SN 2013ai: A Link between Hydrogen-rich and Hydrogen-poor Core-collapse Supernovae

Davis, Scott; Pessi, P. J.; Fraser, M.; Ertini, K.; Martínez, Laureano; Hoêflich, P.; Hsiao, E. Y.; Folatelli, G.; Ashall, C.; Phillips, M. M.; Anderson, J. P.; Bersten, Melina C.; Englert, Berthold-Georg; Fisher, Alec; Benetti, S.; Bunzel, A. Simaz; Burns, Christopher R.; Chen, T. W.; Contreras, C.; Elias‐Rosa, N.; Falco, E.; Galbany, L.; Kirshner, R.; Kumar, Sahana; Lü, Jing; Lyman, J. D.; Marion, G. H.; Mattila, S.; Maund, Justyn R.; Morrell, N.; Serón, J.; Stritzinger, Maximilian; Shahbandeh, Melissa; Sullivan, M.; Suntzeff, N. B.; Young, D. R.

doi:10.3847/1538-4357/abdd36

Cited by 6 publications

(4 citation statements)

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“…The rarity of such events, including SN 2018ivc as suggested here, may well be understood in terms of the binary interaction scenario toward SNe IIb (Section 6.3). We note that the peculiar SN II 2013ai has recently been suggested to have ejecta properties similar to those of SN 1993J and to be a link between SNe II and SNe IIb (Davis et al 2021). However, SN 2013ai shows observational properties different from those of SN 2018ivc (and its cousin SN 1996al); in particular, the lightcurve model suggests a large amount of 56 Ni (0.3-0.4M e ) for SN 2013ai.…”

Section: Implications For the Origin Of Sn 2018ivcmentioning

confidence: 57%

“…However, SN 2013ai shows observational properties different from those of SN 2018ivc (and its cousin SN 1996al); in particular, the lightcurve model suggests a large amount of 56 Ni (0.3-0.4M e ) for SN 2013ai. We also note that the environment of SN 2013ai suggests a much more massive progenitor with M ZAMS ∼ 17M e (Davis et al 2021) compared to that of SN 2018ivc.…”

Section: Implications For the Origin Of Sn 2018ivcmentioning

confidence: 67%

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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

Maeda

Chandra

Moriya

et al. 2022

ApJ

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SN 2018ivc is an unusual Type II supernova (SN II). It is a variant of SNe IIL, which might represent a transitional case between SNe IIP with a massive H-rich envelope and SNe IIb with only a small amount of the H-rich envelope. However, SN 2018ivc shows an optical light-curve evolution more complicated than that of canonical SNe IIL. In this paper, we present the results of prompt follow-up observations of SN 2018ivc with the Atacama Large Millimeter/submillimeter Array. Its synchrotron emission is similar to that of SN IIb 1993J, suggesting that it is intrinsically an SN IIb–like explosion of an He star with a modest (∼0.5–1M ⊙) extended H-rich envelope. Its radio, optical, and X-ray light curves are explained primarily by the interaction between the SN ejecta and the circumstellar material (CSM); we thus suggest that it is a rare example (and the first involving the “canonical” SN IIb ejecta) for which the multiwavelength emission is powered mainly by the SN–CSM interaction. The inner CSM density, reflecting the progenitor activity in the final decade, is comparable to that of SN IIb 2013cu, which shows a flash spectral feature. The outer CSM density, and therefore the mass-loss rate in the final ∼200 yr, is higher than that of SN 1993J by a factor of ∼5. We suggest that SN 2018ivc represents a missing link between SNe IIP and SNe IIb/Ib/Ic in the binary evolution scenario.

