Flash Ionization Signatures in the Type Ibn Supernova SN 2019uo

Gangopadhyay, Anjasha; Misra, Kuntal; Hiramatsu, D.; Wang, Shan-Qin; Hosseinzadeh, G.; Valenti, S.; Zhang, Jujia; Howell, D. Andrew; Arcavi, I.; Anupama, G. C.; Burke, J.; Dastidar, Raya; Itagaki, K.; Kumar, Brajesh; Kumar, Brijesh; Li, Long; McCully, C.; Mo, Jun; Pellegrino, C.; Sai, Hanna; Sahu, D. K.; Sanwal, Pankaj; Singh, Avinash; Singh, Mridweeka; Zhang, Jicheng; Zhang, Tianmeng; Zhang, Xinhan

doi:10.3847/1538-4357/ab6328

Cited by 24 publications

(57 citation statements)

References 49 publications

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“…We measure typical velocities of ∼900 km s −1 (see Table 6), which would imply that the CSM has propagated to a radius of ∼2×10 15 cm when the SN explodes 320 days after the precursor. This radius is approximately consistent with the inner CSM radius required by the modeling of Gangopadhyay et al (2020). Moreover, it roughly coincides with the radius at which the CSM turns optically thin shown in Figure 11: broad features, likely from the shocked CSM, first appear in a spectrum obtained 18 days after the explosion date (see Figure 3 by Gangopadhyay et al 2020).…”

Section: The Type Ibn Sn 2019uosupporting

confidence: 81%

“…This radius is approximately consistent with the inner CSM radius required by the modeling of Gangopadhyay et al (2020). Moreover, it roughly coincides with the radius at which the CSM turns optically thin shown in Figure 11: broad features, likely from the shocked CSM, first appear in a spectrum obtained 18 days after the explosion date (see Figure 3 by Gangopadhyay et al 2020). A CSM shell located at a radius of 2×10 15 cm is swept up by the SN ejecta if they have an average velocity of 13,000 km s −1 .…”

Section: The Type Ibn Sn 2019uosupporting

confidence: 79%

“…Narrow helium features remain visible in later spectra and might originate from an optically thin wind located above the CSM. The same material could also produce the flash-ionization features detected by Gangopadhyay et al (2020) before the SN reaches its peak.…”

Section: The Type Ibn Sn 2019uomentioning

confidence: 95%

“…There is some overlap between flashspectroscopy SNe and the other classes: some flash-spectroscopy SNe show narrow hydrogen lines for several weeks and are here included in the sample of Type IIn SNe (such as SN 2019cmy). SN 2019uo is considered a Type Ibn SN, even though it might show flash-spectroscopy lines at early times (Gangopadhyay et al 2020).…”

Section: Precursor Rates For Different Interacting Snementioning

confidence: 99%

“…It was classified as a Type Ibn based on a spectrum showing narrow helium PCygni features that were obtained nine days after the estimated explosion date (Fremling et al 2019). SN 2019uo was studied by Gangopadhyay et al (2020) in detail, and they find that SN 2019uo is slightly underluminous and evolves quickly, typical for Type Ibn SNe. They model the bolometric light curve with CSM interaction and their best-fitting models require the presence of 0.4-0.7 M e of material located at a radius of (0.2-2) ×10 15 cm.…”

Section: The Type Ibn Sn 2019uomentioning

confidence: 99%

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Bright, Months-long Stellar Outbursts Announce the Explosion of Interaction-powered Supernovae

Strotjohann

Ofek

Gal‐Yam

et al. 2021

ApJ

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Interaction-powered supernovae (SNe) explode within an optically thick circumstellar medium (CSM) that could be ejected during eruptive events. To identify and characterize such pre-explosion outbursts, we produce forcedphotometry light curves for 196 interacting SNe, mostly of Type IIn, detected by the Zwicky Transient Facility between early 2018 and 2020 June. Extensive tests demonstrate that we only expect a few false detections among the 70,000 analyzed pre-explosion images after applying quality cuts and bias corrections. We detect precursor eruptions prior to 18 Type IIn SNe and prior to the Type Ibn SN 2019uo. Precursors become brighter and more frequent in the last months before the SN and month-long outbursts brighter than magnitude −13 occur prior to 25% (5-69%, 95% confidence range) of all Type IIn SNe within the final three months before the explosion. With radiative energies of up to 10 49 erg, precursors could eject ∼1 M e of material. Nevertheless, SNe with detected precursors are not significantly more luminous than other SNe IIn, and the characteristic narrow hydrogen lines in their spectra typically originate from earlier, undetected mass-loss events. The long precursor durations require ongoing energy injection, and they could, for example, be powered by interaction or by a continuum-driven wind. Instabilities during the neon-and oxygen-burning phases are predicted to launch precursors in the final years to months before the explosion; however, the brightest precursor is 100 times more energetic than anticipated.

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Section: The Type Ibn Sn 2019uosupporting

confidence: 81%

Section: The Type Ibn Sn 2019uosupporting

confidence: 79%

Section: The Type Ibn Sn 2019uomentioning

confidence: 95%

Section: Precursor Rates For Different Interacting Snementioning

confidence: 99%

Section: The Type Ibn Sn 2019uomentioning

confidence: 99%

See 3 more Smart Citations

Bright, Months-long Stellar Outbursts Announce the Explosion of Interaction-powered Supernovae

Strotjohann

Ofek

Gal‐Yam

et al. 2021

ApJ

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A global look into the world of interacting supernovae

et al. 2022

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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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Flash Ionization Signatures in the Type Ibn Supernova SN 2019uo

Cited by 24 publications

References 49 publications

Bright, Months-long Stellar Outbursts Announce the Explosion of Interaction-powered Supernovae

Bright, Months-long Stellar Outbursts Announce the Explosion of Interaction-powered Supernovae

A global look into the world of interacting supernovae

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

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