LSQ13ddu: a rapidly evolving stripped-envelope supernova with early circumstellar interaction signatures

Clark, P.; Maguire, K.; Inserra, C.; Prentice, S.; Smartt, S. J.; Contreras, C.; Hossenizadeh, Griffin; Hsiao, E. Y.; Kankare, E.; Kasliwal, Mansi M.; Nugent, P.; Shahbandeh, Melissa; Baltay, C.; Rabinowitz, D.; Arcavi, I.; Ashall, C.; Burns, Christopher R.; Callis, E.; Chen, Ting-Wan; Diamond, T.; Fraser, M.; Howell, D. A.; Karamehmetoglu, E.; Kotak, R.; Lyman, J. D.; Morrell, N.; Phillips, M. M.; Pignata, G.; Pursiainen, M.; Sollerman, J.; Stritzinger, Maximilian; Sullivan, M.; Young, D. R.

doi:10.1093/mnras/stz3598

Cited by 22 publications

(22 citation statements)

References 103 publications

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“…Recent examples of SNe with evidence for early interaction include Type II SNe such as SN 2016bkv (Nakaoka et al 2018), SN 2018zd (Zhang et al 2020), and many others (Khazov et al 2016;Förster et al 2018), and Type I SNe such as LSQ 13abf (Stritzinger et al 2020), LSQ 13ddu (Clark et al 2020), SN 2018bgv and SN 2018don (Lunnan et al 2020), SN 2018gep (Ho et al 2019), SN 2019dge (Yao et al 2020), and SN 2019uo (Gangopadhyay et al 2020). These SNe extend across virtually all spectroscopic classes of SNe (including Type II-P, II-L, IIn, Ib, Ic, Ibn, Ic-BL, superluminous Ic, etc.).…”

Section: Introductionmentioning

confidence: 99%

A Diversity of Wave-driven Presupernova Outbursts

Fuller

2020

ApJ

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Many core-collapse supernova (SN) progenitors show indications of enhanced pre-SN mass loss and outbursts, some of which could be powered by wave energy transport within the progenitor star. Depending on the star's structure, convectively excited waves driven by late-stage nuclear burning can carry substantial energy from the core to the envelope, where the wave energy is dissipated as heat. We examine the process of wave energy transport in single-star SNe progenitors with masses between 11 and 50 M e . Using MESA stellar evolution simulations, we evolve stars until core collapse and calculate the wave power produced and transmitted to the stars' envelopes. These models improve upon prior efforts by incorporating a more realistic wave spectrum and nonlinear damping effects, reducing our wave-heating estimates by ∼1 order of magnitude compared to prior work. We find that waves excited during oxygen/neon burning typically transmit ∼10 46 -10 47 erg of energy at 0.1-10 yr before core collapse in typical (M<30 M e ) SN progenitors. High-mass progenitors can often transmit ∼10 47 -10 48 erg of energy during oxygen/neon burning, but this tends to occur later, at about 0.01-0.1 yr before core collapse. Pre-SN outbursts may be most pronounced in low-mass SN progenitors (M12 M e ) undergoing semidegenerate neon ignition and in high-mass progenitors (M30 M e ) exhibiting convective shell mergers.

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Section: Introductionmentioning

confidence: 99%

A Diversity of Wave-driven Presupernova Outbursts

Fuller

2020

ApJ

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“…SN 2015G is most like SN 2018gjx and is plotted using the estimated explosion date of 3 d prior to the discovery date (2015-03-23.778, but see Shivvers et al 2017b, for a discussion on t exp ). SN 2006jc displays an inverted evolution to that of SN 2018gjx, and two other SNe Ibn LSQ13ddu (Clark et al 2020) and SN 2014av (Pastorello et al 2016), appear to follow the trend of blue to red, albeit from a bluer starting point.…”

Section: G − R Colour Curvesmentioning

confidence: 92%

“…As noted in Section 4.1, our +2.4 d spectrum has He I P-Cygni features consistent with velocities ∼1500 km s −1 , which is at the upper end of the Pastorello et al (2016) distribution. However, as discussed in Clark et al (2020), the resolution of the spectra is also important when making velocity comparisons and can result in higher measured values than are intrinsically present.…”

Section: Characterizing Emission Features Using Gaussian Line Fittingmentioning

confidence: 99%

SN 2018gjx reveals that some SNe Ibn are SNe IIb exploding in dense circumstellar material

Prentice

Maguire

Boian

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the data and analysis of SN 2018gjx, an unusual low-luminosity transient with three distinct spectroscopic phases. Phase I shows a hot blue spectrum with signatures of ionised circumstellar material (CSM), Phase II has the appearance of broad SN features, consistent with those seen in a Type IIb supernova at maximum light, and Phase III is that of a supernova interacting with helium-rich CSM, similar to a Type Ibn supernova. This event provides an apparently rare opportunity to view the inner workings of an interacting supernova. The observed properties can be explained by the explosion of a star in an aspherical CSM. The initial light is emitted from an extended CSM (∼4000 R⊙), which ionises the exterior unshocked material. Some days after, the SN photosphere envelops this region, leading to the appearance of a SN IIb. Over time, the photosphere recedes in velocity space, revealing interaction between the supernova ejecta and the CSM that partially obscures the supernova nebular phase. Modelling of the initial spectrum reveals a surface composition consistent with compact H-deficient Wolf-Rayet and LBV stars. Such configurations may not be unusual, with SNe IIb being known to have signs of interaction so at least some SNe IIb and SNe Ibn may be the same phenomena viewed from different angles or, possibly with differing CSM configurations.

