THE DOUBLE-PEAKED SN 2013ge: A TYPE Ib/c SN WITH AN ASYMMETRIC MASS EJECTION OR AN EXTENDED PROGENITOR ENVELOPE

Drout, M. R.; Milisavljevic, Dan; Parrent, J.; Margutti, R.; Kamble, A.; Söderberg, A. M.; Challis, P.; Chornock, R.; Fong, W.; Frank, Stuart D.; Gehrels, N.; Graham, M. L.; Hsiao, E. Y.; Itagaki, K.; Kasliwal, M. M.; Kirshner, R.; Macomb, D. J.; Marion, G. H.; Norris, J. P.; Phillips, M. M.

doi:10.3847/0004-637x/821/1/57

Cited by 82 publications

(100 citation statements)

References 158 publications

(203 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Examples of SNe IIb that were comprehensively studied in single-object papers are: SN 1993J (Filippenko et al 1993(Filippenko et al , 1994, SN 2008ax (Pastorello et al 2008;Chornock et al 2011;Taubenberger et al 2011;Folatelli et al 2015), SN 2011dh (Bersten et al 2012;Ergon et al 2014Ergon et al , 2015, SN 2011hs (Bufano et al 2014), SN 2010as (Folatelli et al 2014b), and PTF12os (Fremling et al 2016). Among the studies of SNe Ib, we find: SN 1996N (Sollerman et al 1998), SN 1999dn (Cano et al 2014), SN 2005bf (Anupama et al 2005;Tominaga et al 2005;Folatelli et al 2006), SN 2007Y ), SN 2008D (Soderberg et al 2008;Mazzali et al 2008;Modjaz et al 2009;Malesani et al 2009;Bersten et al 2013), SN 2009jf (Valenti et al 2011), SN 2013ge (Drout et al 2016), amd iPTF13bvn (Cao et al 2013;Fremling et al 2014;Bersten et al 2014;Fremling et al 2016). Finally, SNe Ic and Ic-BL examined in dedicated papers are: SN 1994I (Filippenko et al 1995), SN 1997ef (Iwamoto et al 2000Mazzali, Iwamoto, & Nomoto 2000) SN 1998bw (Galama et al 1998;Patat et al 2001), SN 2002ap (Foley et al 2003) SN 2003jd (Valenti et al 2008a) SN 2004aw (Taubenberger et al 2006), SN 2006aj (Mirabal et al 2006; Modjaz et al 2006;…”

Section: Introductionmentioning

confidence: 73%

The Carnegie Supernova Project I

Taddia

Stritzinger

Bersten

et al. 2018

A&A

Self Cite

175

285

View full text Add to dashboard Cite

Stripped-envelope (SE) supernovae (SNe) include H-poor (Type IIb), H-free (Type Ib) and He-free (Type Ic) events thought to be associated with the deaths of massive stars. The exact nature of their progenitors is a matter of debate with several lines of evidence pointing towards intermediate mass (Minit < 20 M⊙) stars in binary systems, while in other cases they may be linked to single massive Wolf-Rayet stars. Here we present the analysis of the light curves of 34 SE SNe published by the Carnegie Supernova Project (CSP-I), which are unparalleled in terms of photometric accuracy and wavelength range. Light-curve parameters are estimated through the fits of an analytical function and trends are searched for among the resulting fit parameters. Detailed inspection of the dataset suggests a tentative correlation between the peak absolute B-band magnitude and ∆m15(B), while the post maximum light curves reveals a correlation between the late-time linear slope and ∆m15. Making use of the full set of optical and near-IR photometry, combined with robust host-galaxy extinction corrections, comprehensive bolometric light curves are constructed and compared to both analytic and hydrodynamical models. This analysis finds consistent results among the two different modeling techniques and from the hydrodynamical models we obtained ejecta masses of 1.1 − 6.2 M⊙, 56 Ni masses of 0.03 − 0.35 M⊙, and explosion energies (excluding two SNe Ic-BL) of 0.25 − 3.0 × 10 51 erg. Our analysis indicates that adopting κ = 0.07 cm 2 g −1 as the mean opacity serves to be a suitable assumption when comparing Arnett-model results to those obtained from hydrodynamical calculations. We also find that adopting He I and O I line velocities to infer the expansion velocity in He-rich and He-poor SNe, respectively, provides ejecta masses relatively similar to those obtained by using the Fe II line velocities, although the use of Fe II as a diagnostic does imply higher explosion energies. The inferred range of ejecta masses are compatible with intermediate mass (MZAMS ≤ 20 M ⊙ ) progenitor stars in binary systems for the majority of SE SNe. Furthermore, our hydrodynamical modeling of the bolometric light curves suggest a significant fraction of the sample may have experienced significant mixing of 56 Ni, particularly in the case of SNe Ic.

show abstract

Section: Introductionmentioning

confidence: 73%

The Carnegie Supernova Project I

Taddia

Stritzinger

Bersten

et al. 2018

A&A

Self Cite

175

285

View full text Add to dashboard Cite

show abstract

“…Some SE SNe, such as SN Ib 1999ex (Stritzinger et al 2002), SN Ib 2008D (Soderberg et al 2008Malesani et al 2009;Modjaz et al 2009), SN Ib/IIb iPTF13bvn (Fremling et al 2016), and many SNe IIb (e.g., SN 1993J, Richmond et al 1994SN 2011dh, Arcavi et al 2011Ergon et al 2014), do show this kind of early emission. The type Ib/c SN 2013ge showed an early peak but only in the ultra-violet (UV) light curves (Drout et al 2016). For SN 2008D, the early peak in the optical has been explained by different scenarios: as a result of the presence of 56 Ni in the outermost layers or as the consequence of a modified density structure within the helium progenitor star (Bersten et al 2013); as a shock-breakout (Rabinak & Waxman 2011); or as the effect of a jet in the explosion .…”

