SN 2009ip at late times - an interacting transient at +2 years
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.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- November 2015
- DOI:
- 10.1093/mnras/stv1919
- arXiv:
- arXiv:1502.06033
- Bibcode:
- 2015MNRAS.453.3886F
- Keywords:
-
- stars: massive;
- stars: mass loss;
- supernovae: general;
- supernovae: individual: (SN2009ip);
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- Submitted to MNRAS