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

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. and Zhang, Bonnie 2015. SN 2009ip at late times - an interacting transient at +2 years. Monthly Notices of the Royal Astronomical Society 453 (4) , pp. 3887-3905. 10.1093/mnras/stv1919

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Abstract

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.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Publisher: Oxford University Press
ISSN: 0035-8711
Date of First Compliant Deposit: 23 January 2019
Date of Acceptance: 18 August 2015
Last Modified: 31 Jan 2019 14:45
URI: http://orca.cf.ac.uk/id/eprint/118730

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