Section: Introductionmentioning

confidence: 99%

iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Taddia

Fremling

Sollerman

et al. 2016

A&A

Self Cite

View full text Add to dashboard Cite

Context. Type Ic supernovae (SNe Ic) arise from the core-collapse of H-(and He-) poor stars, which could either be single Wolf-Rayet (WR) stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak (∼10−15 d), without any early (in the first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D). Aims. We have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long (∼30 d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic to be observed. Our aim is to determine the properties of this explosion and of its progenitor star. Methods. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modeled with hydrodynamical and analytical models, with particular focus on the early emission. Results. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modeling of the bolometric properties reveals a large ejecta mass (∼10 M ) and strong 56 Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended ( 500 R ), low-mass ( 0.045 M ) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored. Conclusions. The large ejecta mass and the presence of H-and He-free extended material around the star suggest that the progenitor of iPTF15dtg was a massive ( 35 M ) WR star that experienced strong mass loss.

show abstract

“…Ic SNe associated with GRBs, may be surrounded by an extended low-mass envelope (Nakar & Piro 2014;Nakar 2015;Drout et al 2016;Nicholl & Smartt 2016;Taddia et al 2016, see also Chapter 2). In this case regimes 2, 3 and 4 may all be encountered, depending on the jet and envelope properties.…”

Section: Dynamics Of Relativistic Jetsmentioning

confidence: 99%

“…Furthermore, optical observations generally constrain R ext to be in the range of a few 10 12 cm to a few 10 13 cm (Nakar 2015;Drout et al 2016;Irwin & Chevalier 2016;Taddia et al 2016). Another option is to decrease t j directly, but this runs into a limit because it must remain somewhat longer than t b, * .…”

Section: /2mentioning

confidence: 99%

See 1 more Smart Citation

Long-Duration, Low-Luminosity Gamma-Ray Bursts: Towards a Comprehensive Model of the Weakest Engine-Driven Explosions

Irwin¹

View full text Add to dashboard Cite

Long-duration, low-luminosity gamma-ray bursts (LLGRBs) are a peculiar subclass of gamma-ray bursts (GRBs) that are up to 5 orders of magnitude less luminous than typical bursts. The observation of Type Ic supernovae (SNe) accompanying LLGRBs supports the notion that, like typical GRBs, they are powered by the gravitational collapse of a massive star's core, but beyond this little is known about their origin, and the differences between the progenitors of LLGRBs and GRBs are unclear.In this dissertation, I present analytical and numerical modeling that aims to improve our understanding of the physical conditions leading to LLGRBs.We consider first the unusual GRB 060218, a well-studied event that is prototypical of the long-duration LLGRB class. We present a model for this burst that can account for the prompt X-ray emission lasting for ∼ 3000 s, the early optical peak lasting for hours, and the X-ray and radio afterglow lasting for several days.The basic ingredients of the model are a long-lived jet (t j ∼ 3000 s) with an unusually low luminosity (L j ∼ 10 47 erg s −1 ), a progenitor star surrounded by an extended (∼ 10 13 cm), optically thick, low-mass (∼ 10 −2 M ) envelope, and a modest amount of dust (A V ∼ 0.1) in the interstellar environment.We fit the observed thermal component of the prompt X-ray emission with a simple photospheric model, and then calculate the nonthermal emission due to inverseCompton (IC) scattering of thermal photons from the external shocks of the jet. We find that this model can fit the observed nonthermal emission, if the conditions are such that the reverse shock dominates the emission. We show that the low-power jet can successfully traverse the progenitor star and extended envelope, and that it can also produce the observed radio emission via external shock synchrotron emission at late times. In the meantime, fast ejecta from the associated SN 2006aj shock the iii extended envelope, which emits a burst of optical emission as it expands and cools, consistent with the early optical peak. We interpret the anomalous X-ray afterglow in GRB 060218 as a light echo from dust situated ∼ 30 pc from the burst. Our results suggest that LLGRB progenitors are shrouded in dense circumstellar envelopes, and that they require both a jet and a supernova. Support for this view comes fromNakar (2015), who considered a different model for LLGRBs involving choked jets, but arrived at the same main conclusions.Motivated by these results, we also perform numerical simulations of jets with standard GRB properties in stars with extended envelopes. We present analytical calculations that predict whether or not the jet escapes successfully from the envelope, and apply them to interpret the numerical results. We find that the jet-driven outflow is more well-confined by the envelope than previous analytical results suggested, leading to a flow that is far from spherically symmetric when it breaks out of the envelope. This is generally true for a wide range of physical parameters. Even though the outf...

show abstract

THE DOUBLE-PEAKED SN 2013ge: A TYPE Ib/c SN WITH AN ASYMMETRIC MASS EJECTION OR AN EXTENDED PROGENITOR ENVELOPE

Cited by 82 publications

References 158 publications

The Carnegie Supernova Project I

The Carnegie Supernova Project I

iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Long-Duration, Low-Luminosity Gamma-Ray Bursts: Towards a Comprehensive Model of the Weakest Engine-Driven Explosions

Contact Info

Product

Resources

About