SN 2007uy - metamorphosis of an aspheric Type Ib explosion
Rupak Roy, Brijesh Kumar, Justyn R. Maund, Patricia Schady, Felipe Olivares E., Daniele Malesani, Giorgos Leloudas, Sumana Nandi, Nial Tanvir, Dan Milisavljevic… 展开作者
Rupak Roy, Brijesh Kumar, Justyn R. Maund, Patricia Schady, Felipe Olivares E., Daniele Malesani, Giorgos Leloudas, Sumana Nandi, Nial Tanvir, Dan Milisavljevic, Jens Hjorth, Kuntal Misra, Brajesh Kumar, S. B. Pandey, Ram Sagar, H. C. Chandola
备注：
22 pages, 13 figures, accepted for publication in MNRAS
Ibc型超新星是罕见的，这些爆炸的详细特征只研究了少数事件。与II型SNe不同，Ibc型的祖先从未在爆炸前的图像中被发现。因此，为了了解其前身的性质和爆炸的特征，调查近因事件是必要的。本文介绍了对NGC 2770（$\sim$ 29.5 Mpc）星系中的Ib型SN 2007 uy的多波长观测结果。测光观测的分析显示，这是一个能量极大的事件，峰值绝对R波段星等为$-18.5\pm0.16$，比观测良好的Ibc型事件的平均值（$-17.6\pm0.6$）亮约1等。SN是高度熄灭的，E（B-V）= 0.63 $\pm$ 0.15等，主要是由于宿主星系中存在的前景物质。从光学光变曲线模型，我们确定，约0.3 M $_{\odot}$放射性$^{56}$镍产生和大约4.4 M $_{\odot}$材料喷射在此爆炸释放的能量$\sim 15\times10^{51}$ erg，表明事件是一个充满活力的。通过光学光谱，我们已经注意到一个明确的非球面演变的几个线形成区域，但没有依赖性的不对称性被认为是对分布的$^{56}$ Ni内喷出物。SN冲击波与环爆物质的相互作用在射电跟踪中明显可见，在早期阶段呈现出同步加速器自吸收（SSA）为主的光变曲线，并有自由吸收（FFA）的贡献。假设一个WR星，风速$\ga 10^3 {\rm km s}^{-1}$，作为一个祖先，我们推导出一个下限的质量损失率推断从无线电数据为$\dot{M} \ga 2.4\times10^{-5}$ M $_{\odot}$，年$^{-1}$，这是一致的结果，获得的其他Ibc型超新星明亮的无线电频率。
英文摘要：
The supernovae of Type Ibc are rare and the detailed characteristics of these explosions have been studied only for a few events. Unlike Type II SNe, the progenitors of Type Ibc have never been detected in pre-explosion images. So, to understand the nature of their progenitors and the characteristics of the explosions, investigation of proximate events are necessary. Here we present the results of multi-wavelength observations of Type Ib SN 2007uy in the nearby ($\sim$ 29.5 Mpc) galaxy NGC 2770. Analysis of the photometric observations revealed this explosion as an energetic event with peak absolute R band magnitude $-18.5\pm0.16$, which is about one mag brighter than the mean value ($-17.6\pm0.6$) derived for well observed Type Ibc events. The SN is highly extinguished, E(B-V) = 0.63$\pm$0.15 mag, mainly due to foreground material present in the host galaxy. From optical light curve modeling we determine that about 0.3 M$_{\odot}$ radioactive $^{56}$Ni is produced and roughly 4.4 M$_{\odot}$ material is ejected during this explosion with liberated energy $\sim 15\times10^{51}$ erg, indicating the event to be an energetic one. Through optical spectroscopy, we have noticed a clear aspheric evolution of several line forming regions, but no dependency of asymmetry is seen on the distribution of $^{56}$Ni inside the ejecta. The SN shock interaction with the circumburst material is clearly noticeable in radio follow-up, presenting a Synchrotron Self Absorption (SSA) dominated light curve with a contribution of Free Free Absorption (FFA) during the early phases. Assuming a WR star, with wind velocity $\ga 10^3 {\rm km s}^{-1}$, as a progenitor, we derive a lower limit to the mass loss rate inferred from the radio data as $\dot{M} \ga 2.4\times10^{-5}$ M$_{\odot}$, yr$^{-1}$, which is consistent with the results obtained for other Type Ibc SNe bright at radio frequencies.
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University of Turku（图尔库大学）；Cosmic Dawn Center (DAWN)（宇宙黎明中心 (DAWN)）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Aalto University Department of Electronics and Nanoengineering（阿尔托大学电子与纳米工程系）；Kyoto University（京都大学）；INAF Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所 (ICE, CSIC)）；UCD School of Physics（都柏林大学物理学院）；Institut d'Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究 institute (IEEC)）；Finnish Centre for Astronomy with ESO (FINCA)（芬兰ESO天文学中心 (FINCA)）；European University Cyprus（塞浦路斯欧洲大学）；Stockholm University（斯德哥尔摩大学）
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University of Virginia（弗吉尼亚大学）；Virginia Institute for Theoretical Astronomy, University of Virginia（弗吉尼亚理论天文学研究所）；National Radio Astronomy Observatory（国家射电天文台）；South African Astronomical Observatory（南非天文台）；Department of Astronomy, University of Cape Town（开普敦大学天文学系）；NITheCS National Institute for Theoretical and Computational Sciences, South Africa（南非理论与计算科学国家研究所）；INAF–Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）
University of Florida（佛罗里达大学）；Center for Astrophysics | Harvard & Smithsonian（哈佛-史密森尼天体物理中心）；California Institute of Technology（加州理工学院）；The University of Tokyo（东京大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）
