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Light curves of hydrogen-poor superluminous supernovae from the palomar transient factory

Light curves of hydrogen-poor superluminous supernovae from the palomar transient factory
Light curves of hydrogen-poor superluminous supernovae from the palomar transient factory

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 ≲ Mg ≲ -20 mag, and these peaks are not powered by radioactive 56Ni, 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 10 M o 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 ∼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.

machine-readable tables, material: figure sets
0004-637X
De Cia, Annalisa
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Gal-Yam, A.
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Rubin, A.
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Leloudas, G.
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Vreeswijk, P.
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Perley, D. A.
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Quimby, R.
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Yan, Lin
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Sullivan, M.
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Flörs, A.
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Sollerman, J.
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Bersier, D.
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Cenko, S. B.
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Gal-Yam, M.
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Maguire, K.
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Ofek, E. O.
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Prentice, S.
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Schulze, S.
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Spyromilio, J.
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Valenti, S.
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Arcavi, I.
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Corsi, A.
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Howell, D. A.
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Mazzali, P.
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Kasliwal, M. M.
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Taddia, F.
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Yaron, O.
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De Cia, Annalisa
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Gal-Yam, A.
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Rubin, A.
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Leloudas, G.
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Vreeswijk, P.
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Perley, D. A.
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Quimby, R.
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Yan, Lin
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Sullivan, M.
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Flörs, A.
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Sollerman, J.
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Bersier, D.
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Cenko, S. B.
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Gal-Yam, M.
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Maguire, K.
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Ofek, E. O.
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Prentice, S.
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Schulze, S.
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Spyromilio, J.
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Valenti, S.
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Arcavi, I.
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Corsi, A.
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Howell, D. A.
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Mazzali, P.
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Kasliwal, M. M.
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Taddia, F.
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Yaron, O.
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De Cia, Annalisa, Gal-Yam, A., Rubin, A., Leloudas, G., Vreeswijk, P., Perley, D. A., Quimby, R., Yan, Lin, Sullivan, M., Flörs, A., Sollerman, J., Bersier, D., Cenko, S. B., Gal-Yam, M., Maguire, K., Ofek, E. O., Prentice, S., Schulze, S., Spyromilio, J., Valenti, S., Arcavi, I., Corsi, A., Howell, D. A., Mazzali, P., Kasliwal, M. M., Taddia, F. and Yaron, O. (2018) Light curves of hydrogen-poor superluminous supernovae from the palomar transient factory. The Astrophysical Journal, 860 (2). (doi:10.3847/1538-4357/aab9b6).

Record type: Article

Abstract

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 ≲ Mg ≲ -20 mag, and these peaks are not powered by radioactive 56Ni, 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 10 M o 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 ∼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.

Text
LIGHT CURVES OF HYDROGEN-POOR SUPERLUMINOUS SUPERNOVAE - Accepted Manuscript
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Accepted/In Press date: 23 March 2018
e-pub ahead of print date: 20 June 2018
Keywords: machine-readable tables, material: figure sets

Identifiers

Local EPrints ID: 422624
URI: https://eprints.soton.ac.uk/id/eprint/422624
ISSN: 0004-637X
PURE UUID: f1486680-051e-4ae0-bc3f-21b6ba27d236
ORCID for M. Sullivan: ORCID iD orcid.org/0000-0001-9053-4820

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Date deposited: 26 Jul 2018 16:30
Last modified: 20 Jul 2019 00:40

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Contributors

Author: Annalisa De Cia
Author: A. Gal-Yam
Author: A. Rubin
Author: G. Leloudas
Author: P. Vreeswijk
Author: D. A. Perley
Author: R. Quimby
Author: Lin Yan
Author: M. Sullivan ORCID iD
Author: A. Flörs
Author: J. Sollerman
Author: D. Bersier
Author: S. B. Cenko
Author: M. Gal-Yam
Author: K. Maguire
Author: E. O. Ofek
Author: S. Prentice
Author: S. Schulze
Author: J. Spyromilio
Author: S. Valenti
Author: I. Arcavi
Author: A. Corsi
Author: D. A. Howell
Author: P. Mazzali
Author: M. M. Kasliwal
Author: F. Taddia
Author: O. Yaron

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