A Pre-explosion Effervescent Zone for the Circumstellar Material in SN 2023ixf

Soker, Noam

doi:10.1088/1674-4527/ace51f

Cited by 9 publications

(5 citation statements)

References 44 publications

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“…The spectropolarimetric observations presented in this work align with the conclusions of Smith et al (2023), where the CSM was also suggested as being asymmetric from the lack of blueshifted absorption components in the narrow P Cygni profiles. Another possible model for the CSM includes the presence of a preexplosion effervescence zone (see Soker 2023). The polarimetry results suggest that such an effervescence zone may be flat due to the rotation of the progenitor or binary interaction.…”

Section: Discussionmentioning

confidence: 99%

Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf

Vasylyev,

Yang 杨,

Filippenko

et al. 2023

ApJL

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We present six epochs of optical spectropolarimetry of the Type II supernova (SN) 2023ixf ranging from ∼2 to 15 days after the explosion. Polarimetry was obtained with the Kast double spectrograph on the Shane 3 m telescope at Lick Observatory, representing the earliest such observations ever captured for an SN. We observe a high continuum polarization p cont ≈ 1% on days +1.4 and +2.5 before dropping to 0.5% on day +3.5, persisting at that level up to day +14.5. Remarkably, this change coincides temporally with the disappearance of highly ionized “flash” features. The decrease of the continuum polarization is accompanied by a ∼70° rotation of the polarization position angle (PA) as seen across the continuum. The early evolution of the polarization may indicate different geometric configurations of the electron-scattering atmosphere as seen before and after the disappearance of the emission lines associated with highly ionized species (e.g., He ii, C iv, and N iii), which are likely produced by elevated mass loss shortly prior to the SN explosion. We interpret the rapid change of polarization and PA from days +2.5 to +4.5 as the time when the SN ejecta emerge from the dense asymmetric circumstellar material (CSM). The temporal evolution of the continuum polarization and the PA is consistent with an aspherical SN explosion that exhibits a distinct geometry compared to the CSM. The rapid follow-up spectropolarimetry of SN 2023ixf during the shock ionization phase reveals an exceptionally asymmetric mass-loss process leading up to the explosion.

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Section: Discussionmentioning

confidence: 99%

Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf

Vasylyev,

Yang 杨,

Filippenko

et al. 2023

ApJL

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“…Therefore, it is possible that the progenitor experienced a relatively enhanced mass loss (M M 2 10 4   » ´yr −1 ) until several years before the explosion and experienced an extreme mass loss (M M 10 10 3 0 -  =yr −1 ) later during 1-3 yr before the explosion. It is also worth mentioning that the discrepancy of mass-loss rate maybe originates from nonhomogeneous CSM (Beasor et al 2023;Smith et al 2023;Soker 2023).…”

Section: Mass-loss Ratementioning

confidence: 99%

The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101

Niu,

Sun,

Maund

et al. 2023

ApJL

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As one of the closest supernovae (SNe) in the last decade, SN 2023ixf is an unprecedented target to investigate the progenitor star that exploded. However, there is still significant uncertainty in the reported progenitor properties. In this work, we present a detailed study of SN 2023ixf’s progenitor with two independent analyses. We first modeled its spectral energy distribution (SED) based on Hubble Space Telescope optical, Spitzer mid-infrared (IR), and ground-based near-IR data. We find that stellar pulsation and circumstellar extinction have great impacts on SED fitting, and the result suggests a relatively massive red supergiant surrounded by C-rich dust with an initial mass of 16.2–17.4 M ⊙. The corresponding rate of mass loss occurring at least 3 yr before the SN explosion is about 2 × 10−4 M ⊙ yr−1. We also derived the star formation history of the SN environment based on resolved stellar populations, and the most recent star-forming epoch corresponds to a progenitor initial mass of 17–19 M ⊙, in agreement with that from our SED fitting. Therefore, we conclude that the progenitor of SN 2023ixf is close to the high-mass end for Type II SN progenitors.

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“…In such a binary scenario, eruptive mass loss from a single RSG may not be the driving force behind the dense CSM that we observe. In addition, Soker (2021Soker ( , 2023 suggested that the long-lived effervescent zone formed around RSGs could be an alternative scenario for the dense CSM around the progenitors of Type II SNe.…”

Section: Comparison With Other Precursor Studiesmentioning

confidence: 99%

A Comprehensive Optical Search for Pre-explosion Outbursts from the Quiescent Progenitor of SN 2023ixf

Dong 董,

Sand,

Valenti

et al. 2023

ApJ

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We perform a comprehensive search for optical precursor emission at the position of SN 2023ixf using data from the DLT40, ZTF, and ATLAS surveys. By comparing the current data set with precursor outburst hydrodynamical model light curves, we find that the probability of a significant outburst within 5 yr of explosion is low, and the circumstellar material (CSM) ejected during any possible precursor outburst is likely smaller than ∼0.015M ⊙. By comparing to a set of toy models, we find that, if there was a precursor outburst, the duration must have been shorter than ∼100 days for a typical brightness of M r ≃ −9 mag or shorter than 200 days for M r ≃ −8 mag; brighter, longer outbursts would have been discovered. Precursor activity like that observed in the normal Type II SN 2020tlf (M r ≃ −11.5) can be excluded in SN 2023ixf. If the dense CSM inferred by early flash spectroscopy and other studies is related to one or more precursor outbursts, then our observations indicate that any such outburst would have to be faint and only last for days to months, or it occurred more than 5 yr prior to the explosion. Alternatively, any dense, confined CSM may not be due to eruptive mass loss from a single red supergiant progenitor. Taken together, the results of SN 2023ixf and SN 2020tlf indicate that there may be more than one physical mechanism behind the dense CSM inferred around some normal Type II supernovae.

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A Pre-explosion Effervescent Zone for the Circumstellar Material in SN 2023ixf

Cited by 9 publications

References 44 publications

Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf

Early Time Spectropolarimetry of the Aspherical Type II Supernova SN 2023ixf

The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101

A Comprehensive Optical Search for Pre-explosion Outbursts from the Quiescent Progenitor of SN 2023ixf

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