Superluminous supernovae from PESSTO

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/101259

Title:	Superluminous supernovae from PESSTO
Authors:	陳婷琬;Nicholl, M.;Smartt, S. J.;Jerkstrand, A.;Inserra, C.;Anderson, J. P.;Baltay, C.;Benetti, S.;Chen, T.-W.;Elias-Rosa, N.;Feindt, U.;Fraser, M.;Gal-Yam, A.;Hadjiyska, E.;Howell, D. A.;Kotak, R.;Lawrence, A.;Leloudas, G.;Margheim, S.;Mattila, S.;McCrum, M.;McKinnon, R.;Mead, A.;Nugent, P.;Rabinowitz, D.;Rest, A.;Smith, K. W.;Sollerman, J.;Sullivan, M.;Taddia, F.;Valenti, S.;Walker, E. S.;Young, D. R.
Contributors:	理學院天文研究所
Keywords:	Astrophysics;Light;Luminosity;Radioactivity;Spectrum analysis;Supernovae;supernovae: general;supernovae: individual: LSQ12dlf;supernovae: individual: SN 2013dg;supernovae: individual: SSS120810:231802-560926;X-ray astronomy
Date:	2014-11-01
Issue Date:	2026-04-21 14:28:35 (UTC+8)
Publisher:	Oxford University Press;London: Oxford University Press
Abstract:	摘要： We present optical spectra and light curves for three hydrogen-poor superluminous supernovae followed by the Public ESO Spectroscopic Survey of Transient Objects (PESSTO). Time series spectroscopy from a few days after maximum light to 100 d later shows them to be fairly typical of this class, with spectra dominated by Ca ii, Mg ii, Fe ii, and Si ii, which evolve slowly over most of the post-peak photospheric phase. We determine bolometric light curves and apply simple fitting tools, based on the diffusion of energy input by magnetar spin-down, 56Ni decay, and collision of the ejecta with an opaque circumstellar shell. We investigate how the heterogeneous light curves of our sample (combined with others from the literature) can help to constrain the possible mechanisms behind these events. We have followed these events to beyond 100–200 d after peak, to disentangle host galaxy light from fading supernova flux and to differentiate between the models, which predict diverse behaviour at this phase. Models powered by radioactivity require unrealistic parameters to reproduce the observed light curves, as found by previous studies. Both magnetar heating and circumstellar interaction still appear to be viable candidates. A large diversity is emerging in observed tail-phase luminosities, with magnetar models failing in some cases to predict the rapid drop in flux. This would suggest either that magnetars are not responsible, or that the X-ray flux from the magnetar wind is not fully trapped. The light curve of one object shows a distinct rebrightening at around 100 d after maximum light. We argue that this could result either from multiple shells of circumstellar material, or from a magnetar ionization front breaking out of the ejecta. 其他題名： Mon. Not. R. Astron. Soc 出版者： London: Oxford University Press 出版日期： 2014-11-01 出處： Monthly notices of the Royal Astronomical Society, 2014-11, Vol.444 (3), p.2096-2113 資源來源： Alma/SFX Local Collection 版權： 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2014 版權： Copyright Oxford University Press, UK Nov 1, 2014 識別號： ISSN: 0035-8711 識別號： ISSN: 1365-2966 識別號： EISSN: 1365-2966 識別號： DOI: 10.1093/mnras/stu1579
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

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