DETECTION OF AN OUTBURST ONE YEAR PRIOR TO THE EXPLOSION OF SN 2011ht

Fraser, M.; Magee, M.; Kotak, R.; Smartt, S. J.; Smith, K.; Polshaw, J.; Drake, A. J.; Boles, T.; Lee, Chien‐Hsiu; Burgett, W. S.; Chambers, K.; Draper, P. W.; Flewelling, H.; Hodapp, Klaus W.; Kaiser, N.; Kudritzki, R. P.; Magnier, E. A.; Price, P. A.; Tonry, J.; Wainscoat, R. J.; Waters, C.

doi:10.1088/2041-8205/779/1/l8

Cited by 103 publications

(90 citation statements)

References 44 publications

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“…Finally, one of the SNe IIn with the LC plateau, SN 2011ht, is found to have brightened a year before the major luminosity increase in 2011 (Fraser et al 2013). If SN 2011ht is associated with a super-AGB star, the pre-outburst could be related to the thermal pulses of He-shell burning in the super-AGB progenitor.…”

Section: Type Iin Supernovae With Lc Plateau (Type Iin-p)mentioning

confidence: 97%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

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The most massive stars on the asymptotic giant branch (AGB), or the so-called super-AGB stars, are thought to produce supernovae triggered by electron captures in their degenerate O+Ne+Mg cores. Super-AGB stars are expected to have slow winds with high mass-loss rates, so their circumstellar density is high. The explosions of super-AGB stars are therefore presumed to occur in this dense circumstellar environment. We provide the first synthetic light curves for such events by exploding realistic electron-capture supernova progenitors within their super-AGB winds. We find that the early light curve -that is, before the recombination wave reaches the bottom of the hydrogen-rich envelope of supernova ejecta (the plateau phase) -is not affected by the dense wind. However, after the luminosity drop following the plateau phase, the luminosity remains much higher when the super-AGB wind is taken into account. We compare our results to the historical light curve of SN 1054, the progenitor of the Crab Nebula, and show that the explosion of an electron-capture supernova within an ordinary super-AGB wind can explain the observed light curve features. We conclude that SN 1054 could have been a Type IIn supernova without any extra extreme mass loss, which was previously suggested to be necessary to account for its early high luminosity. We also show that our light curves match Type IIn supernovae with an early plateau phase or the so-called Type IIn-P supernovae, and suggest that they are electron-capture supernovae within super-AGB winds. Although some electron-capture supernovae can be bright in the optical spectral range due to the large progenitor radius, their X-ray luminosity from the interaction does not necessarily get as bright as other Type IIn supernovae whose optical luminosities are also powered by the interaction. Thus, we suggest that optically bright X-ray-faint Type IIn supernovae can emerge from electron-capture supernovae. Optically faint Type IIn supernovae, such as SN 2008S, can also originate from electron-capture supernovae if their hydrogen-rich envelope masses are small. We argue that some of them can be observed as Type IIn-b supernovae due to the small hydrogen-rich envelope mass.

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Section: Type Iin Supernovae With Lc Plateau (Type Iin-p)mentioning

confidence: 97%

Electron-capture supernovae exploding within their progenitor wind

Moriya

Tominaga

Langer

et al. 2014

A&A

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“…in the UVW2 band over 40 days, peaking at a u-band magnitude of about −18. Fraser et al (2013) reported on an outburst peaking at a z-band absolute magnitude of −11.8 detected ∼9 months prior to the explosion, and with the last detection ∼4 months before the explosion. The event was detected by both PanSTARRS-1 and the Catalina Sky Survey.…”

Section: Sn 2011htmentioning

confidence: 99%

“…Recently, five SNe with candidate pre-explosion outbursts (precursors) have been detected a few months to years prior to the SN explosion: SN 2006jc (Foley et al 2007; Pastorello et al 2007), SN 2009ip (Mauerhan et al 2013a(Mauerhan et al , 2014Pastorello et al 2013Ofek et al 2013b), PTF 11qcj (Corsi et al 2014), and SN 2011ht (Fraser et al 2013). In most cases, these precursors were detected from SNe IIn, or closely related events.…”