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Section: Implications For the Origin Of Sn 2018ivcmentioning

confidence: 57%

Section: Implications For the Origin Of Sn 2018ivcmentioning

confidence: 67%

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

Maeda

Chandra

Moriya

et al. 2022

ApJ

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“…There are no TRGB or Cepheid distances to the system, and estimates from the Tully-Fisher relation (13-17 Mpc; Bottinelli et al 1984Bottinelli et al , 1986Russell 2002;Theureau et al 2007) are discordant with that determined from SN Ia 1975A (33-50 Mpc;Arnett 1982;Davis et al 2021). Thus, a PNLF distance to the galaxies would be interesting.…”

Section: Ngc 2207/ic 2163mentioning

confidence: 76%

Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data

Jacoby,

Ciardullo,

Roth

et al. 2024

ApJS

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Thanks to the MUSE integral field spectrograph on board the Very Large Telescope (VLT), extragalactic distance measurements with the [O iii] λ5007 planetary nebula luminosity function (PNLF) are now possible out to ∼40 Mpc. Here we analyze the VLT/MUSE data for 20 galaxies from the ESO public archive to identify the systems’ planetary nebulae (PNe) and determine their PNLF distances. Three of the galaxies do not contain enough PNe for a robust measure of the PNLF, and the results for one other system are compromised of the galaxy’s internal extinction. However, we obtain robust PNLF distances for the remaining 16 galaxies, two of which are isolated and beyond 30 Mpc in a relatively unperturbed Hubble flow. From these data, we derive a Hubble constant of 74.2 ± 7.2 (stat) ±3.7 (sys) km s−1 Mpc−1, a value that is very similar to that found from other quality indicators (e.g., Cepheids, the tip of the red giant branch, and surface brightness fluctuations). At present, the uncertainty is dominated by the small number of suitable galaxies in the ESO archive and their less-than-ideal observing conditions and calibrations. Based on our experience with these systems, we identify the observational requirements necessary for the PNLF to yield a competitive value for H 0 that is independent of the Type Ia supernova distance scale.

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“…The Type II SNe typically reach peak luminosity within 1−2 weeks, whereas Type IIb SNe require more time (Pessi et al 2019). Additionally, the late-time luminosity decline of Type IIb SNe is noticeably slower compared to Type II-L SNe but faster than Type II-P SNe, and the different decline rates were proposed to correlate with the amount of hydrogen retained by the progenitor (Davis et al 2021). It has been claimed that Type Ib, IIb, II-L, and Type II-P SNe all result from the collapse of massive stars, with their main differences depending on the details of the mass loss and the amount of mixing (Davis et al 2021).…”

Section: Bolometric Light Curvementioning

confidence: 99%

SN 2019tua: A Type IIb Supernova with Multiple Bumps in the Light Curves

Huang,

Wang,

et al. 2024

ApJ

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We present photometric and spectroscopic observations and analysis of the Type IIb supernova (SN) SN 2019tua, which exhibits multiple bumps in its declining light curves between 40 and 65 days after discovery. SN 2019tua shows a time to peak of about 25 days, similar to other Type IIb SNe. Our observations indicate a decrease in its brightness of about 1 mag in the 60 days after the peak. At about days 50 and 60, its multiband light curves exhibit bumpy behavior. The complex luminosity evolution of SN 2019tua could not be well modeled with a single currently popular energy source model, e.g., radioactive decay of 56Ni, magnetar, interaction between the ejecta and a circumstellar shell. Even though the magnetar model has a smaller χ 2/dof value, the complex changes in SN 2019tua’s brightness suggest that more than one physical process might be involved. We propose a hybrid circumstellar medium (CSM) interaction plus 56Ni model to explain the bolometric light curve of SN 2019tua. The fitting results show that the ejecta mass M ej ≈ 2.4 M ⊙, the total CSM mass M CSM ≈ 1.0 M ⊙, and the 56Ni mass M Ni ≈ 0.4 M ⊙. The total kinetic energy of the ejecta is E k ≈ 0.5 × 1051 erg. Preexisting multiple shells suggest that the progenitor of SN 2019tua experienced mass ejections within approximately ∼6–44 yr prior to the explosion.

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SN 2013ai: A Link between Hydrogen-rich and Hydrogen-poor Core-collapse Supernovae

Abstract: We present a study of optical and near-infrared (NIR) spectra along with the light curves of SN 2013ai. These data range from discovery until 380 days after explosion. SN 2013ai is a fast declining type II supernova (SN II) with an unusually long rise time; 18.9 ± 2.7d in V -band and a

Cited by 6 publications

References 102 publications

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

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

Toward Precision Cosmology with Improved Planetary Nebula Luminosity Function Distances Using VLT-MUSE. II. A Test Sample from Archival Data

SN 2019tua: A Type IIb Supernova with Multiple Bumps in the Light Curves

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