A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction

Maeda, Keiichi; Chandra, Poonam; Moriya, Takashi J.; Reguitti, A.; Ryder, S. D.; Matsuoka, Tomoki; Michiyama, Tomonari; Pignata, G.; Hiramatsu, D.; Bostroem, K. A.; Kundu, Esha; Kuncarayakti, H.; Bersten, Melina C.; Pooley, David; Lee, S.-H.; Patnaude, Daniel; Rodríguez, Ó.; Folatelli, G.

doi:10.3847/1538-4357/aca1b7

Cited by 12 publications

(32 citation statements)

References 93 publications

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“…Such a scenario may also be in line with its optical spectral features showing broad and boxy emission lines (Dessart & Hillier 2022). Maeda et al (2023) further proposed that SN 2018ivc and a fraction of SNe IIL may be a direct link between SNe IIb and SNe IIP in the binary evolution where the sequence of SNe Ic/Ib-IIb-(some) IIL-IIP is mainly controlled by the initial orbital separation. This is along the same line as previously suggested by Nomoto et al (1995Nomoto et al ( , 1996 but with a substantial difference in the mode of binary interaction (see Section 4 for more details).…”

Section: Introductionmentioning

confidence: 81%

“…Discovered by the D < 40 Mpc SN survey (Tartaglia et al 2018) on 2018 November 24 (UT) within a day of the explosion (Valenti et al 2018;Bostroem et al 2020), SN 2018ivc is an outlier of the SN IIL subclass with its faint and rapidly evolving optical light curve. Maeda et al (2023) presented and analyzed the data taken by the Atacama Large Millimeter/submillimeter Array (ALMA) covering 4-198 days since the (well-determined) explosion date, together with the optical and X-ray light curves. They suggested that SN 2018ivc is indeed an analog of an SN IIb explosion (potentially with a slightly more massive H-rich envelope), with its different observational features from canonical SNe IIb originating in its powering mechanism, the SN-CSM interaction.…”

Section: Introductionmentioning

confidence: 99%

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Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors

Maeda

Michiyama

Chandra

et al. 2023

ApJL

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Long-term observations of synchrotron emission from supernovae (SNe), covering more than a year after the explosion, provide a unique opportunity to study the poorly understood evolution of massive stars in the final millennium of their lives via changes in the mass-loss rate. Here we present a result of our long-term monitoring of the peculiar Type IIL SN 2018ivc using the Atacama Large Millimeter/submillimeter Array. Following the initial decay, it showed unprecedented rebrightening starting ∼1 yr after the explosion. This is one of the rare examples showing such rebrightening in the synchrotron emission and the first case at millimeter wavelengths. We find it to be in the optically thin regime, unlike the optically thick centimeter emission. As such, we can robustly reconstruct the distribution of the circumstellar matter and thus the mass-loss history in the final ≳1000 yr. We find that the progenitor of SN 2018ivc had experienced a very high mass-loss rate (≳10−3 M ⊙ yr−1) ∼1500 yr before the explosion, which was followed by a moderately high mass-loss rate (≳10−4 M ⊙ yr−1) up until the explosion. From this behavior, we suggest that SN 2018ivc represents an extreme version of a binary evolution toward SNe IIb, which bridges the hydrogen-poor SNe (toward SNe Ib/c, without a hydrogen envelope) and hydrogen-rich SNe (SNe IIP, with a massive envelope).

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Section: Introductionmentioning

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors

Maeda

Michiyama

Chandra

et al. 2023

ApJL

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“…It is possible that other SNe IIb with little synthesized 56 Ni may be undercounted due to their rapidly-fading or underluminous light curves. Maeda et al (2023) also concluded that the light curve of SN 2018ivc was powered at least in part by circumstellar interaction. Sustained circumstellar interaction has been inferred for other SNe IIb, either through late-time spectral features (Maeda et al 2015;Fremling et al 2019) or through X-ray and radio observations (Fransson et al 1996).…”

Section: Bolometric Luminosities and Numerical Modelingmentioning

confidence: 96%

“…On the other hand, in the case of SN 2018ivc, both a low 56 Ni mass (M Ni ≤ 0.015M ) and progenitor mass (M ZAMS 12M ) are inferred (Maeda et al 2023). It is possible that other SNe IIb with little synthesized 56 Ni may be undercounted due to their rapidly-fading or underluminous light curves.…”