Section: Introductionmentioning

confidence: 99%

PRECURSORS PRIOR TO TYPE IIn SUPERNOVA EXPLOSIONS ARE COMMON: PRECURSOR RATES, PROPERTIES, AND CORRELATIONS

Ofek

Sullivan

Shaviv

et al. 2014

ApJ

240

264

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There is a growing number of Type IIn supernovae (SNe) which present an outburst prior to their presumably final explosion. These precursors may affect the SN display, and are likely related to poorly charted phenomena in the final stages of stellar evolution. By coadding Palomar Transient Factory (PTF) images taken prior to the explosion, here we present a search for precursors in a sample of 16 Type IIn SNe. We find five SNe IIn that likely have at least one possible precursor event (PTF 10bjb, SN 2010mc, PTF 10weh, SN 2011ht, and PTF 12cxj), three of which are reported here for the first time. For each SN we calculate the control time. We find that precursor events among SNe IIn are common: at the one-sided 99% confidence level, >50% of SNe IIn have at least one pre-explosion outburst that is brighter than 3 × 10 7 L taking place up to 1/3 yr prior to the SN explosion. The average rate of such precursor events during the year prior to the SN explosion is likely 1 yr −1 , and fainter precursors are possibly even more common. Ignoring the two weakest precursors in our sample, the precursors rate we find is still on the order of one per year. We also find possible correlations between the integrated luminosity of the precursor and the SN total radiated energy, peak luminosity, and rise time. These correlations are expected if the precursors are mass-ejection events, and the early-time light curve of these SNe is powered by interaction of the SN shock and ejecta with optically thick circumstellar material.

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“…Some supernova (SN) progenitors exhibit vigorous variability or possible explosive outbursts shortly (weeks to years) prior to the SN explosion (Foley et al 2007;Pastorello et al 2007;2013, Fraser et al 2013Mauerhan et al 2013;Ofek et al 2013aOfek et al , 2013bOfek et al , 2014aMargutti et al 2014). SNe showing such activity are mostly of Type IIn (and Ibn), with spectra showing a blue continuum and hydrogen Balmer (and helium) emission lines (Schlegel 1990;Filippenko 1991Filippenko , 1997Pastorello et al 2008;Kiewe et al 2012).…”

Section: Introductionmentioning

confidence: 99%

PTF13efv—AN OUTBURST 500 DAYS PRIOR TO THE SNHUNT 275 EXPLOSION AND ITS RADIATIVE EFFICIENCY

Ofek

Cenko

Shaviv

et al. 2016

ApJ

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The progenitors of some supernovae (SNe) exhibit outbursts with super-Eddington luminosities prior to their final explosions. This behavior is common among SNe IIn, but the driving mechanisms of these precursors are not yet well-understood. SNHunt 275 was announced as a possible new SN during 2015 May. Here we report on preexplosion observations of the location of this event by the Palomar Transient Factory (PTF) and report the detection of a precursor about 500 days prior to the 2015 May activity (PTF 13efv). The observed velocities in the 2015 transient and its 2013 precursor absorption spectra are low (1000-2000 km s −1 ), so it is not clear yet if the recent activity indeed marks the final disruption of the progenitor. Regardless of the nature of this event, we use the PTF photometric and spectral observations, as well as Swift-UVOT observations, to constrain the efficiency of the radiated energy relative to the total kinetic energy of the precursor. We find that, using an order-of-magnitude estimate and under the assumption of spherical symmetry, the ratio of the radiated energy to the kinetic energy is in the range of 4 × 10 −2 to 3.4 × 10 3 .

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DETECTION OF AN OUTBURST ONE YEAR PRIOR TO THE EXPLOSION OF SN 2011ht

Cited by 103 publications

References 44 publications

Electron-capture supernovae exploding within their progenitor wind

Electron-capture supernovae exploding within their progenitor wind

PRECURSORS PRIOR TO TYPE IIn SUPERNOVA EXPLOSIONS ARE COMMON: PRECURSOR RATES, PROPERTIES, AND CORRELATIONS

PTF13efv—AN OUTBURST 500 DAYS PRIOR TO THE SNHUNT 275 EXPLOSION AND ITS RADIATIVE EFFICIENCY

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