Examinando por Autor "Prentice, Simon"

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    A very luminous magnetar-powered supernova associated with an ultra-long γ-ray burst
    (Nature Publishing Group, 2015-07) Greiner, Jochen; Mazzali, Paolo A.; Kann, D. Alexander; Krühler, Thomas; Pian, Elena; Prentice, Simon; Olivares, E.; Rossi, Andrea; Klose, Sylvio; Taubenberger, Stefan; Knust, Fabian; Afonso, Paulo; Ashall, Chris; Bolmer, Jan; Delvaux, Corentin; Diehl, Roland; Elliott, Jonathan; Filgas, Robert; Fynbo, Johan P.U.; Graham, John F.; Guelbenzu, Ana Nicuesa; Kobayashi, Shiho; Leloudas, Giorgos; Savaglio, Sandra; Schady, Patricia; Schmidl, Sebastian; Schweyer, Tassilo; Sudilovsky, Vladimir; Tanga, Mohit; Updike, Adria C.; Van Eerten, Hendrik; Varela, Karla
    A new class of ultra-long-duration (more than 10,000 seconds) γ-ray bursts has recently been suggested. They may originate in the explosion of stars with much larger radii than those producing normal long-duration γ-ray bursts or in the tidal disruption of a star. No clear supernova has yet been associated with an ultra-long-duration γ-ray burst. Here we report that a supernova (SN 2011kl) was associated with the ultra-long-duration γ-ray burst GRB 111209A, at a redshift z of 0.677. This supernova is more than three times more luminous than type Ic supernovae associated with long-duration γ-ray bursts, and its spectrum is distinctly different. The slope of the continuum resembles those of super-luminous supernovae, but extends further down into the rest-frame ultraviolet implying a low metal content. The light curve evolves much more rapidly than those of super-luminous supernovae. This combination of high luminosity and low metal-line opacity cannot be reconciled with typical type Ic supernovae, but can be reproduced by a model where extra energy is injected by a strongly magnetized neutron star (a magnetar), which has also been proposed as the explanation for super-luminous supernovae. © 2015 Macmillan Publishers Limited. All rights reserved.
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    Monthly Notices of the Royal Astronomical Society
    (Oxford University Press, 2020-02) Clark, Peter; Maguire, Kate; Inserra, Cosimo; Prentice, Simon; Stephen, J. Smartt; Contreras, Carlos; Hossenizadeh, Griffin; Hsiao, Eric Y.; Kankare, Erkki; Kasliwal, Mansi; Nugent, Peter; Shahbandeh, Melissa; Baltay, Charles; Rabinowitz, David; Arcavi, Iair; Ashall, Chris; Burns, Christopher R.; Callis, Emma; Chen, Ting-Wan; Diamond, Tiara; Fraser, Morgan; Howell, D. Andrew; Karamehmetoglu, Emir; Kotak, Rubina; Lyman, Joseph; Morrell, Nidia; Phillips, Mark; Pignata, Giuliano; Pursiainen, Miika; Sollerman, Jesper; Stritzinger, Maximilian; Sullivan, Mark; Young, David
    This paper describes the rapidly evolving and unusual supernova LSQ13ddu, discovered by the La Silla-QUEST survey. LSQ13ddu displayed a rapid rise of just 4.8 ± 0.9 d to reach a peak brightness of −19.70 ± 0.02 mag in the LSQgr band. Early spectra of LSQ13ddu showed the presence of weak and narrow He I features arising from interaction with circumstellar material (CSM). These interaction signatures weakened quickly, with broad features consistent with those seen in stripped-envelope SNe becoming dominant around two weeks after maximum. The narrow He I velocities are consistent with the wind velocities of luminous blue variables but its spectra lack the typically seen hydrogen features. The fast and bright early light curve is inconsistent with radioactive 56Ni powering but can be explained through a combination of CSM interaction and an underlying 56Ni decay component that dominates the later time behaviour of LSQ13ddu. Based on the strength of the underlying broad features, LSQ13ddu appears deficient in He compared to standard SNe Ib. © 2019 The Author(s)