SN 2009ip at late times - an interacting transient at +2 years
Morgan Fraser, Rubina Kotak, Andrea Pastorello, Anders Jerkstrand, Stephen J. Smartt, Ting-Wan Chen, Michael Childress, Gerard Gilmore, Cosimo Inserra, Erkki Ka… 展开作者
Morgan Fraser, Rubina Kotak, Andrea Pastorello, Anders Jerkstrand, Stephen J. Smartt, Ting-Wan Chen, Michael Childress, Gerard Gilmore, Cosimo Inserra, Erkki Kankare, Steve Margheim, Seppo Mattila, Stefano Valenti, Christopher Ashall, Stefano Benetti, Maria Teresa Botticella, Franz Erik Bauer, Heather Campbell, Nancy Elias-Rosa, Mathilde Fleury, Avishay Gal-Yam, Stephan Hachinger, D. Andrew Howell, Laurent Le Guillou, Pierre-François Léget, Antonia Morales-Garoffolo, Joe Polshaw, Susanna Spiro, Mark Sullivan, Stefan Taubenberger, Massimo Turatto, Emma S. Walker, David R. Young, Bonnie Zhang
We present photometric and spectroscopic observations of the interacting transient SN 2009ip taken during the 2013 and 2014 observing seasons. We characterise the photometric evolution as a steady and smooth decline in all bands, with a decline rate that is slower than expected for a solely $^{56}$Co-powered supernova at late phases. No further outbursts or eruptions were seen over a two year period from 2012 December until 2014 December. SN 2009ip remains brighter than its historic minimum from pre-discovery images. Spectroscopically, SN 2009ip continues to be dominated by strong, narrow ($\lesssim$2000 km~s$^{-1}$) emission lines of H, He, Ca, and Fe. While we make tenuous detections of [Fe~{\sc ii}] $λ$7155 and [O~{\sc i}] $λλ$6300,6364 lines at the end of 2013 June and the start of 2013 October respectively, we see no strong broad nebular emission lines that could point to a core-collapse origin. In general, the lines appear relatively symmetric, with the exception of our final spectrum in 2014 May, when we observe the appearance of a redshifted shoulder of emission at +550 km~s$^{-1}$. The lines are not blue-shifted, and we see no significant near- or mid-infrared excess. From the spectroscopic and photometric evolution of SN 2009ip until 820 days after the start of the 2012a event, we still see no conclusive evidence for core-collapse, although whether any such signs could be masked by ongoing interaction is unclear.
Exploring stellar evolution with Luminous Red Novae and Interacting Gap Transients
Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB)（巴塞罗那大学宇宙科学研究所）；Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB)（巴塞罗那大学量子物理与天体物理学系）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究院）
SU Lyn是一个由一颗白矮星和一颗红巨星组成的双星系统。虽然已知它在X射线波长下是明亮和可变的，但它的光学对应物看起来是一个没有突出发射线的红巨星。由于缺乏相互作用系统的典型光学特征，该系统被归类为隐藏的共生星。我们提出的光学监测系统的结果。虽然SU Lyn没有表现出实质性的光度变化，但光谱观测揭示了一种复杂的行为。该系统表现出很强的发射线的变化，包括天鹅座P配置文件，不断变化的线发射环境，和变量变红。X射线和光学观测都表明，SU Lyn的组件在过去12年的监测中只相互作用了很短的时间。我们第一次表明，SU Lyn在X射线明亮时类似于一个经典的共生星，之后仍然隐藏。我们还讨论了红巨星目前的演化状态，以及系统未来可能的演化。我们认为，苏林可能是一个经典的，持久的共生系统的祖先。
Circumbinary Discs as the Origin of Circumstellar Material around Interacting H-poor Supernovae and Fast Blue Optical Transients
Graduate Institute for Advanced Studies, SOKENDAI（SOKENDAI 高级研究研究生院）；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）；Department of Physics and Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学物理系与哥伦比亚天体物理学实验室）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；School of Physics and Astronomy, Monash University（莫纳什大学物理与天文学学院）
