> Details

Ofek, E. O.; Cenko, S. B.; Shaviv, N. J.; Duggan, G.; Strotjohann, N.-L.; Rubin, A.; Kulkarni, S. R.; Gal-Yam, A.; Sullivan, M.; Cao, Y.; Nugent, P. E.; Kasliwal, M. M.; Sollerman, J.; Fransson, C.; Filippenko, A. V.; Perley, D. A.; Yaron, O.; Laher, R.

PTF13efv—AN OUTBURST 500 DAYS PRIOR TO THE SNHUNT 275 EXPLOSION AND ITS RADIATIVE EFFICIENCY

Reference
management

Bookmarks

Remove from
bookmarks

Share this on Whatsapp

Close

Bookmarks



You can manage bookmarks using lists, please log in to your user account for this.
  • Media type: E-Article
  • Title: PTF13efv—AN OUTBURST 500 DAYS PRIOR TO THE SNHUNT 275 EXPLOSION AND ITS RADIATIVE EFFICIENCY
  • Contributor: Ofek, E. O.; Cenko, S. B.; Shaviv, N. J.; Duggan, G.; Strotjohann, N.-L.; Rubin, A.; Kulkarni, S. R.; Gal-Yam, A.; Sullivan, M.; Cao, Y.; Nugent, P. E.; Kasliwal, M. M.; Sollerman, J.; Fransson, C.; Filippenko, A. V.; Perley, D. A.; Yaron, O.; Laher, R.
  • imprint: American Astronomical Society, 2016
  • Published in: The Astrophysical Journal
  • Language: Not determined
  • DOI: 10.3847/0004-637x/824/1/6
  • ISSN: 0004-637X; 1538-4357
  • Origination:
  • Footnote:
  • Description: <jats:title>ABSTRACT</jats:title> <jats:p>The progenitors of some supernovae (SNe) exhibit outbursts with super-Eddington luminosities prior to their final explosions. This behavior is common among SNe IIn, but the driving mechanisms of these precursors are not yet well-understood. SNHunt 275 was announced as a possible new SN during 2015 May. Here we report on pre-explosion observations of the location of this event by the Palomar Transient Factory (PTF) and report the detection of a precursor about 500 days prior to the 2015 May activity (PTF 13efv). The observed velocities in the 2015 transient and its 2013 precursor absorption spectra are low (1000–2000 km s<jats:sup>−1</jats:sup>), so it is not clear yet if the recent activity indeed marks the final disruption of the progenitor. Regardless of the nature of this event, we use the PTF photometric and spectral observations, as well as <jats:italic>Swift</jats:italic>-UVOT observations, to constrain the efficiency of the radiated energy relative to the total kinetic energy of the precursor. We find that, using an order-of-magnitude estimate and under the assumption of spherical symmetry, the ratio of the radiated energy to the kinetic energy is in the range of 4 × 10<jats:sup>−2</jats:sup> to 3.4 × 10<jats:sup>3</jats:sup>.</jats:p>
  • Access State: Open Access