Long-duration superluminous supernovae at late times

Jerkstrand, A.; Smartt, S. J.; Inserra, C.; Nicholl, M.; Chen, T.-W.; Krühler, T.; Sollerman, J.; Taubenberger, S.; Gal-Yam, A.; Kankare, E.; Maguire, Kate; Fraser, M.; Valenti, S.; Sullivan, M.; Cartier, R.; Young, D. R.

doi:10.48550/arxiv.1608.02994

Cited by 6 publications

(12 citation statements)

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“…This has already been pointed out by, e.g., Metzger et al (2015). Very recently, spectroscopic observations of two SLSNe-I, LSQ14an and SN 2015bn in their nebular phases by Jerkstrand et al (2016) and Nicholl et al (2016a) revealed optical spectra reminiscent of those of broad-lined Ic SNe, such as SN 1998bw, further supporting the link between SLSNe-I and GRBs.…”

Section: Possible Link Between Slsne-i and Grbsmentioning

confidence: 52%

Supernova ejecta with a relativistic wind from a central compact object: a unified picture for extraordinary supernovae

Suzuki

Maeda

2016

Mon. Not. R. Astron. Soc.

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The hydrodynamical interaction between freely expanding supernova ejecta and a relativistic wind injected from the central region is studied in analytic and numerical ways. As a result of the collision between the ejecta and the wind, a geometrically thin shell surrounding a hot bubble forms and expands in the ejecta. We use a self-similar solution to describe the early dynamical evolution of the shell and carry out a two-dimensional special relativistic hydrodynamic simulation to follow further evolution. The Rayleigh-Taylor instability inevitably develops at the contact surface separating the shocked wind and ejecta, leading to the complete destruction of the shell and the leakage of hot gas from the hot bubble. The leaking hot materials immediately catch up with the outermost layer of the supernova ejecta and thus different layers of the ejecta are mixed. We present the spatial profiles of hydrodynamical variables and the kinetic energy distributions of the ejecta. We stop the energy injection when a total energy of 10 52 erg, which is 10 times larger than the initial kinetic energy of the supernova ejecta, is deposited into the ejecta and follow the subsequent evolution. From the results of our simulations, we consider expected emission from supernova ejecta powered by the energy injection at the centre and discuss the possibility that superluminous supernovae and broad-lined Ic supernovae could be produced by similar mechanisms.

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Section: Possible Link Between Slsne-i and Grbsmentioning

confidence: 52%

Supernova ejecta with a relativistic wind from a central compact object: a unified picture for extraordinary supernovae

Suzuki

Maeda

2016

Mon. Not. R. Astron. Soc.

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“…At the same phase, the Fe II λ5169 features in SLSNe Ic and SNe Ic-bl are systematically and quantifiably broader than those in SNe Ic. Moreover, similarities between SLSNe Ic and SNe Ic-bl have been observed in host galaxy properties (Lunnan et al 2014;Angus et al 2016) and nebular phase velocities (Jerkstrand et al 2016). Thus, although the continuum of the SLSN Ic spectra is much bluer than that of the SN Ic-bl spectra, the many spectral and environmental similarities between SLSNe Ic and SNe Ic-bl, including those connected with GRBs, indicate that the two subtypes may have similar explosion engines and progenitors, which could be partly explained by a multidimensional magnetar model with different energy injection rates (Metzger et al 2015;Suzuki & Maeda 2016).…”

Section: Conclusion and Next Stepsmentioning

confidence: 80%

“…which at that phase has an average value of 15,000 (+/− 2,600) km s −1 , we note that this implies that the absorption velocity of SLSNe Ic at the date of maximum light, which is usually the one used for ejecta mass estimates, will have to be even higher. Moreover, Jerkstrand et al (2016) found that SLSNe Ic and SNe Ic-bl have similar nebular-phase spectra in terms of velocities. These similarities in observations indicate that SLSNe Ic and SNe Ic-bl may have similar explosion engines, which is consistent with a multi-dimensional magnetar model in Suzuki & Maeda (2016), where they claimed that SLSNe Ic and SNe Ic-bl could be produced by a similar engine with different energy injection rates.…”

Section: Slsne Ic and Sne Ic-bl Have Comparable Fe IImentioning

confidence: 86%

Analyzing the Largest Spectroscopic Data Set of Hydrogen-poor Super-luminous Supernovae

