuji;Linda J. Smith;L. Staveley-Smith;A. Tielens;T. Ueta;S. V. Dyk;K. Volk;M. Werner;D. Zaritsky
通讯作者：
M. Meixner;K. Gordon;R. Indebetouw;J. Hora;B. Whitney;R. Blum;W. Reach;J. Bernard;M. Meade;B. Babler;C. Engelbracht;B. For;K. Misselt;U. Vijh;C. Leitherer;M. Cohen;E. Churchwell;F. Boulanger;J. Frogel;Y. Fukui;J. Gallagher;V. Gorjian;J. Harris;D. Kelly;A. Kawamura;Soyoung Kim;W. Latter;S. Madden;Ciska Markwick-Kemper;A. Mizuno;N. Mizuno;J. Mould;A. Nota;M. Oey;K. Olsen;T. Onishi;R. Paladini;N. Panagia;P. Pérez-González;H. Shibai;Sato Shuji;Linda J. Smith;L. Staveley-Smith;A. Tielens;T. Ueta;S. V. Dyk;K. Volk;M. Werner;D. Zaritsky