DES13S2cmm: the first superluminous supernova from the Dark Energy Survey

Papadopoulos, A.; D’Andrea, C. B.; Sullivan, M.; Nichol, R. C.; Barbary, Kyle; Biswas, Rahul; Brown, P. J.; Covarrubias, R.; Finley, D. A.; Fischer, J. A.; Foley, R. J.; Goldstein, Daniel A.; Gupta, R.; Keßler, R.; Kovacs, E.; Kuhlmann, S.; Lidman, C.; March, M.; Nugent, P.; Šako, M.; Smith, R. C.; Spinka, H.; Wester, W. C.; Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Banerji, M.; Bernstein, Joseph P.; Bernstein, R. A.; Carnero, A.; Costa, L. N. da; DePoy, D. L.; Desai, S.; Diehl, H. T.; Eifler, T. F.; Evrard, A. E.; Flaugher, B.; Frieman, J.; Gerdes, D. W.; Gruen, David; Honscheid, K.; James, D. J.; Kuêhn, K.; Kuropatkin, N.; Lahav, O.; Maia, M. A. G.; Makler, M.; Marshall, J. L.; Merritt, K. W.; Miller, C. J.; Miquel, R.; Ogando, R. L. C.; Plazas, A. A.; Roe, Natalie A.; Romer, A. K.; Rykoff, E. S.; Sánchez, E.; Santiago, B.; Scarpine, V.; Schubnell, M.; Sevilla-Noarbe, I.; Soares-Santos, M.; Suchyta, E.; Swanson, M. E. C.; Tarlè, G.; Thaler, J. J.; Tucker, L. D.; Wechsler, Risa H.; Zuntz, J.

doi:10.1093/mnras/stv174

Cited by 58 publications

(40 citation statements)

References 62 publications

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“…Recently, however, new classes of SNe have emerged that only partially fit into this classical scheme. In particular, a number of very luminous events have been detected by different surveys, many at redshifts exceeding 0.5 (e.g., Quimby et al 2007;Barbary et al 2009;Quimby et al 2011;Chomiuk et al 2011;Leloudas et al 2012;Lunnan 2013;Howell et al 2013;Papadopoulos et al 2015, see Gal-Yam (2012 for a review). Although they are collectively ⋆ E-mail: P.Mazzali@ljmu.ac.uk classified as superluminous supernovae (SLSNe), their observational properties are quite diverse.…”

Section: Introductionmentioning

confidence: 99%

“…These SNe typically show strong absorption lines of lighter elements, including oxygen, and have never been observed in the nebular phase as they are typically too distant to be observed at late times. Their light curves do not appear to be consistent with being powered by 56 Ni decay (Inserra et al 2013;Howell et al 2013;Papadopoulos et al 2015). One alternative to 56 Ni is that the SN is powered by energy emitted by a magnetized, rapidly spinning neutron star (a Magnetar), (e.g., Bucciantini et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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Spectrum formation in superluminous supernovae (Type I)

Mazzali

Sullivan

Pian

et al. 2016

Mon. Not. R. Astron. Soc.

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140

246

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The near-maximum spectra of most superluminous supernovae that are not dominated by interaction with a H-rich CSM (SLSN-I) are characterised by a blue spectral peak and a series of absorption lines which have been identified as O II. SN 2011kl, associated with the ultra-long gamma-ray burst GRB111209A, also had a blue peak but a featureless optical/UV spectrum. Radiation transport methods are used to show that the spectra (not including SN 2007bi, which has a redder spectrum at peak, like ordinary SNe Ic) can be explained by a rather steep density distribution of the ejecta, whose composition appears to be typical of carbon-oxygen cores of massive stars which can have low metal content. If the photospheric velocity is ∼ 10000 − 15000 km s −1 several lines form in the UV. O II lines, however, arise from very highly excited lower levels, which require significant departures from Local Thermodynamic Equilibrium to be populated. These SLSNe are not thought to be powered primarily by 56 Ni decay. An appealing scenario is that they are energised by X-rays from the shock driven by a magnetar wind into the SN ejecta. The apparent lack of evolution of line velocity with time that characterises SLSNe up to about maximum is another argument in favour of the magnetar scenario. The smooth UV continuum of SN 2011kl requires higher ejecta velocities (∼ 20000 km s −1 ): line blanketing leads to an almost featureless spectrum. Helium is observed in some SLSNe after maximum. The high ionization near maximum implies that both He and H may be present but not observed at early times. The spectroscopic classification of SLSNe should probably reflect that of SNe Ib/c. Extensive time coverage is required for an accurate classification.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Spectrum formation in superluminous supernovae (Type I)

