dc.creator | Nicholl, M. | |
dc.creator | Berger, E. | |
dc.creator | Smartt, S. J. | |
dc.creator | Margutti, R. | |
dc.creator | Kamble, A. | |
dc.creator | Alexander, K. D. | |
dc.creator | Chen, T. W. | |
dc.creator | Inserra, C. | |
dc.creator | Arcavi, I. | |
dc.creator | Blanchard, P. K. | |
dc.creator | Cartier Ugarte, Regis | |
dc.creator | Chambers, K. C. | |
dc.creator | Childress, M. J. | |
dc.creator | Chornock, R. | |
dc.creator | Cowperthwaite, P. S. | |
dc.creator | Drout, M. | |
dc.creator | Flewelling, H. A. | |
dc.creator | Fraser, M. | |
dc.creator | Gal Yam, Avishay | |
dc.creator | Galbany, Lluis | |
dc.creator | Harmanen, J. | |
dc.creator | Holohien, T- W. -S | |
dc.creator | Hosseinzadeh, G. | |
dc.creator | Howell, D. A. | |
dc.creator | Huber, M. E. | |
dc.creator | Jerkstrand, A. | |
dc.creator | Kankare, E. | |
dc.creator | Kochanek, C. S. C. S. | |
dc.creator | Lin, Z. -Y. | |
dc.creator | Lunnan, R. | |
dc.creator | Magnier, E. A. | |
dc.creator | Maguire, K. | |
dc.creator | McCully, C. | |
dc.creator | McDonald, M. | |
dc.creator | Metzger, B. D. | |
dc.creator | Milisavljevic, D. | |
dc.creator | Mitra, A. | |
dc.creator | Reynolds, T. | |
dc.creator | Saario, J. | |
dc.creator | Shappee, B. J. | |
dc.creator | Smith, K. W. | |
dc.creator | Valenti, S. | |
dc.creator | Villar, V. A. | |
dc.creator | Waters, C. | |
dc.creator | Young, D. R. | |
dc.date.accessioned | 2016-12-27T20:16:38Z | |
dc.date.accessioned | 2019-04-26T01:06:15Z | |
dc.date.available | 2016-12-27T20:16:38Z | |
dc.date.available | 2019-04-26T01:06:15Z | |
dc.date.created | 2016-12-27T20:16:38Z | |
dc.date.issued | 2016 | |
dc.identifier | The Astrophysical Journal, 826:39 (31pp), 2016 July 20 | |
dc.identifier | 10.3847/0004-637X/826/1/39 | |
dc.identifier | http://repositorio.uchile.cl/handle/2250/142147 | |
dc.identifier.uri | http://repositorioslatinoamericanos.uchile.cl/handle/2250/2446234 | |
dc.description.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 (M-U approximate to -23.1) and in a fainter galaxy (M-B approximate to -16.0) than other SLSNe at z similar to 0.1. 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 greater than or similar to 10 M-circle dot stripped progenitor exploding with similar to 10(51) erg kinetic energy, forming a magnetar with a spin-down timescale of similar to 20 days (thus avoiding a gamma-ray burst) that reheats the ejecta and drives ionization fronts. The most likely alternative scenario-interaction with similar to 20 M-circle dot of dense, inhomogeneous circumstellar material-can be tested with continuing radio follow-up. | |
dc.language | en | |
dc.publisher | IOP Publishing | |
dc.rights | http://creativecommons.org/licenses/by-nc-nd/3.0/cl/ | |
dc.rights | Attribution-NonCommercial-NoDerivs 3.0 Chile | |
dc.source | The Astrophysical Journal | |
dc.subject | Supernovae: general | |
dc.subject | Supernovae: individual (SN 2015bn) | |
dc.title | SN 2015bn: a detailed multi-wavelength view of a nearbysuperluminous supernova | |
dc.type | Artículos de revistas | |