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Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory
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Number of Authors: 272018 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 860, no 2, article id 100Article in journal (Refereed) Published
Abstract [en]

We investigate the light-curve properties of a sample of 26 spectroscopically confirmed hydrogen- poor superluminous supernovae (SLSNe-I) in the Palomar Transient Factory survey. These events are brighter than SNe Ib/c and SNe Ic-BL, on average, by about 4 and 2. mag, respectively. The peak absolute magnitudes of SLSNe-I in rest-frame g band span -22 less than or similar to M-g less than or similar to -20 mag, and these peaks are not powered by radioactive Ni-56, unless strong asymmetries are at play. The rise timescales are longer for SLSNe than for normal SNe Ib/c, by roughly 10 days, for events with similar decay times. Thus, SLSNe-I can be considered as a separate population based on photometric properties. After peak, SLSNe-I decay with a wide range of slopes, with no obvious gap between rapidly declining and slowly declining events. The latter events show more irregularities (bumps) in the light curves at all times. At late times, the SLSN-I light curves slow down and cluster around the 56Co radioactive decay rate. Powering the late-time light curves with radioactive decay would require between 1 and 10M(circle dot) of Ni masses. Alternatively, a simple magnetar model can reasonably fit the majority of SLSNe-I light curves, with four exceptions, and can mimic the radioactive decay of 56Co, up to similar to 400 days from explosion. The resulting spin values do not correlate with the host-galaxy metallicities. Finally, the analysis of our sample cannot strengthen the case for using SLSNe-I for cosmology.

Place, publisher, year, edition, pages
2018. Vol. 860, no 2, article id 100
Keywords [en]
supernovae: general
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-158251DOI: 10.3847/1538-4357/aab9b6ISI: 000435374600014OAI: oai:DiVA.org:su-158251DiVA, id: diva2:1238219
Available from: 2018-08-13 Created: 2018-08-13 Last updated: 2018-08-13Bibliographically approved

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De Cia, AnnalisaSollerman, JesperPrentice, S.Taddia, Francesco
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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