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“…We measure from a selection of He lines in the +47 days Keck spectrum an absorption velocity of 230 ± 130 km s −1 , relative to the intermediate-width emission line centers. Based on the analysis of similar features in SN Ibn LSQ13ddu (Clark et al 2020) in low and high resolution spectra, this velocity can be considered an upper limit to the velocity of the unperturbed CSM around SN 2020bqj due to our lack of spectra with high spectral resolution.…”

Section: Spectral Line Evolutionmentioning

confidence: 99%

“…Normal SE SNe (Type Ib/c) have lightcurves that are generally consistent with powering by the decay of radioactive material synthesized in the explosion and present in the ejecta ( 56 Ni → 56 Co → 56 Fe, e.g., Prentice et al 2016. In the case of SNe Ibn, however, the high peak luminosity and the rapid lightcurve evolution typically exclude 56 Ni decay as the main powering mechanism for their lightcurves, as the decline rate is usually too steep to reconcile with the amount of 56 Ni required to explain the peak luminosity (e.g., Moriya & Maeda 2016). Instead, models combining radioactive decay and interaction with a (He-rich) CSM shell have been used to reproduce the observed fast-evolving SN Ibn lightcurves (Karamehmetoglu et al 2019;Wang & Li 2019;Clark et al 2020;Gangopadhyay et al 2020). These model fits result in 56 Ni and CSM masses that are consistent with WR progenitors, although they are affected by substantial uncertainties and degeneracy given the large number of free model parameters.…”

Section: Introductionmentioning

confidence: 99%

SN 2020bqj: A Type Ibn supernova with a long-lasting peak plateau

Kool

Karamehmetoglu

Sollerman

et al. 2021

A&A

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Context. Type Ibn supernovae (SNe Ibn) are a rare class of stripped envelope supernovae interacting with a helium-rich circumstellar medium (CSM). The majority of the SNe Ibn reported in the literature display a surprising homogeneity in their fast-evolving lightcurves and are typically found in actively starforming spiral galaxies. Aims. We present the discovery and the study of SN 2020bqj (ZTF20aalrqbu), a SN Ibn with a long-duration peak plateau lasting 40 days and hosted by a faint low-mass galaxy. We aim to explain its peculiar properties using an extensive photometric and spectroscopic data set. Methods. We compare the photometric and spectral evolution of SN 2020bqj with regular SNe Ibn from the literature, as well as with other outliers in the SN Ibn subclass. We fit the bolometric and multi-band lightcurves with powering mechanism models such as radioactive decay and CSM interaction. We also model the host galaxy of SN 2020bqj. Results. The risetime, peak magnitude and spectral features of SN 2020bqj are consistent with those of most SNe Ibn, but the SN is a clear outlier in the subclass based on its bright, long-lasting peak plateau and the low mass of its faint host galaxy. We show through modeling that the lightcurve of SN 2020bqj can be powered predominantly by shock heating from the interaction of the SN ejecta and a dense CSM, combined with radioactive decay. The peculiar Type Ibn SN 2011hw is a close analog to SN 2020bqj in terms of lightcurve and spectral evolution, suggesting a similar progenitor and CSM scenario. In this scenario a very massive progenitor star in the transitional phase between a luminous blue variable and a compact Wolf-Rayet star undergoes core-collapse, embedded in a dense helium-rich CSM with an elevated opacity compared to normal SNe Ibn, due to the presence of residual hydrogen. This scenario is consistent with the observed properties of SN 2020bqj and the modeling results. Conclusions. SN 2020bqj is a compelling example of a transitional SN Ibn/IIn based on not only its spectral features, but also its lightcurve, host galaxy properties and the inferred progenitor properties. The strong similarity with SN 2011hw suggests this subclass may be the result of a progenitor in a stellar evolution phase that is distinct from those of progenitors of regular SNe Ibn.

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LSQ13ddu: a rapidly evolving stripped-envelope supernova with early circumstellar interaction signatures

Cited by 22 publications

References 103 publications

A Diversity of Wave-driven Presupernova Outbursts

A Diversity of Wave-driven Presupernova Outbursts

SN 2018gjx reveals that some SNe Ibn are SNe IIb exploding in dense circumstellar material

SN 2020bqj: A Type Ibn supernova with a long-lasting peak plateau

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