A PANCHROMATIC VIEW OF THE RESTLESS SN 2009ip REVEALS THE EXPLOSIVE EJECTION OF A MASSIVE STAR ENVELOPE

Margutti, R.; Milisavljević, D.; Söderberg, A. M.; Chornock, R.; Zauderer, B. A.; Murase, Kohta; Guidorzi, C.; Sanders, Nathan; Kuin, P.; Fransson, Claes; Levesque, Emily M.; Chandra, Poonam; Berger, E.; Bianco, Federica; Brown, P. J.; Challis, Peter; Chatzopoulos, E.; Cheung, C. C.; Choi, Changsu; Chomiuk, Laura; Чугай, Н. Н.; Contreras, C.; Drout, M. R.; Fesen, Robert A.; Foley, R. J.; Fong, W.; Friedman, Andrew S.; Gall, C.; Gehrels, N.; Hjorth, J.; Hsiao, E. Y.; Kirshner, R.; Im, Myungshin; Leloudas, G.; Lunnan, R.; Marion, G. H.; Martin, John; Morrell, N.; Neugent, Kathryn F.; Omodei, N.; Phillips, M. M.; Rest, A.; Silverman, J. M.; Strader, Jay; Stritzinger, M. D.; Szalai, T.; Utterback, N. B.; Vinkó, J.; Wheeler, J. C.; Arnett, David; Campana, S.; Chevalier, Roger A.; Ginsburg, Adam; Kamble, A.; Roming, P. W. A.; Pritchard, T. A.; Stringfellow, Guy S.

doi:10.1088/0004-637x/780/1/21

Cited by 217 publications

(315 citation statements)

References 137 publications

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“…We note that these statistical results are in accord with individual well-studied cases like SN 2009ip, in which several precursors were documented (e.g., Prieto et al 2013;Margutti et al 2014).…”

Section: Precursor Ratesupporting

confidence: 87%

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

Ofek

Sullivan

Shaviv

et al. 2014

ApJ

237

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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Section: Precursor Ratesupporting

confidence: 87%

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

Ofek

Sullivan

Shaviv

et al. 2014

ApJ

237

264

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“…The progenitor of Type IIn SN 2005gl is found to have an absolute brightness of M V −10 mag and it belongs to the most luminous class of stars. The progenitor of Type IIn SN 2009ip provided us with more remarkable information about the progenitors' activities (e.g., Margutti et al 2014;Smith et al 2014;Mauerhan et al 2013;Prieto et al 2013; but see also Fraser et al 2013a;Pastorello et al 2013). The luminosity of the progenitor was again close to M V = −10 mag, and it is presumed to be near the Eddington luminosity.…”

Section: Introductionmentioning

confidence: 98%

Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion

Moriya

2014

A&A

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We present a novel mechanism for enhancing the mass-loss rates of massive stars shortly before their explosion. The neutrino luminosities of the stellar core of massive stars increase as they get closer to the time of the core collapse. As emitted neutrinos escape freely from the core, the core mass is significantly reduced when the neutrino luminosity is high. If a star is near the Eddington luminosity when the neutrino luminosity is high, the star can exceed the Eddington luminosity because of the core neutrino mass loss. We suggest that the stellar surface mass-loss rates due to the core neutrino emission can be higher than 10 −4 M yr −1 from ∼1 year before the core collapse. The mass-loss rates can exceed 10 −2 M yr −1 ∼ 10 days before the core collapse. This mass-loss mechanism may be able to explain the enhanced mass loss observed in some supernova progenitors shortly before their explosion. Even if the star is not close enough to the Eddington luminosity to enhance the mass loss, the star can still expand because of the reduced gravitational force. This mechanism can be activated in Wolf-Rayet stars, and it can create the hydrogen-poor, as well as hydrogen-rich, dense circumstellar media observed in some supernovae.

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“…Intense mass loss via eruptive events sometimes manifests itself as precursors prior to the SN explosion , as in SN 2006jc (Pastorello et al 2007), SN 2010mc (Ofek et al 2013), PTF11qcj (Corsi et al 2014), and possibly SN 2009ip (whether an SN was finally produced is controversial; e.g., Mauerhan et al 2013;Graham et al 2014;Margutti et al 2014;Ofek et al 2014;Martin et al 2015). Mass loss from…”

Section: Introductionmentioning

confidence: 99%

FLASH SPECTROSCOPY: EMISSION LINES FROM THE IONIZED CIRCUMSTELLAR MATERIAL AROUND <10-DAY-OLD TYPE II SUPERNOVAE

Khazov

Yaron

Gal‐Yam

et al. 2016

ApJ

Self Cite

212

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Supernovae (SNe) embedded in dense circumstellar material (CSM) may show prominent emission lines in their early-time spectra ( 10 days after the explosion), owing to recombination of the CSM ionized by the shockbreakout flash. From such spectra ("flash spectroscopy"), we can measure various physical properties of the CSM, as well as the mass-loss rate of the progenitor during the year prior to its explosion. Searching through the Palomar Transient Factory (PTF and iPTF) SN spectroscopy databases from 2009 through 2014, we found 12 SNe II showing flash-ionized (FI) signatures in their first spectra. All are younger than 10 days. These events constitute 14% of all 84 SNe in our sample having a spectrum within 10 days from explosion, and 18% of SNeII observed at ages <5 days, thereby setting lower limits on the fraction of FI events. We classified as "blue/featureless" (BF) those events having a first spectrum that is similar to that of a blackbody, without any emission or absorption signatures. It is possible that some BF events had FI signatures at an earlier phase than observed, or that they lack dense CSM around the progenitor. Within 2 days after explosion, 8 out of 11 SNe in our sample are either BF events or show FI signatures. Interestingly, we found that 19 out of 21 SNe brighter than an absolute magnitude M R =−18.2 belong to the FI or BF groups, and that all FI events peaked above M R =−17.6 mag, significantly brighter than average SNeII.

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A PANCHROMATIC VIEW OF THE RESTLESS SN 2009ip REVEALS THE EXPLOSIVE EJECTION OF A MASSIVE STAR ENVELOPE

Cited by 217 publications

References 137 publications

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

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

Mass loss of massive stars near the Eddington luminosity by core neutrino emission shortly before their explosion

FLASH SPECTROSCOPY: EMISSION LINES FROM THE IONIZED CIRCUMSTELLAR MATERIAL AROUND <10-DAY-OLD TYPE II SUPERNOVAE

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