A shock flash breaking out of a dusty red supergiant

Li, Gaici; Hu, Maokai; Li, Wenxiong; Yang, Yi; Wang, Xiaofeng; Yan, Shengyu; Hu, Lei; Zhang, Jujia; Mao, Yiming; Riise, Henrik; Gao, Xing; Sun, Tianrui; Liu, Jialian; Xiong, Dingrong; Wang, Lifan; Mo, Jun; Iskandar, Abdusamatjan; Xi, Gaobo; Xiang, Danfeng; Wang, Lingzhi; Sun, Guoyou; Zhang, Keming; Chen, Jian; Lin, Weili; Guo, Fangzhou; Liu, Qichun; Cai, Guangyao; Zhou, Wenjie; Zhao, Jingyuan; Chen, Jin; Zheng, Xin; Li, Keying; Zhang, Mi; Xu, Shijun; Lyu, Xiaodong; Castro-Tirado, Alberto J.; Chufarin, Vasilii; Potapov, Nikolay; Ionov, Ivan; Korotkiy, Stanislav; Nazarov, Sergey; Sokolovsky, Kirill; Hamann, Norman; Herman, Eliot

doi:10.1038/s41586-023-06843-6

Cited by 10 publications

(10 citation statements)

References 60 publications

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“…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. We note that the modeling by Martinez et al (2024) results in a constraint on an extended CSM, at ∼8 × 10 14 cm, which is consistent with the confidence intervals on R in ; however, we posit that the lowerdensity dusty CSM extends well beyond that (see also Li et al 2024). In Figure 15 we show a cartoon schematic of the approximate progenitor CSM geometry, with the asymmetric (Smith et al 2023;Vasylyev et al 2023;Li et al 2024), confined CSM indicated above the photosphere and the inner radius of the simplistically spherical dust shell represented, as well as the range of possible binary orbits; this again illustrates Figure 15.…”

Section: Further Thoughtssupporting

confidence: 84%

“…We note that the modeling by Martinez et al (2024) results in a constraint on an extended CSM, at ∼8 × 10 14 cm, which is consistent with the confidence intervals on R in ; however, we posit that the lowerdensity dusty CSM extends well beyond that (see also Li et al 2024). In Figure 15 we show a cartoon schematic of the approximate progenitor CSM geometry, with the asymmetric (Smith et al 2023;Vasylyev et al 2023;Li et al 2024), confined CSM indicated above the photosphere and the inner radius of the simplistically spherical dust shell represented, as well as the range of possible binary orbits; this again illustrates Figure 15. A cartoon schematic of the SN 2023ixf progenitor candidate prior to explosion, to approximate scale, based on observational and modeling inference.…”

Section: Further Thoughtssupporting

confidence: 84%

“…Here we represent the stellar photosphere at its median effective radius R å ≈ 1390 R e . Immediately above that is the dense, asymmetric (Smith et al 2023;Vasylyev et al 2023;Li et al 2024), confined CSM inferred by Zimmerman et al (2024). The inner radius R in of the (assumed) spherically symmetric dust shell, which we infer here from our SED modeling, is shown at its median value of 10 R å ≈ 1 × 10 15 cm.…”

Section: Further Thoughtsmentioning

confidence: 64%

“…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. Further signs of early CSM interaction at other wavelengths include the detection of the SN in X-rays (up to 20 keV) at several epochs, starting about 4 days after explosion and beyond (Chandra et al 2023b;Grefenstette et al 2023;Mereminskiy et al 2023;Chandra et al 2024), as well as, after initial radio and submillimeter nondetections (Chandra et al 2023a;Berger et al 2023), detection at centimeter wavelengths ∼29 days postdiscovery (Matthews et al 2023).…”

Section: Introductionmentioning

confidence: 96%

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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: 84%

Section: Further Thoughtssupporting

confidence: 84%

Section: Further Thoughtsmentioning

confidence: 64%

Section: Introductionmentioning

confidence: 96%

See 2 more Smart Citations

The SN 2023ixf Progenitor in M101. II. Properties

Van Dyk,

Srinivasan,

Andrews

et al. 2024

ApJ

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“…Moreover, interaction of SN ejecta with CSM can also result in higher temperature and fast rise in the early light curves (e.g., Haynie & Piro 2021;Terreran et al 2022;Jacobson-Galán et al 2022;Irani et al 2023). Most interestingly, the serendipitous capture of pre-and postexplosion of SN 2023ixf have witnessed that the resulted shock passed through the dust shell, leading to a quick change of shock radiation from red to blue light (Li et al 2024). The close-by CSM are possibly common for SNe IIP/IIL, but the mass-loss rate derived from their spectra or light curves are far higher than that from their RSG progenitors.…”

Section: Introductionmentioning

confidence: 99%

The Red Supergiant Progenitor of Type II Supernova 2024ggi

Xiang,

Mo,

Wang

et al. 2024

ApJL

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We present a detailed analysis of the progenitor and its local environment for the recently discovered Type II supernova (SN) 2024ggi at a distance of about 6.7 Mpc, by utilizing the pre-explosion images from the Hubble Space Telescope and Spitzer Space Telescope. The progenitor is identified as a red bright variable star, with absolute F814W-band magnitudes being −6.2 mag in 1995 to −7.2 mag in 2003, respectively, consistent with that of a normal red supergiant star. Combining with the historical mid-infrared light curves, a pulsational period of about 379 days can be inferred for the progenitor star. Fitting its spectral energy distribution with stellar spectral models yields the stellar parameters of temperature, radius, and bolometric luminosity as T * = 3290 − 27 + 19 K, R * = 887 − 51 + 60 R ⊙, and log(L/L ⊙) = 4.92 − 0.04 + 0.05 , respectively. The above parameters indicate that the progenitor of SN 2024ggi is consistent with the stellar evolutionary track of a solar-metallicity massive star with an initial mass of 13 − 1 + 1 M ⊙. Moreover, our analysis indicates a relatively low mass-loss rate (i.e., <3 × 10−6 M ⊙ yr−1) for the progenitor compared to that inferred from flash spectroscopy and X-ray detection (i.e., 10−2–10−5 M ⊙ yr−1), implying a significant enhancement in mass loss within a few years prior to the explosion.

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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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A shock flash breaking out of a dusty red supergiant

Cited by 10 publications

References 60 publications

The SN 2023ixf Progenitor in M101. II. Properties

The SN 2023ixf Progenitor in M101. II. Properties

The Red Supergiant Progenitor of Type II Supernova 2024ggi

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

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