450 d of Type II SN 2013ej in optical and near-infrared

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/102022

Title:	450 d of Type II SN 2013ej in optical and near-infrared
Authors:	陳婷琬;Yuan, Fang;Jerkstrand, A.;Valenti, S.;Sollerman, J.;Seitenzahl, I. R.;Pastorello, A.;Schulze, S.;Chen, T.-W.;Childress, M. J.;Fraser, M.;Fremling, C.;Kotak, R.;Ruiter, A. J.;Schmidt, B. P.;Smartt, S. J.;Taddia, F.;Terreran, G.;Tucker, B. E.;Barbarino, C.;Benetti, S.;Elias-Rosa, N.;Gal-Yam, A.;Howell, D. A.;Inserra, C.;Kankare, E.;Lee, M. Y.;Li, K. L.;Maguire, K.;Margheim, S.;Mehner, A.;Ochner, P.;Sullivan, M.;Tomasella, L.;Young, D. R.
Contributors:	理學院天文研究所
Keywords:	Astrophysics;Emission;Light curve;Luminosity;Massive stars;Near infrared radiation;Nebulae;Optics;Photometry;Photosphere;Spectrum analysis;Star & galaxy formation;Supernovae;supernovae: general;supernovae: individual: SN 2013ej
Date:	2016-09-11
Issue Date:	2026-04-21 14:57:06 (UTC+8)
Publisher:	Oxford University Press;London: Oxford University Press (OUP)
Abstract:	摘要： We present optical and near-infrared photometric and spectroscopic observations of SN 2013ej, in galaxy M74, from 1 to 450 d after the explosion. SN 2013ej is a hydrogen-rich supernova, classified as a Type IIL due to its relatively fast decline following the initial peak. It has a relatively high peak luminosity (absolute magnitude M V = −17.6) but a small 56Ni production of ∼0.023 M⊙. Its photospheric evolution is similar to other Type II SNe, with shallow absorption in the H α profile typical for a Type IIL. During transition to the radioactive decay tail at ∼100 d, we find the SN to grow bluer in B − V colour, in contrast to some other Type II supernovae. At late times, the bolometric light curve declined faster than expected from 56Co decay and we observed unusually broad and asymmetric nebular emission lines. Based on comparison of nebular emission lines most sensitive to the progenitor core mass, we find our observations are best matched to synthesized spectral models with a M ZAMS = 12–15 M⊙ progenitor. The derived mass range is similar to but not higher than the mass estimated for Type IIP progenitors. This is against the idea that Type IIL are from more massive stars. Observations are consistent with the SN having a progenitor with a relatively low-mass envelope. 出版者： London: Oxford University Press (OUP) 出版日期： 2016-09-11 出處： Monthly Notices of the Royal Astronomical Society, 2016-09, Vol.461 (2), p.2003-2018 資源來源： Alma/SFX Local Collection 版權： 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2016 版權： Copyright Oxford University Press, UK Sep 11, 2016 識別號： ISSN: 0035-8711 識別號： ISSN: 1365-2966 識別號： ISSN: 1365-8711 識別號： EISSN: 1365-2966 識別號： DOI: 10.1093/mnras/stw1419
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

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