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|Title:||SN 2011fu: a type IIb supernova with a luminous double-peaked light curve||Authors:||Morales-Garoffolo, A.
ELIAS DE LA ROSA, NANCY DEL CARMEN
Domínguez, R. M.
Howell, D. A.
Smartt, S. J.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||454||Issue:||1||First Page:||95||Abstract:||We present optical and near-infrared observations of the type IIb supernova (SN) 2011fu from a few days to ~300 d after explosion. The SN presents a double-peaked light curve (LC) similar to that of SN 1993J, although more luminous and with a longer cooling phase after the primary peak. The spectral evolution is also similar to SN 1993J's, with hydrogen dominating the spectra to ~40 d, then helium gaining strength, and nebular emission lines appearing from ~60 d post-explosion. The velocities derived from the P-Cygni absorptions are overall similar to those of other type IIb SNe. We have found a strong similarity between the oxygen and magnesium line profiles at late times, which suggests that these lines are forming at the same location within the ejecta. The hydrodynamical modelling of the pseudo-bolometric LC and the observed photospheric velocities suggest that SN 2011fu was the explosion of an extended star (R~ 450 R<SUB>☉</SUB>), in which 1.3 × 10<SUP>51</SUP> erg of kinetic energy were released and 0.15 M<SUB>☉</SUB> of <SUP>56</SUP>Ni were synthesized. In addition, a better reproduction of the observed early pseudo-bolometric LC is achieved if a more massive H-rich envelope than for other type IIb SNe is considered (0.3 M<SUB>☉</SUB>). The hydrodynamical modelling of the LC and the comparison of our late-time spectra with nebular spectral models for type IIb SNe, point to a progenitor for SN 2011fu with a Zero Age Main Sequence (ZAMS) mass of 13-18 M<SUB>☉</SUB>.||Acknowledgments:||AMG acknowledges financial support by the Spanish Ministerio de Economía y Competitividad (MINECO) grant ESP2013-41268-R. NER acknowledges the support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251 ‘Astronomy Fellowships in Italy’ (AstroFIt). ST acknowledges support by TRR33 ‘The Dark Universe’ of the German Research Foundation (DFG). AP, SB, NER, and LT are partially supported by the PRIN-INAF 2014 within the project ‘Transient Universe: unveiling new types of stellar explosions with PESSTO.’ This work was partly supported by the European Union FP7 programme through ERC grant number 320360. SJS acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no.  and STFC grants ST/I001123/1 and ST/L000709/1. Data of this work have been taken in the framework of the European supernova collaboration involved in the ESO-NTT large programme 184.D-1140 led by Stefano Benetti. This work is partially based on observations made with the Liverpool Telescope which is operated by Liverpool John Moores University with financial support from the UK Science and Technology Facilities Council, the Nordic Optical Telescope operated by the Nordic Optical Telescope Scientific Association, the Gran Telescopio de Canarias , and the William Hershel Telescope (operated by the Isaac Newton Group) in the Spanish Observatorio del Roque de los Muchachos (ORM) of the Instituto de Astrofísica de Canarias ; the 2.2 m telescope of the Centro Astronómico Hispano Alemán (Calar Alto, Spain); the 1.82 m Copernico Telescope operated by INAF- Osservatorio Astronomico di Padova and the 1.22 m Galileo Telescope of Dipartimento di Fisica e Astonomia (Universitá di Padova) at the Asiago Observatory (Italy); the Telescopio Carlos Sánchez operated by the Instituto de Astrofísica de Canarias in the Spanish Observatorio del Teide ; the Faulkes Telescope North situated on Mt. Haleakala (Hawaii, U.S.A.); and the 0.4 m telescope at the Observatorio Astronómico de Cantabria (Spain). We would like to thank F. Ciabattari and E. Mazzoni from the ISSP for providing us the discovery and confirmation image of the SN taken at the Osservatorio di Monte Agliale (Lucca, Italy). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.||URI:||http://hdl.handle.net/20.500.12386/24137||URL:||https://academic.oup.com/mnras/article/454/1/95/1132801||ISSN:||0035-8711||DOI:||10.1093/mnras/stv1972||Bibcode ADS:||2015MNRAS.454...95M||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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