Mazzali

Sullivan

Pian

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

140

246

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show abstract

“…Studies of literature samples of SLSNe have suggested that the scatter in SLSN-I luminosities is intrinsically low and can be further improved by considering correlations with colors and decline rates (Inserra & Smartt 2014;Papadopoulos et al 2015), leading to increased interest in the potential use of SLSNe as standardizable candles (Wei et al 2015;Scovacricchi et al 2016). Beyond potential cosmology applications, high-redshift SLSNe also offer a probe for studying highredshift galaxies (Berger et al 2012;Vreeswijk et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Hydrogen-poor Superluminous Supernovae from the Pan-STARRS1 Medium Deep Survey

Lunnan

Chornock

Berger

et al. 2018

ApJ

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103

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present light curves and classification spectra of 17 hydrogen-poor superluminous supernovae (SLSNe) from the Pan-STARRS1 Medium Deep Survey (PS1 MDS). Our sample contains all objects from the PS1MDS sample with spectroscopic classification that are similar to either of the prototypes SN 2005ap or SN 2007bi, without an explicit limit on luminosity. With a redshift range z 0.3 1.6 < < , PS1MDS is the first SLSN sample primarily probing the high-redshift population; our multifilter PS1 light curves probe the rest-frame UV emission, and hence the peak of the spectral energy distribution. We measure the temperature evolution and construct bolometric light curves, and find peak luminosities of 0.5 5 10 44 ( -) ergs −1 and lower limits on the total radiated energies of 0.3 2 10 51 ( -) erg. The light curve shapes are diverse, with both rise and decline times spanning a factor of ∼5 and several examples of double-peaked light curves. When correcting for the flux-limited nature of our survey, we find a median peak luminosity at 4000Å of M 21.1 mag 4000 = -and a spread of 0.7 mag s = .

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“…One interesting feature of slowly-declining Type Ic SLSNe is that their LC decline rates are often consistent with the 56 Co decay rate for a long time (e.g., Nicholl et al 2016a;Chen et al 2015;Papadopoulos et al 2015;Yan et al 2015;Lunnan et al 2016;Vreeswijk et al 2016). If we just examine the late-phase LCs, the simplest way to explain them is the 56 Co decay.…”

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confidence: 97%

Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae

Moriya

Chen

Langer

2017

ApJ

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Many Type Ic superluminous supernovae have light-curve decline rates after their luminosity peak which are close to the nuclear decay rate of 56 Co, consistent with the interpretation that they are powered by 56 Ni and possibly pair-instability supernovae. However, their rise times are typically shorter than those expected from pair-instability supernovae, and Type Ic superluminous supernovae are often suggested to be powered by magnetar spin-down. If magnetar spin-down is actually a major mechanism to power Type Ic superluminous supernovae, it should be able to produce decline rates similar to the 56 Co decay rate rather easily. In this study, we investigate the conditions for magnetars under which their spin-down energy input can behave like the 56 Ni nuclear decay energy input. We find that an initial magnetic field strength within a certain range is sufficient to keep the magnetar energy deposition within a factor of a few of the 56 Co decay energy for several hundreds of days. Magnetar spin-down needs to be by almost pure dipole radiation with the braking index close to 3 to mimic 56 Ni in a wide parameter range. Not only late-phase 56 Co-decay-like light curves, but also rise time and peak luminosity of most 56 Ni-powered light curves can be reproduced by magnetars. Bolometric light curves for more than 700 days are required to distinguish the two energy sources solely by them. We expect that more slowly-declining superluminous supernovae with short rise times should be found if they are mainly powered by magnetar spin-down.

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DES13S2cmm: the first superluminous supernova from the Dark Energy Survey

Cited by 58 publications

References 62 publications

Spectrum formation in superluminous supernovae (Type I)

Spectrum formation in superluminous supernovae (Type I)

Hydrogen-poor Superluminous Supernovae from the Pan-STARRS1 Medium Deep Survey

Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae

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DES13S2cmm: the first superluminous supernova from the Dark Energy Survey

Cited by 58 publications

References 62 publications

Spectrum formation in superluminous supernovae (Type I)

Spectrum formation in superluminous supernovae (Type I)

Hydrogen-poor Superluminous Supernovae from the Pan-STARRS1 Medium Deep Survey

Properties of Magnetars Mimicking 56Ni-Powered Light Curves in Type IC Superluminous Supernovae

Contact Info

Product

Resources

About

Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae