Hydrogen-poor superluminous stellar explosions

Quimby, R.; Kulkarni, S. R.; Kasliwal, M. M.; Gal‐Yam, A.; Arcavi, I.; Sullivan, M.; Nugent, P.; Thomas, R. C.; Howell, D. A.; Nakar, Ehud; Bildsten, Lars; Theissen, Christopher A.; Law, Nicholas M.; Dekany, Richard; Rahmer, Gustavo; Hale, David; Smith, Roger M.; Ofek, E. O.; Zolkower, Jeffry; Velur, V.; Walters, Richard; Henning, John; Bui, K.; McKenna, D.; Poznanski, D.; Cenko, S. B.

doi:10.1038/nature10095

Cited by 501 publications

(557 citation statements)

References 17 publications

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“…The SLSN PTF09cnd (Quimby et al 2011), discovered by the Palomar Transient Factory (PTF), has coverage of both the pre-and post-maximum epochs. We use the original classification spectrum taken at the 4.2-m William Herschel Telescope (WHT) with the Intermediate dispersion Spectrograph and Imaging System (ISIS), as well as two later spectra taken at the 10-m Keck-I telescope with the Low Resolution Imaging Spectrograph (LRIS) (see Quimby et al 2011, for details on the spectra).…”

Section: Line-rich Slsne: Ptf09cndmentioning

confidence: 99%

“…We use the original classification spectrum taken at the 4.2-m William Herschel Telescope (WHT) with the Intermediate dispersion Spectrograph and Imaging System (ISIS), as well as two later spectra taken at the 10-m Keck-I telescope with the Low Resolution Imaging Spectrograph (LRIS) (see Quimby et al 2011, for details on the spectra). Because of the relatively low redshift (z = 0.258), data only cover the UV redwards of 2500 Å. PTF09cnd was significantly less luminous than iPTF13ajg, and reached maximum more rapidly, but its spectra resemble those of iPTF13ajg, showing the O II line series in the optical prior to maximum and a few strong metal lines in the only partially observed near-UV.…”

Section: Line-rich Slsne: Ptf09cndmentioning

confidence: 99%

“…A variety of SLSN spectra have been presented in various papers (e.g., Quimby et al 2011;Chomiuk et al 2011;Inserra et al 2013;Vreeswijk et al 2014;Nicholl et al 2014). Only in a few cases are time-series of spectra available.…”

Section: Introductionmentioning

confidence: 99%

“…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%

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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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137

235

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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: Line-rich Slsne: Ptf09cndmentioning

confidence: 99%

Section: Line-rich Slsne: Ptf09cndmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Spectrum formation in superluminous supernovae (Type I)

Mazzali

Sullivan

Pian

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

137

235

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“…A number of broad absorption features are visible at wavelengths shorter than 5000Å. These absorptions somewhat resemble the O II features observed in spectra of superluminous stripped envelope SNe (such as SNe 2005ap and 2010gx, see Figure 4, Quimby et al 2011;Pastorello et al 2010) or even the putative higher ionization CNO lines detected by Modjaz et al (2009) in the earliest spectrum of the more canonical Type Ib SN 2008D. In order to identify the lines in this early spectrum, we computed a model using the spectral synthesis code SYNOW (Fisher 2000).…”

Section: Spectral Evolutionmentioning

confidence: 65%

Massive stars exploding in a He-rich circumstellar medium – V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006

Pastorello

Wyrzykowski

Valenti

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present optical observations of the peculiar Type Ibn supernova (SN Ibn) OGLE-2012-SN-006, discovered and monitored by the OGLE − IV survey, and spectroscopically followed by P ESST O at late phases. Stringent pre-discovery limits constrain the explosion epoch with fair precision to JD = 2456203.8 ± 4.0. The rise time to the I-band light curve maximum is about two weeks. The object reaches the peak absolute magnitude M I = −19.65 ± 0.19 on JD = 2456218.1 ± 1.8. After maximum, the light curve declines for about 25 days with a rate of 4 mag 100d −1 . The symmetric I-band peak resembles that of canonical Type Ib/c supernovae (SNe), whereas SNe Ibn usually exhibit asymmetric and narrower early-time light curves. Since 25 days past maximum, the light curve flattens with a decline rate slower than that of the 56 Co to 56 Fe decay, although at very late phases it steepens to approach that rate. However, other observables suggest that the match with the 56 Co decay rate is a mere coincidence, and the radioactive decay is not the main mechanism powering the light curve of OGLE-2012-SN-006. An early-time spectrum is dominated by a blue continuum, with only a marginal evidence for the presence of He I lines marking this SN Type. This spectrum shows broad absorptions bluewards than 5000Å, likely O II lines, which are similar to spectral features observed in super-luminous SNe at early epochs. The object has been spectroscopically monitored by P ESST O from 90 to 180 days after peak, and these spectra show the typical features observed in a number of SN 2006jc-like events, including a blue spectral energy distribution and prominent and narrow (v F W HM ≈ 1900 km s −1 ) He I emission lines. This suggests that the ejecta are interacting with He-rich circumstellar material. The detection of broad (10 4 km s −1 ) O I and Ca II features likely produced in the SN ejecta (including the [O I] λλ6300,6364 doublet in the latest spectra) lends support to the interpretation of OGLE-2012-SN-006 as a core-collapse event.

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Stellar Forensics with the Supernova‐GRB Connection

Modjaz¹

2011

Reviews in Modern Astronomy

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Long-duration gamma-ray bursts (GRBs) and Type Ib/c Supernovae (SNe Ib/c) are amongst nature's most magnificent explosions. While GRBs launch relativistic jets, SNe Ib/c are core-collapse explosions whose progenitors have been stripped of their hydrogen and helium envelopes. Yet for over a decade, one of the key outstanding questions is which conditions lead to each kind of explosion and death in massive stars. Determining the fates of massive stars is not only a vibrant topic in itself, but also impacts using GRBs as star formation indicators over distances of up to 13 billion light-years and for mapping the chemical enrichment history of the universe. This article reviews a number of comprehensive observational studies that probe the progenitor environments, their metallicities and the explosion geometries of SN with and without GRBs, as well as the emerging field of SN environmental studies. Furthermore, it discusses SN 2008D/XRT 080109 which was discovered serendipitously with the Swift satellite via its X-ray emission from shock breakout, and which has generated great interest amongst both observers and theorists while illustrating a novel technique for stellar forensics. The article concludes with an outlook on how the most promising venues of research -with the many existing and upcoming large-scale surveys such as the Palomar Transient Factory and LSST -will shed new light on the diverse deaths of massive stars.

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Hydrogen-poor superluminous stellar explosions

Cited by 501 publications

References 17 publications

Spectrum formation in superluminous supernovae (Type I)

Spectrum formation in superluminous supernovae (Type I)

Massive stars exploding in a He-rich circumstellar medium – V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006

Stellar Forensics with the Supernova‐GRB Connection

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