SN 2009ip at late times - An interacting transient at +2 years

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/101760

Title:	SN 2009ip at late times - An interacting transient at +2 years
Authors:	陳婷琬;Fraser, Morgan;Kotak, Rubina;Pastorello, Andrea;Jerkstrand, Anders;Smartt, Stephen J.;Chen, Ting-Wan;Childress, Michael;Gilmore, Gerard;Inserra, Cosimo;Kankare, Erkki;Margheim, Steve;Mattila, Seppo;Valenti, Stefano;Ashall, Christopher;Benetti, Stefano;Botticella, Maria Teresa;Bauer, Franz Erik;Campbell, Heather;Elias-Rosa, Nancy;Fleury, Mathilde;Gal-Yam, Avishay;Hachinger, Stephan;Howell, D. Andrew;Le Guillou, Laurent;Léget, Pierre-François;Morales-Garoffolo, Antonia;Polshaw, Joe;Spiro, Susanna;Sullivan, Mark;Taubenberger, Stefan;Turatto, Massimo;Walker, Emma S.;Young, David R.;Zhang, Bonnie
Contributors:	理學院天文研究所
Keywords:	Astrophysics;Bands;Emission spectroscopy;Emissions;Evolution;Historic;Nebulae;Phases;Photometry;Red shift;Spectroscopy;Spectrum analysis;Star & galaxy formation;Supernovae;Supernovas
Date:	2015-11-11
Issue Date:	2026-04-21 14:43:24 (UTC+8)
Publisher:	Oxford University Press;London: Oxford University Press
Abstract:	摘要： We present photometric and spectroscopic observations of the interacting transient SN 2009ip taken during the 2013 and 2014 observing seasons. We characterize the photometric evolution as a steady and smooth decline in all bands, with a decline rate that is slower than expected for a solely 56Co-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 (≲2000 km s− 1) emission lines of H, He, Ca, and Fe. While we make tenuous detections of [Fe ii] λ7155 and [O i] λλ6300, 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 blueshifted, and we see no significant near- or mid-infrared excess. From the spectroscopic and photometric evolution of SN 2009ip until 820 d 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. 出版者： London: Oxford University Press 出版日期： 2015-11-11 出處： Monthly notices of the Royal Astronomical Society, 2015-11, Vol.453 (4), p.3886-3905 資源來源： Alma/SFX Local Collection 版權： 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2015 版權： Copyright Oxford University Press, UK Nov 11, 2015 識別號： ISSN: 0035-8711 識別號： ISSN: 1365-8711 識別號： ISSN: 1365-2966 識別號： EISSN: 1365-2966 識別號： DOI: 10.1093/mnras/stv1919
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

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