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| 題名: | SN 2015bn: A DETAILED MULTI-WAVELENGTH VIEW of A NEARBY SUPERLUMINOUS SUPERNOVA |
| 作者: | 陳婷琬;Nicholl, M.;Berger, E.;Smartt, S. J.;Margutti, R.;Kamble, A.;Alexander, K. D.;Chen, T.-W.;Inserra, C.;Arcavi, I.;Blanchard, P. K.;Cartier, R.;Chambers, K. C.;Childress, M. J.;Chornock, R.;Cowperthwaite, P. S.;Drout, M.;Flewelling, H. A.;Fraser, M.;Gal-Yam, A.;Galbany, L.;Harmanen, J.;Holoien, T. W.-S.;Hosseinzadeh, G.;Howell, D. A.;Huber, M. E.;Jerkstrand, A.;Kankare, E.;Kochanek, C. S.;Lin, Z.-Y.;Lunnan, R.;Magnier, E. A.;Maguire, K.;McCully, C.;McDonald, M.;Metzger, B. D.;Milisavljevic, D.;Mitra, A.;Reynolds, T.;Saario, J.;Shappee, B. J.;Smith, K. W.;Valenti, S.;Villar, V. A.;Waters, C.;Young, D. R. |
| 貢獻者: | 理學院天文研究所 |
| 關鍵詞: | Astrophysics;ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;BOLOMETERS;COSMIC GAMMA BURSTS;DIAGRAMS;EMISSION;Evolution;EXPLOSIONS;GALAXIES;Gamma ray bursts;IONIZATION;Light curve;LUMINOSITY;MASS TRANSFER;NEUTRON STARS;PHOTOMETRY;Physics;Progenitors (astrophysics);Radio;RED SHIFT;SPECTRA;STELLAR WINDS;SUPERNOVAE;supernovae: general;supernovae: individual (SN 2015bn);Time;WAVELENGTHS |
| 日期: | 2016-07-20 |
| 上傳時間: | 2026-04-21 14:55:13 (UTC+8) |
| 出版者: | IOP Publishing Ltd.;United States: The American Astronomical Society |
| 摘要: | 摘要： ABSTRACT We present observations of SN 2015bn (=PS15ae = CSS141223-113342+004332 = MLS150211-113342+004333), a Type I superluminous supernova (SLSN) at redshift z = 0.1136. As well as being one of the closest SLSNe I yet discovered, it is intrinsically brighter ( ) and in a fainter galaxy ( ) than other SLSNe at . We used this opportunity to collect the most extensive data set for any SLSN I to date, including densely sampled spectroscopy and photometry, from the UV to the NIR, spanning −50 to +250 days from optical maximum. SN 2015bn fades slowly, but exhibits surprising undulations in the light curve on a timescale of 30-50 days, especially in the UV. The spectrum shows extraordinarily slow evolution except for a rapid transformation between +7 and +20-30 days. No narrow emission lines from slow-moving material are observed at any phase. We derive physical properties including the bolometric luminosity, and find slow velocity evolution and non-monotonic temperature and radial evolution. A deep radio limit rules out a healthy off-axis gamma-ray burst, and places constraints on the pre-explosion mass loss. The data can be consistently explained by a M stripped progenitor exploding with erg kinetic energy, forming a magnetar with a spin-down timescale of ∼20 days (thus avoiding a gamma-ray burst) that reheats the ejecta and drives ionization fronts. The most likely alternative scenario-interaction with ∼20 M of dense, inhomogeneous circumstellar material-can be tested with continuing radio follow-up.
其他題名： APJ
其他題名： Astrophys. J
出版者： United States: The American Astronomical Society
出版日期： 2016-07-20
出處： The Astrophysical Journal, 2016-07, Vol.826 (1), p.39--39
資源來源： Institute of Physics Journals
版權： 2016. The American Astronomical Society. All rights reserved.
版權： licence_http://creativecommons.org/publicdomain/zero
識別號： ISSN: 0004-637X
識別號： EISSN: 1538-4357
識別號： DOI: 10.3847/0004-637X/826/1/39 |
| 顯示於類別: | [天文研究所] 期刊論文
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