Journal
ASTROPHYSICAL JOURNAL
Volume 860, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/aab9b6
Keywords
supernovae: general
Categories
Funding
- Weizmann Institute of Science Koshland Center for Basic Research
- NASA through the Einstein Fellowship Program [PF6-170148]
- EU/FP7-ERC grant [615929]
- STFC through an Ernest Rutherford Fellowship
- Israel Science Foundation, Minerva, Israeli ministry of Science
- US-Israel Binational Science Foundation
- I-CORE Program of the Planning and Budgeting Committee
- Israel Science Foundation
- NSF CAREER [1455090]
- GROWTH project by the National Science Foundation [1545949]
- US Department of Energy as a part of the Laboratory Directed Research and Development program
- Discovery Communications. Large Monolithic Imager (LMI) on DCT from the National Science Foundation [AST-1005313]
- W.M. Keck Foundation
- STFC [ST/F007159/1, ST/P002218/1, ST/M000095/1, ST/P006892/1, ST/R000484/1, ST/L00061X/1, ST/M003035/1] Funding Source: UKRI
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1455090] Funding Source: National Science Foundation
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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.
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