SN 2019zrk, a bright SN 2009ip analog with a precursor

Fransson, Claes; Sollerman, J.; Strotjohann, N. L.; Yang, S.; Schulze, S.; Barbarino, C.; Kool, Erik C.; Ofek, E. O.; Crellin-Quick, Arien; De, Kishalay; Drake, A. J.; Fremling, Christoffer; Gal‐Yam, A.; Ho, Anna Y. Q.; Kasliwal, M. M.

doi:10.1051/0004-6361/202243452

Cited by 10 publications

(26 citation statements)

References 99 publications

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“…The total radiate energy during the main outburst (which I also refer to as explosion) is E rad,ex ≃ 5 × 10 49 erg. Fransson et al (2022) point out that like the case with SN 2009ip (Margutti et al 2014) the total radiated energy can be much larger due to substantial contribution from UV and X-rays.…”

Section: Introductionmentioning

confidence: 88%

“…In my summary (section 5) I will connect 2009ip-like events to other luminous and superluminous CCSNe. Fransson et al (2022) find the merger scenario to be the most promising to explain the properties of SN 2019zrk. It is not clear whether they refer to a main sequence companion that enters the envelope of a RSG as and Kashi, Soker, & Moskovitz (2013) discussed for SN 2009ip, or whether they refer to a NS (or even a BH) companion that enters the RSG envelop as Gilkis, Soker, & Kashi (2019) suggested already for SN2009ip.…”

Section: Introductionmentioning

confidence: 96%

“…In this study I argue that jets must play the major roles in the pre-explosion (section 2), in the explosion (section 3), and in the post-explosion (section 4) powering of the 2009ip-like event SN 2019zrk. Fransson et al (2022) present a thorough observational study of SN 2019zrk (for an early study see Strotjohann et al 2021). It reached a maximum magnitude of M r = −19.2 and showed expansion velocities of up to v ex ≃ 16, 000 km s −1 .…”

Section: Introductionmentioning

confidence: 96%

“…Let me elaborate on this by referring to two problems that Fransson et al (2022) mention in their discussion of SN 2019zrk. Both of these have already been solved with jets.…”

Section: Introductionmentioning

confidence: 99%

“…Both of these have already been solved with jets. Fransson et al (2022) claim that a possible problem for the merger model might be the large velocity observed in the precursor of SN 2009ip, ≈ 12, 000 km s −1 (Foley et al 2011;Pastorello et al 2013). I disagree, because even for a main sequence companion that launches jets at ≈ 2000 − 3000 km s −1 the interaction of the jets with the CSM can accelerate gas to velocities of 10, 000 km s −1 , as Tsebrenko & Soker (2013) showed for parameters that fit SN 2009ip and Akashi & Kashi (2020) showed for the parameters that fit the Great Eruption of Eta Carinae (an energetic ILOT event).…”

Section: Introductionmentioning

confidence: 99%

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Pre-explosion, explosion, and post-explosion jets in supernova SN 2019zrk

Soker

2022

Preprint

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I analyse some properties of the luminous transient event SN 2019zrk and conclude that jets were the main powering sources of the pre-explosion outburst (pre-cursor) and ejection of a massive circumstellar matter (CSM), of the very energetic explosion itself, and of the post-explosion bump in the light curve. The pre-explosion energy source is mainly a companion (main sequence, Wolf-Rayet, neutron star or black hole) star that accreted mass and launched jets. I find that the fast expansion of the CSM after acceleration by the explosion ejecta requires the explosion energy to be 10 52 erg. Only jetdriven explosions can supply this energy in such SN 2009ip-like transients. I conclude that ejecta-CSM interaction is extremely unlikely to power the bright bump at about 110 days after explosion. Instead, I show by applying a jet-driven bump toy-model that post-explosion jets are the most likely explanation for the bump. I leave open the question of whether the explosion itself (main outburst) was a core collapse supernova (CCSN) or a common envelope jets supernova (CEJSN). In this study I further connect peculiar transient events, here 2009ip-like transient events, to CCSNe by arguing that jets drive all events, from regular CCSNe through superluminous CCSNe and to many other peculiar and super-energetic transient events, including CEJSNe. Jet-powering cannot be ignored when analyzing all these types of transients.

