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|Title:||Supersolar Ni/Fe production in the Type IIP SN 2012ec||Authors:||Jerkstrand, A.
Smartt, S. J.
Chen, T. -W.
BOTTICELLA, MARIA TERESA
DELLA VALLE, Massimo
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||448||Issue:||3||First Page:||2482||Abstract:||SN 2012ec is a Type IIP supernova (SN) with a progenitor detection and comprehensive photospheric phase observational coverage. Here, we present Very Large Telescope and Public ESO Spectroscopic Survey of Transient Objects observations of this SN in the nebular phase. We model the nebular [O I] λλ6300, 6364 lines and find their strength to suggest a progenitor main-sequence mass of 13-15 M<SUB>☉</SUB>. SN 2012ec is unique among hydrogen-rich SNe in showing a distinct line of stable nickel [Ni II] λ7378. This line is produced by <SUP>58</SUP>Ni, a nuclear burning ash whose abundance is a sensitive tracer of explosive burning conditions. Using spectral synthesis modelling, we use the relative strengths of [Ni II] λ7378 and [Fe II] λ7155 (the progenitor of which is <SUP>56</SUP>Ni) to derive a Ni/Fe production ratio of 0.20 ± 0.07 (by mass), which is a factor 3.4 ± 1.2 times the solar value. High production of stable nickel is confirmed by a strong [Ni II] 1.939 μm line. This is the third reported case of a core-collapse SN producing a Ni/Fe ratio far above the solar value, which has implications for core-collapse explosion theory and galactic chemical evolution models.||Acknowledgments:||We thank S. Sim, B. Müller, K. Nomoto, and R. Fesen for discussion, and R. Sethuram for contributing the NGC 1084 galaxy spectrum. We thank R. Kotak for use of LT data, P. Meikle for providing spectra of SN 2002hh and J. Andrews for providing spectra on SN 2007it. We have made use of the SUSPECT and WISEREP (Yaron Gal-Yam 2012 ) databases. This work is based in part on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects) ESO program 188.D-3003. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreements no.  (SJS) and no.  and STFC grants ST/I001123/1 and ST/L000709/1 (SJS).||URI:||http://hdl.handle.net/20.500.12386/23898||URL:||https://academic.oup.com/mnras/article/448/3/2482/1089335||ISSN:||0035-8711||DOI:||10.1093/mnras/stv087||Bibcode ADS:||2015MNRAS.448.2482J||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Sep 26, 2020
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