Journal
ASTROPHYSICAL JOURNAL
Volume 819, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/0004-637X/819/1/35
Keywords
supernovae: individual (PTF10iam, SNLS04D4ec, SNLS05D2bk, SNLS06D1hc, Dougie)
Categories
Funding
- ESO program [176. A-0589]
- National Science Foundation [1313484, PHY 11-25915, AST 11-09174]
- Israeli Science Foundation
- EU/FP7/ERC grant
- BSF
- GIF
- Minerva
- Quantum universe I-Core program of the planning and budgeting committee
- ISF
- Kimmel Investigator award
- Danish National Research Foundation
- W. M. Keck Foundation
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- Science and Technology Facilities Council [ST/M000966/1] Funding Source: researchfish
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1109174, 1313484] Funding Source: National Science Foundation
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We present observations of four rapidly rising (t(rise) approximate to 10 days) transients with peak luminosities between those of supernovae (SNe) and superluminous SNe (M-peak approximate to-20)-one discovered and followed by the Palomar Transient Factory (PTF) and three by the Supernova Legacy Survey. The light curves resemble those of SN 2011kl, recently shown to be associated with an ultra-long-duration gamma-ray burst (GRB), though no GRB was seen to accompany our SNe. The rapid rise to a luminous peak places these events in a unique part of SN phase space, challenging standard SN emission mechanisms. Spectra of the PTF event formally classify it as an SN II due to broad Ha emission, but an unusual absorption feature, which can be interpreted as either high velocity Ha (though deeper than in previously known cases) or Si II (as seen in SNe Ia), is also observed. We find that existing models of white dwarf detonations, CSM interaction, shock breakout in a wind (or steeper CSM), and magnetar spin down cannot readily explain the observations. We consider the possibility that a Type 1.5 SN scenario could be the origin of our events. More detailed models for these kinds of transients and more constraining observations of future such events should help to better determine their nature.
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