CONSTRAINING EXPLOSION TYPE OF YOUNG SUPERNOVA REMNANTS USING 24 μm EMISSION MORPHOLOGY

CONSTRAINING EXPLOSION TYPE OF YOUNG SUPERNOVA REMNANTS USING 24 μm EMISSION MORPHOLOGY
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利用 24μm 发射形态约束年轻超新星遗迹的爆炸类型

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发表时间：
2013
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通讯作者：
E. Figueroa
E. Figueroa
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文献类型：
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作者：
C. Peters;L. Lopez;E. Ramirez;K. Stassun;E. Figueroa

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确定超新星遗迹（SNRs）的爆炸类型可能具有挑战性，因为SNRs有数百至数千年的历史，超新星是根据爆炸后几天的光谱特性进行分类的。先前对银河系和大麦哲伦云超新星的热X射线辐射的研究表明，Ia型和核心坍缩（CC）超新星具有统计上不同的对称性，因此可以根据它们的X射线形态对这些源进行分类。在这封信中，我们扩展了相同的技术，多极扩展技术，使用功率比，红外（IR）图像的信噪比，以测试它们是否可以使用其温暖的尘埃排放的对称性，以及类型。我们分析了斯皮策空间望远镜多波段成像光度计24 μm观测到的先前使用的X射线样品，我们发现这两类SNR根据它们的IR形态分开。Ia型超新星在统计上比CC型超新星更圆和镜像对称，这可能是由于不同的星周环境和祖先的爆炸几何形状。从广义上讲，我们的工作表明，红外辐射保留了信息的爆炸起源的SNR和提供了一种新的方法来类型的SNR的基础上，红外形态。
Determination of the explosion type of supernova remnants (SNRs) can be challenging, as SNRs are hundreds to thousands of years old and supernovae are classified based on spectral properties days after explosion. Previous studies of thermal X-ray emission from Milky Way and Large Magellanic Cloud SNRs have shown that Type Ia and core-collapse (CC) SNRs have statistically different symmetries, and thus these sources can be typed based on their X-ray morphologies. In this Letter, we extend the same technique, a multipole expansion technique using power ratios, to infrared (IR) images of SNRs to test whether they can be typed using the symmetry of their warm dust emission as well. We analyzed archival Spitzer Space Telescope Multiband Imaging Photometer 24 μm observations of the previously used X-ray sample, and we find that the two classes of SNRs separate according to their IR morphologies. The Type Ia SNRs are statistically more circular and mirror symmetric than the CC SNRs, likely due to the different circumstellar environments and explosion geometries of the progenitors. Broadly, our work indicates that the IR emission retains information of the explosive origins of the SNR and offers a new method to type SNRs based on IR morphology.
SPITZER SURVEY OF THE LARGE MAGELLANIC CLOUD, SURVEYING THE AGENTS OF A GALAXY'S EVOLUTION (SAGE). IV. DUST PROPERTIES IN THE INTERSTELLAR MEDIUM
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