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Section: Introductionmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 96%

Section: Introductionmentioning

confidence: 96%

“…Let me elaborate on this by referring to two problems that Fransson et al (2022) mention in their discussion of SN 2019zrk. Both of these have already been solved with jets.…”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Pre-explosion, explosion, and post-explosion jets in supernova SN 2019zrk

Soker

2022

Preprint

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Multi-epoch variability of AT 2000ch (SN 2000ch) in NGC 3432

Müller

Frohn

Dirks

et al. 2023

A&A

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Context. AT 2000ch is a highly variable massive star and supernova imposter in NGC 3432 first detected in 2000. It is similar and often compared to SN 2009ip, and it is therefore expected to undergo a core-collapse supernova (SN) -a SN imposter of similar brightness-in the near future. Aims. We characterize the long-term variability of AT 2000ch in the radio and optical regimes with archival data reaching back to the year 1984. We use these newly reduced observations in addition to observations in the literature to restrict the mass-loss rates of AT 2000ch at multiple epochs based on different approaches, and to infer the general properties of its circumstellar nebula with respect to the detected radio brightness. Methods. We extend the known optical light curve of AT 2000ch up to the beginning of 2022 by performing point spread function (PSF) photometry on archival data from the Palomar Transient Factory and the Zwicky Transient Facility. We reduced archival radio continuum observations obtained with the Very Large Array using standard calibration and imaging methods and complemented these with pre-reduced chang-es observations as well as observations obtained with the Westerbork Synthesis Radio Telescope and LOw Frequency ARray. For the analysis of AT 2000ch, we consider the optical light curve and color evolution, its radio continuum brightness at different frequencies and times, and the corresponding spectral indices. We estimated mass-loss rates and optical depths based on radio continuum brightnesses and Hα fluxes. Results. We report two newly detected outbursts of AT 2000ch similar to those found in the 2000s and 13 re-brightening events, of which at least four are not conclusively detected because of insufficient sampling of the light curve. The dates of all outbursts and significant, well-sampled re-brightening events are consistent with a period of ∼ 201 ± 12 days over a total time-span of two decades. Such a behavior has never been found for any SN imposter, especially not for candidate SN 2009ip analogs. During 2010 to 2012 and 2014 to 2018, we only have a few detections, which is insufficient to come to any conclusion as to a possible less eruptive phase of the transient. We find steady dimming after the most recent re-brightening events and possible evidence of porosity in the circumstellar envelope, suggesting AT 2000ch may currently be in transition to a state of relative calm. We identified a second, unrelated source at a projected distance of ∼ 23 pc (∼ 0.5 ) that has contaminated the optical measurements of AT 2000ch at its minimum luminosity over the last two decades probably on a 5%−10 % level, but this does not affect our overall findings and is negligible during re-brightening. We are able to restrict the mass-loss rate of AT 2000ch to range between several 10 −6 M /yr and several 10 −5 M /yr. The fresh ejecta appear to be optically thick to radio continuum emission at least within the first ∼ 25 days after significant re-brightening. Conclusions. We suggest that other SN imposter and proba...

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Searching for precursor activity of Type IIn supernovae

Reguitti,

Pignata,

Pastorello

et al. 2024

A&A

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We conducted a search for luminous outbursts prior to the explosion of Type IIn supernovae (SNe IIn). We built a sample of 27 objects spectroscopically classified as SNe IIn and all located at $z<0.015$. Using deep archival SN fields images ---taken up to nearly 20 years prior to the SN explosions themselves--- from transient surveys (PTF, ZTF, DES and CHASE) and major astronomical observatories (European Southern Observatory, ESO and National Optical Astronomy Observatory, NOAO), we found at least one outburst years to months before the explosion of seven SNe IIn, with the earliest precursor being 10 years prior to the explosion of SN 2019bxq. The maximum absolute magnitudes of the outbursts range between $-$11.5 mag and $-$15 mag, and the eruptive phases last for a few weeks to a few years. The $g-r$ colour measured for three objects during their outburst is relatively red, with $g-r$ ranging between 0.5 and 1.0 mag. This is similar to the colour expected during the eruptions of luminous blue variables. We note that the light curves of SNe with pre-SN outbursts have faster decline rates than those of the SNe that do not show pre-SN outbursts. SN 2011fh is remarkable, as it is still visible 12 years after the luminous SN-like event, indicating that the progenitor possibly survived, or that the interaction is still ongoing. We detect precursor activity in 29<!PCT!> of bona fide SNe IIn in our sample. However, a quantitative assessment of the observational biases affecting the sample suggests that this fraction is an underestimation of the intrinsic precursor occurrence rate.

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SN 2019zrk, a bright SN 2009ip analog with a precursor

Cited by 10 publications

References 99 publications

Pre-explosion, explosion, and post-explosion jets in supernova SN 2019zrk

Pre-explosion, explosion, and post-explosion jets in supernova SN 2019zrk

Multi-epoch variability of AT 2000ch (SN 2000ch) in NGC 3432

Searching for precursor activity of Type IIn supernovae

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