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

Prentice, S.; Maguire, K.; Boian, Ioana; Groh, J. H.; Anderson, J. P.; Barbarino, C.; Bostroem, K. A.; Burke, J.; Clark, P.; Dong, Yize; Fraser, M.; Galbany, L.; Gromadzki, M.; Gutiérrez, C. P.; Howell, D. A.; Hiramatsu, D.; Inserra, C.; James, P. A.; Kankare, E.; Kuncarayakti, H.; Mazzali, Paolo A.; McCully, C.; Müller-Bravo, T. E.; Nichol, M.; Pellegrino, C.; Smartt, S. J.; Sollerman, J.; Tartaglia, L.; Valenti, S.; Young, D. R.

doi:10.1093/mnras/staa2947

Cited by 21 publications

(22 citation statements)

References 132 publications

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“…We note that none of the He i lines display the degree of asymmetry seen in hydrogen, although transients exist displaying double-peaked helium lines, such as the Type Ibn SN 2006jc; (Foley et al 2007;Pastorello et al 2008), as well as some displaying asymmetric He i and symmetric H emission e.g. the Type Ibn/IIb SN 2018gjx (Prentice et al 2020).…”

Section: Helium Evolutionmentioning

confidence: 74%

Photometric and spectroscopic evolution of the interacting transient AT 2016jbu (Gaia16cfr)

Brennan,

Fraser,

Johansson

et al. 2021

Preprint

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We present comprehensive, multi-wavelength observations of AT 2016jbu, an interacting transient. High cadence photometric coverage reveals that AT 2016jbu underwent significant photometric variability followed by two luminous events, the latter of which reached an absolute magnitude of M V ∼ −18.5 mag. This is similar to the transient SN 2009ip whose nature is still debated. Spectra are dominated by narrow emission lines and show a blue continuum during the peak of the second event. AT 2016jbu shows signatures of a complex, non-homogeneous circumstellar material (CSM). We see slowly evolving asymmetric hydrogen line profiles, with velocities of 500 km s −1 seen in narrow emission features from a slow moving CSM, and up to 10,000 km s −1 seen in broad absorption from some high velocity material. Similar velocities are seen in other SN 2009ip-like transients. Late-time spectra (∼ +1 year) show a lack of forbidden emission lines expected from a core-collapse supernova during the nebular phase and are dominated by strong emission from H, He i and Ca ii. Strong asymmetric emission features, a bumpy lightcurve, and continually evolving spectra suggest late time CSM interaction is inhibiting the emergence of any nebular features. We compare the evolution of Hα among SN 2009ip-like transients and find possible evidence for orientation angle effects. The light-curve evolution of AT 2016jbu suggests similar, but not identical, circumstellar environments to other SN 2009ip-like transients. In Paper II we continue the discussion of AT 2016jbu and SN 2009ip-like transients and using the data presented here, we focus on the local environment, the progenitor, and on modelling the transient itself.

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Section: Helium Evolutionmentioning

confidence: 74%

Photometric and spectroscopic evolution of the interacting transient AT 2016jbu (Gaia16cfr)

Brennan,

Fraser,

Johansson

et al. 2021

Preprint

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“…There is precedent for SNe IIb which also show signs of interaction. SN 2018gjx (Prentice et al 2020) was an object which spectroscopically resembled a SN IIb before going on to show narrow spectral features typical of a SN Ibn after ∼40 days, although DES14X2fna is two mags brighter at peak and does not show narrow spectral features during our spectroscopic coverage so is not directly comparable. Our semi-analytic fits using MOSFiT suggest that CSM interaction combined with 56 Ni decay could power the light curve of DES14X2fna.…”

Section: Power Sourcementioning

confidence: 87%

Understanding the extreme luminosity of DES14X2fna

Grayling,

Gutiérrez,

Sullivan

et al. 2021

Preprint

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We present DES14X2fna, a high-luminosity, fast-declining type IIb supernova (SN IIb) at redshift 𝑧 = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching 𝑀 𝑟 −19.3 mag 20 days after explosion. This object does not show a linear decline tail in the light curve until 60 days after explosion, after which it declines very rapidly (4.38±0.10 mag 100 d −1 in 𝑟-band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard 56 Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as a SN Ia in ∼1.1-2.4 per cent of cases in DES, depending on the probability threshold used for a positive classification.

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“…There is precedent for SNe IIb that also show signs of interaction. SN 2018gjx (Prentice et al 2020) was an object that spectroscopically resembled an SN IIb before going on to show narrow spectral features typical of an SN Ibn after ∼40 d, although DES14X2fna is two mags brighter at peak and does not show narrow spectral features during our spectroscopic coverage so is not directly comparable. Our semi-analytic fits using MOSFiT suggest that CSM interaction combined with 56 Ni decay could power the light curve of DES14X2fna.…”

Section: Power Sourcementioning

confidence: 88%

Understanding the extreme luminosity of DES14X2fna

Grayling

Gutiérrez

Sullivan

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

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We present DES14X2fna, a high-luminosity, fast-declining type IIb supernova (SN IIb) at redshift z = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching Mr ≃ −19.3 mag 20 days after explosion. This object does not show a linear decline tail in the light curve until ≃60 days after explosion, after which it declines very rapidly (4.30 ± 0.10 mag 100 d−1 in r-band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard 56Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as a SN Ia in ∼1.1-2.4 per cent of cases in DES, depending on the probability threshold used for a positive classification.

show abstract

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

Cited by 21 publications

References 132 publications

Photometric and spectroscopic evolution of the interacting transient AT 2016jbu (Gaia16cfr)

Photometric and spectroscopic evolution of the interacting transient AT 2016jbu (Gaia16cfr)

Understanding the extreme luminosity of DES14X2fna

Understanding the extreme luminosity of DES14X2fna

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