Supernova PTF 09uj: A Possible Shock Breakout From a Dense Circumstellar Wind

Ofek, E. O.; Rabinak, Itay; Neill, James D.; Arcavi, I.; Cenko, S. B.; Waxman, Eli; Kulkarni, S. R.; Gal‐Yam, A.; Nugent, P.; Bildsten, Lars; Bloom, J.; Filippenko, A. V.; Forster, Karl; Howell, D. A.; Jacobsen, J.; Kasliwal, M. M.; Law, Nicholas M.; Martin, Charles W.; Poznanski, D.; Quimby, R.; Shen, Ken J.; Sullivan, M.; Dekany, Richard; Rahmer, Gustavo; Hale, David; Smith, R. J.; Zolkower, J.; Velur, V.; Walters, Richard; Henning, John; Bui, K.; McKenna, Dan

doi:10.1088/0004-637x/724/2/1396

Cited by 187 publications

(274 citation statements)

References 39 publications

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“…Ofek et al (2010) suggested that the early light curves of some Type IIn SNe are powered by shock breakout in a dense CSM (see also Chevalier & Irwin 2011). One particular case, PTF 09uj, showed some evidence for a shock breakout from a dense circumstellar wind.…”

Section: Interpretation Of the First Peakmentioning

confidence: 98%

iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

Gorbikov

Gal‐Yam

Ofek

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present optical photometric and spectroscopic observations of the Type Ibn (SN 2006jc-like) supernova iPTF13beo. Detected by the intermediate Palomar Transient Factory ∼3 hours after the estimated first light, iPTF13beo is the youngest and the most distant (∼430 Mpc) Type Ibn event ever observed. The iPTF13beo light curve is consistent with light curves of other Type Ibn SNe and with light curves of fast Type Ic events, but with a slightly faster rise-time of two days. In addition, the iPTF13beo Rband light curve exhibits a double-peak structure separated by ∼9 days, not observed before in any Type Ibn SN. A low-resolution spectrum taken during the iPTF13beo rising stage is featureless, while a late-time spectrum obtained during the declining stage exhibits narrow and intermediate-width He I and Si II features with FWHM ≈ 2000-5000 km s −1 and is remarkably similar to the prototypical SN Ibn 2006jc spectrum. We suggest that our observations support a model of a massive star exploding in a dense He-rich circumstellar medium (CSM). A shock breakout in a CSM model requires an eruption releasing a total mass of ∼0.1 M⊙ over a time scale of couple of weeks prior to the SN explosion.

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Section: Interpretation Of the First Peakmentioning

confidence: 98%

iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

Gorbikov

Gal‐Yam

Ofek

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Although such a radius is 10 times larger than that of WR stars believed to be GRB progenitors, it is appealing that the model can also explain the mysterious UV component in GRB 060218. Envelopes of M ext ∼ 10 −7 M are observed for pre-exploded WRs, but there is increasing evidence for exceptionally high mass loss in the weeks prior to collapse [62,63]. Accompanying theoretical explanations have been proposed [64][65][66].…”

Section: Dynamics Of Relativistic Jetsmentioning

confidence: 99%

Choked jets and low-luminosity gamma-ray bursts as hidden neutrino sources

2016

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We consider gamma-ray burst (GRB) jets that are choked by extended material as sources of high-energy cosmic neutrinos. We take into account the jet propagation physics both inside the progenitor star and the surrounding dense medium. Radiation constraints, which are relevant for high-energy neutrino production are considered as well. Efficient shock acceleration of cosmic rays is possible for sufficiently low-power jets and/or jets buried in a dense, extended wind or outer envelope. Such conditions also favor GRB jets to become stalled, and the necessary conditions for stalling are explicitly derived. Such choked jets may explain transrelativistic supernovae (SNe) and low-luminosity (LL) GRBs, giving a unified picture of GRBs and GRB-SNe. Focusing on this unified scenario for GRBs, we calculate the resulting neutrino spectra from choked jets including the relevant microphysical processes such as multipion production in pp and pγ interactions, as well as the energy losses of mesons and muons. We obtain diffuse neutrino spectra using the latest results for the luminosity function of LL GRBs. Although uncertainties are large, we confirm that LL GRBs can potentially give a significant contribution to the diffuse neutrino flux. Our results are consistent with the present IceCube data and do not violate the stacking limits on classical highluminosity GRBs. We find that high-energy neutrino production in choked jets is dominated by pγ interactions. These sources are dark in GeV-TeV gamma-rays, and do not contribute significantly to the Fermi diffuse gamma-ray background. Assuming stalled jets can launch a quasi-spherical shock in the dense medium, "precursor" TeV neutrinos emerging prior to the shock breakout gamma-ray emission can be used as smoking gun evidence for a choked jet model for LL GRBs. Our results strengthen the relevance of wide field-of-view sky monitors with better sensitivities in the 1−100 keV range.PACS numbers: 95.85. Ry, 97.60.Bw, 98.70.Rz

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“…We also added to this table SN 2009ip, for which similar outbursts were detected and characterized. If these SN light curves are powered by shock breakout followed by interaction of the SN ejecta with a dense CSM, then we expect that some of the outburst and SN properties will be correlated (Ofek et al 2010, Ofek et al 2014a, 2014bSvirski et al 2012). If a substantial fraction of Figure 19.…”

Section: Correlation Between the Precursor And Sn Propertiesmentioning

confidence: 99%

“…These are dubbed Type IIn SNe (Schlegel 1990;Filippenko 1997;Kiewe et al 2012) and they probably have massive progenitors (e.g., Gal-Yam & Leonard 2009). Their emission lines likely originate from relatively abundant circumstellar material (CSM) around the SN progenitor star (e.g., Chevalier & Fransson 1994;Chugai & Danziger 1994;Chugai et al 2003;Ofek et al 2007Ofek et al , 2010Ofek et al , 2014bSmith et al 2008Smith et al , 2009), ejected only a short time (on the order of months to decades) prior to the SN explosion (Dessart et al 2009;Gal-Yam & Leonard 2009;Ofek et al 2010Ofek et al , 2013b. Several theoretical mechanisms have been suggested to explain this high mass loss in the final stages of stellar evolution (e.g., Rakavy et al 1967;Woosley et al 2007;Yoon & Cantiello 2010;Arnett & Meakin 2011;Chevalier 2012;Quataert & Shiode 2012;Shiode & Quataert 2014;Soker & Kashi 2013).…”

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

231

262

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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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Supernova PTF 09uj: A Possible Shock Breakout From a Dense Circumstellar Wind

Cited by 187 publications

References 39 publications

iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

iPTF13beo: the double-peaked light curve of a Type Ibn supernova discovered shortly after explosion

Choked jets and low-luminosity gamma-ray bursts as hidden neutrino sources

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

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