Section: Bolometric Luminosities and Numerical Modelingmentioning

confidence: 99%

“…ies using samples of these objects have found average 56 Ni masses of ≈ 0.10 -0.15 M and average ejecta masses of ≈ 2.2 -4.5 M (Lyman et al 2016;Prentice et al 2016;Taddia et al 2018), in better agreement with ejecta parameters of other stripped-envelope and H-rich core-collapse SNe. However, rare cases of underluminous SNe IIb with low inferred M Ni have been discovered (e.g., Nakaoka et al 2019;Maeda et al 2023). These objects have light curves that appear transitional between standard SNe II-P and SNe IIb, which differ from the observed photometric evolution of SN 2020bio.…”

Section: Bolometric Luminosities and Numerical Modelingmentioning

confidence: 99%

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SN 2020bio: A Double-peaked Type IIb Supernova with Evidence of Early-time Circumstellar Interaction

Pellegrino¹,

Hiramatsu²,

Arcavi³

et al. 2023

Preprint

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We present photometric and spectroscopic observations of SN 2020bio, a double-peaked Type IIb supernova (SN) discovered within a day of explosion, primarily obtained by Las Cumbres Observatory and Swift. SN 2020bio displays a rapid and long-lasting initial decline throughout the first week of its light curve, similar to other well-studied Type IIb SNe. This early-time emission is thought to originate from the cooling of the extended outer envelope of the progenitor star that is shock-heated by the SN explosion. We compare SN 2020bio to a sample of other double-peaked Type IIb SNe to investigate its progenitor properties. Analytical model fits to the early-time emission give progenitor radius (≈ 100-1500 R ) and H-rich envelope mass (≈ 0.01-0.5 M ) estimates that are consistent with other Type IIb SNe. However, SN 2020bio displays several peculiarities, including: 1) weak H spectral features and narrow emission lines indicative of pre-existing circumstellar material; 2) an underluminous secondary light curve peak which implies a small amount of synthesized 56 Ni (M Ni ≈ 0.02 M ); and 3) lowluminosity nebular [O I] features. These observations are more consistent with a lower-mass progenitor (M ZAMS ≈ 12 M ) that was stripped of most of its H envelope before exploding. This study adds to the growing diversity in the observed properties of Type IIb SNe and their progenitors.

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The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves

Kuncarayakti,

Sollerman,

Izzo

et al. 2023

A&A

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We report on our study of the supernova (SN) 2022xxf based on observations obtained during the first four months of its evolution. The light curves (LCs) display two humps of similar maximum brightness separated by 75 days, unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf is the most nearby SN IcBL to date (in NGC 3705, z = 0.0037, at a distance of about 20 Mpc). Optical and near-infrared photometry and spectroscopy were used to identify the energy source powering the LC. Nearly 50 epochs of high signal-to-noise ratio spectroscopy were obtained within 130 days, comprising an unparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets to date. The global spectral appearance and evolution of SN 2022xxf points to typical SN Ic/IcBL, with broad features (up to ~14 000 km s−1) and a gradual transition from the photospheric to the nebular phase. However, narrow emission lines (corresponding to ~ 1000–2500 km s−1) are present in the spectra from the time of the second rise, suggesting slower-moving circumstellar material (CSM). These lines are subtle, in comparison to the typical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn, and Icn, but some are readily noticeable at late times, such as in Mg I λ5170 and [O I] λ5577. Unusually, the near-infrared spectra show narrow line peaks in a number of features formed by ions of O and Mg. We infer the presence of CSM that is free of H and He. We propose that the radiative energy from the ejecta-CSM interaction is a plausible explanation for the second LC hump. This interaction scenario is supported by the color evolution, which progresses to blue as the light curve evolves along the second hump, and by the slow second rise and subsequent rapid LC drop. SN 2022xxf may be related to an emerging number of CSM-interacting SNe Ic, which show slow, peculiar LCs, blue colors, and subtle CSM interaction lines. The progenitor stars of these SNe likely experienced an episode of mass loss consisting of H/He-free material shortly prior to explosion.

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A Multiwavelength View of the Rapidly Evolving SN 2018ivc: An Analog of SN IIb 1993J but Powered Primarily by Circumstellar Interaction

Cited by 12 publications

References 93 publications

Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors

Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors

SN 2020bio: A Double-peaked Type IIb Supernova with Evidence of Early-time Circumstellar Interaction

The broad-lined Type-Ic supernova SN 2022xxf and its extraordinary two-humped light curves

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