The complex circumstellar environment of supernova 2023ixf

Zimmerman, E. A.; Irani, I.; Chen, P.; Gal-Yam, A.; Schulze, S.; Perley, D. A.; Sollerman, J.; Filippenko, A. V.; Shenar, T.; Yaron, O.; Shahaf, S.; Bruch, R. J.; Ofek, E. O.; De Cia, A.; Brink, T. G.; Yang, Y.; Vasylyev, S. S.; Ben Ami, S.; Aubert, M.; Badash, A.; Bloom, J. S.; Brown, P. J.; De, K.; Dimitriadis, G.; Fransson, C.; Fremling, C.; Hinds, K.; Horesh, A.; Johansson, J. P.; Kasliwal, M. M.; Kulkarni, S. R.; Kushnir, D.; Martin, C.; Matuzewski, M.; McGurk, R. C.; Miller, A. A.; Morag, J.; Neil, J. D.; Nugent, P. E.; Post, R. S.; Prusinski, N. Z.; Qin, Y.; Raichoor, A.; Riddle, R.; Rowe, M.; Rusholme, B.; Sfaradi, I.; Sjoberg, K. M.; Soumagnac, M.; Stein, R. D.; Strotjohann, N. L.; Terwel, J. H.; Wasserman, T.; Wise, J.; Wold, A.; Yan, L.; Zhang, K.

doi:10.1038/s41586-024-07116-6

Cited by 13 publications

(35 citation statements)

References 55 publications

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“…We have found from our SED modeling that at ∼10 15 cm (or, ∼10 R å ) the CSM was cool enough for dust to form significantly and the resulting dust shell extended outward as the density progressively declined. That Zimmerman et al (2024) concluded that the density beyond the dense, confined CSM and shock breakout regime must fall off as ∝r −2 lends support to our assumption of a similar density distribution for the dust shell. Following Grefenstette et al (2023), Zimmerman et al (2024) assumed a gas density ∼ 4 × 10 −16 g cm −3 at ∼10 15 cm, whereas we found the dust density to be ∼10 −17 to ∼10 −18 g cm −3 at this radius (R in ); these two density estimates are consistent for a reasonable assumed gas-to-dust ratio of 200.…”

Section: Further Thoughtssupporting

confidence: 75%

“…We will therefore consider solar, subsolar, and supersolar metallicities below when analyzing the properties of the progenitor candidate. We note that Zimmerman et al (2024) inferred from absorption lines detected in HST ultraviolet (UV) spectra of the SN, likely arising from the star's CSM, that the CSM metallicity was approximately solar. From observations of emission regions near the star those authors also inferred solar to slightly subsolar metallicity.…”

Section: Supernova Site Metallicitymentioning

confidence: 88%

“…We note, however, that we have shown that it could be plausible to set up the CSM with just a steady, low wind velocity and a moderate M  over the course of the RSG phase, without the need to invoke a superwind or eruption: the range in values for R in for the dust shell are essentially consistent with the estimates of the confined CSM dimensions obtained from the SN itself (e.g., Bostroem et al 2023;Jacobson-Galán et al 2023). (Furthermore, Zimmerman et al 2024 argued that radiative acceleration can explain the observed high-velocity flash-feature profiles without invoking a recent pre-SN stellar eruption to accelerate matter.) We caution that wind velocities  100 km s −1 might even hamper significant dust production, since matter needs to remain long enough within the dust-formation zone.…”

Section: Further Thoughtsmentioning

confidence: 99%

“…From the BPASS models a surviving companion would have luminosities of, for instance, −5.3 and −4.8 mag in WFC3/UVIS F275W and F336W, respectively. Zimmerman et al (2024), via an analysis of early time UV spectra obtained of the SN with HST, estimated densities and dimensions of different regimes within the star's CSM. Those authors determined that a higher-density (∼5 × 10 −13 g cm −3 ), confined (2 × 10 14 cm; see also Martinez et al 2024) region of CSM above the stellar photosphere (they estimated the star's radius at ∼5 × 10 13 cm, whereas our estimate is a factor of 2 larger, ∼1 × 10 14 cm; see Section 8) extended the shock breakout.…”

Section: Further Thoughtsmentioning

confidence: 99%

“…Early photometric and spectroscopic studies of the SN have described the evidence for interaction of the SN shock with a dense, confined (<2 × 10 15 cm) CSM, which further boosted (by 2 mag) the SN's early time optical luminosity (Bostroem et al 2023;Hiramatsu et al 2023;Hosseinzadeh et al 2023;Jacobson-Galán et al 2023;Smith et al 2023;Teja et al 2023;Yamanaka et al 2023). Zimmerman et al (2024) further constrained the confined CSM, which led to an extended shock breakout, at <2 × 10 14 cm. Smith et al (2023), Vasylyev et al (2023), and Li et al (2024) presented evidence for asymmetry in the CSM and the SN ejecta.…”

Section: Introductionmentioning

confidence: 98%

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The SN 2023ixf Progenitor in M101. II. Properties