Liu

Modjaz

Bianco

2017

ApJ

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Super-luminous supernovae (SLSNe) are tremendously luminous explosions whose power sources and progenitors are highly debated. Broad-lined SNe Ic (SNe Ic-bl) are the only type of SNe that are connected with long-duration gamma ray bursts (GRBs). Studying the spectral similarity and difference between the populations of hydrogen-poor SLSNe (SLSNe Ic) and of hydrogen-poor stripped-envelope core-collapse SNe, in particular SNe Ic and SNe Ic-bl, can provide crucial observations to test predictions of theories based on various power source models and progenitor models. In this paper, we collected all of the published optical spectra of 32 SLSNe Ic, 21 SNe Ic-bl, as well as 17 SNe Ic, quantified their spectral features, constructed average spectra, and compared them in a systematic way using new tools we have developed. We find that SLSNe Ic and SNe Ic-bl, including those connected with GRBs, have comparable widths for their spectral features and average absorption velocities at all phases. Thus, our findings strengthen the connection between SLSNe Ic and GRBs. In particular, SLSNe Ic have average Fe II λ5169 absorption velocities of −15, 000 + / − 2, 600 km s −1 at 10 days after peak, which are higher than those of SNe Ic by ∼ 7, 000 km s −1 on average. SLSNe Ic also have significantly broader Fe II λ5169 lines than SNe Ic. Moreover, we find that such high absorption and width velocities of SLSNe Ic may be hard to explain by the interaction model, and none of 13 SLSNe Ic with measured absorption velocities spanning over 10 days has a convincing flat velocity-evolution, which is inconsistent with the magnetar model in one dimension. Lastly, we compare SN 2011kl, the first SN connected with an ultra-long GRB, with the mean spectrum of SLSNe Ic and of SNe Ic-bl.

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“…A defining prediction of magnetar-powered models is the formation of a constant-density shell due to the central overpressure from the magnetised wind (Kasen & Bildsten 2010;Woosley 2010;Metzger et al 2014). This shell could perhaps also help to account for the relative strength (and width) of the O I λ7774 recombination line in SLSNe/hypernovae, if its electron density is 10 8 cm −3 at this phase (Mazzali et al 2004;Nicholl et al 2013;Jerkstrand et al 2016b). Normal SNe Ic without an engine-or GRB-SNe, where the engine punches right through the stellar envelope rather than forming a shelldo not exhibit a strong line here.…”

Section: Discussionmentioning

confidence: 99%

“…Mazzali et al (2001) found good agreement between oxygen masses derived with equation 1 and from synthetic spectra, and that oxygen constituted 60-70% of the ejected mass, giving us a total mass M ej ≈ 14 M . This should be treated with caution due to uncertain physical conditions and an exponential temperature dependence: taking the plausible range 4000-6000 K based on nebular models of hypernovae (Mazzali et al 2001), the allowed range is Jerkstrand et al (2016b) have calculated detailed spectroscopic models for SN 2015bn at +300 d and find that a similar ejecta mass is required. Interestingly, Mazzali et al (2016) derived similar masses for other SLSNe using spectroscopic models of the photospheric phase; thus a consistent picture is emerging.…”

Section: Discussionmentioning

confidence: 99%

SUPERLUMINOUS SUPERNOVA SN 2015bn IN THE NEBULAR PHASE: EVIDENCE FOR THE ENGINE-POWERED EXPLOSION OF A STRIPPED MASSIVE STAR

Nicholl

Berger

Margutti

et al. 2016

ApJL

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109

117

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We present nebular-phase imaging and spectroscopy for the hydrogen-poor superluminous supernova SN 2015bn, at redshift z = 0.1136, spanning +250-400 d after maximum light. The light curve exhibits a steepening in the decline rate from 1.4 mag (100 d) −1 to 1.7 mag (100 d) −1 , suggestive of a significant decrease in the opacity. This change is accompanied by a transition from a blue continuum superposed with photospheric absorption lines to a nebular spectrum dominated by emission lines of oxygen, calcium and magnesium. There are no obvious signatures of circumstellar interaction or large 56 Ni mass. We show that the spectrum at +400 d is virtually identical to a number of energetic Type Ic supernovae such as SN 1997dq, SN 2012au, and SN 1998bw, indicating similar core conditions and strengthening the link between 'hypernovae'/long gamma-ray bursts and superluminous supernovae. A single explosion mechanism may unify these events that span absolute magnitudes of −22 < M B < −17. Both the light curve and spectrum of SN 2015bn are consistent with an engine-driven explosion ejecting 7 − 30 M of oxygen-dominated ejecta (for reasonable choices in temperature and opacity). A strong and relatively narrow O I λ7774 line, seen in a number of these energetic events but not in normal supernovae, may point to an inner shell that is the signature of a central engine.

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Long-duration superluminous supernovae at late times

Cited by 6 publications

References 0 publications

Supernova ejecta with a relativistic wind from a central compact object: a unified picture for extraordinary supernovae

Supernova ejecta with a relativistic wind from a central compact object: a unified picture for extraordinary supernovae

Analyzing the Largest Spectroscopic Data Set of Hydrogen-poor Super-luminous Supernovae

SUPERLUMINOUS SUPERNOVA SN 2015bn IN THE NEBULAR PHASE: EVIDENCE FOR THE ENGINE-POWERED EXPLOSION OF A STRIPPED MASSIVE STAR

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