Van Dyk,

Srinivasan,

Andrews

et al. 2024

ApJ

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We follow our first paper with an analysis of the ensemble of the extensive preexplosion ground- and space-based infrared observations of the red supergiant (RSG) progenitor candidate for the nearby core-collapse supernova SN 2023ixf in Messier 101, together with optical data prior to the explosion obtained with the Hubble Space Telescope (HST). We have confirmed the association of the progenitor candidate with the supernova (SN), as well as constrained the metallicity at the SN site, based on SN observations with instruments at Gemini-North. The internal host extinction to the SN has also been confirmed from a high-resolution Keck spectrum. We fit the observed spectral energy distribution (SED) for the star, accounting for its intrinsic variability, with dust radiative-transfer modeling, which assumes a silicate-rich dust shell ahead of the underlying stellar photosphere. The star is heavily dust obscured, likely the dustiest progenitor candidate yet encountered. We found median estimates of the star’s effective temperature and luminosity of 2770 K and 9.0 × 104 L ⊙, with 68% credible intervals of 2340–3150 K and (7.5–10.9) × 104 L ⊙, respectively. The candidate may have a Galactic RSG analog, IRC −10414, with a strikingly similar SED and luminosity. Via comparison with single-star evolutionary models we have constrained the initial mass of the progenitor candidate from 12 M ⊙ to as high as 14 M ⊙. We have had available to us an extraordinary view of the SN 2023ixf progenitor candidate, which should be further followed up in future years with HST and the James Webb Space Telescope.

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Section: Further Thoughtssupporting

confidence: 75%

Section: Supernova Site Metallicitymentioning

confidence: 88%

Section: Further Thoughtsmentioning

confidence: 99%

Section: Further Thoughtsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

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The SN 2023ixf Progenitor in M101. II. Properties

Van Dyk,

Srinivasan,

Andrews

et al. 2024

ApJ

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Early-time γ-ray constraints on cosmic-ray acceleration in the core-collapse SN 2023ixf with the Fermi Large Area Telescope

Martí-Devesa,

Cheung,

Di Lalla

et al. 2024

A&A

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While supernova remnants (SNRs) have been considered the most relevant Galactic cosmic ray (CR) accelerators for decades, core-collapse supernovae (CCSNe) could accelerate particles during the earliest stages of their evolution and hence contribute to the CR energy budget in the Galaxy. Some SNRs have indeed been associated with TeV gamma -rays, yet proton acceleration efficiency during the early stages of an SN expansion remains mostly unconstrained. The multi-wavelength observation of SN 2023ixf, a Type II supernova (SN) in the nearby galaxy M101 (at a distance of 6.85 Mpc), opens the possibility to constrain CR acceleration within a few days after the collapse of the red super-giant stellar progenitor. With this work, we intend to provide a phenomenological, quasi-model-independent constraint on the CR acceleration efficiency during this event at photon energies above 100 MeV. We performed a maximum-likelihood analysis of gamma -ray data from the Fermi Large Area Telescope up to one month after the SN explosion. We searched for high-energy, non-thermal emission from its expanding shock, and estimated the underlying hadronic CR energy reservoir assuming a power-law proton distribution consistent with standard diffusive shock acceleration. We do not find significant gamma -ray emission from SN 2023ixf. Nonetheless, our non-detection provides the first limit on the energy transferred to the population of hadronic CRs during the very early expansion of a CCSN. Under reasonable assumptions, our limits would imply a maximum efficiency on the CR acceleration of as low as 1<!PCT!>, which is inconsistent with the common estimate of 10<!PCT!> in generic SNe. However, this result is highly dependent on the assumed geometry of the circumstellar medium, and could be relaxed back to 10<!PCT!> by challenging spherical symmetry. Consequently, a more sophisticated, inhomogeneous characterisation of the shock and the progenitor's environment is required before establishing whether or not Type II SNe are indeed efficient CR accelerators at early times.

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Spectroscopic observations of progenitor activity 100 days before a Type Ibn supernova

Brennan,

Sollerman,

Irani

et al. 2024

A&A

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Obtaining spectroscopic observations of the progenitors of core-collapse supernovae is often unfeasible, due to an inherent lack of knowledge as to what stars experience supernovae and when they will explode. In this Letter we present photometric and spectroscopic observations of the progenitor activity of before the He-rich progenitor explodes as a Type Ibn supernova. The progenitor of shows an exponential rise in flux prior to core collapse. Complex He I emission line features are observed in the progenitor spectra, with a P Cygni-like profile, as well as an evolving broad base with velocities of the order of 10,000 The luminosity and evolution of is consistent with a Type Ibn, reaching a peak $r$-band magnitude of $-18.8$ mag, although there is some uncertainty regarding the distance to the host, NGC 4388, which is located in the Virgo cluster. We present additional evidence of asymmetric He-rich material being present both prior to and after the explosion of which suggests that this material survived the ejecta interaction. Broad O I C I and the Ca II triplet lines are observed at late phases, confirming that was a genuine supernova, rather than a non-terminal interacting transient. provides insight into the final moments of a massive star's life, demonstrating that the progenitor is likely highly unstable before core collapse.

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The complex circumstellar environment of supernova 2023ixf

Cited by 13 publications

References 55 publications

The SN 2023ixf Progenitor in M101. II. Properties

The SN 2023ixf Progenitor in M101. II. Properties

Early-time γ-ray constraints on cosmic-ray acceleration in the core-collapse SN 2023ixf with the Fermi Large Area Telescope

Spectroscopic observations of progenitor activity 100 days before a Type Ibn supernova

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