The dusty and extremely red progenitor of the type II supernova 2023ixf in Messier 101

Xiang, Danfeng; Mo, Jun; Wang, Lingzhi; Wang, Xiaofeng; Zhang, Jujia; Lin, Han; Wang, Lifan

doi:10.1007/s11433-023-2267-0

Cited by 14 publications

(11 citation statements)

References 83 publications

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“…These values are broadly consistent with previous studies on the progenitor of SN 2023ixf. Our luminosity is consistent with most other work within the uncertainties (Jencson et al 2023;Neustadt et al 2024;Niu et al 2023;Qin et al 2023;Soraisam et al 2023;Van Dyk et al 2023;Xiang et al 2024), with Soraisam et al (2023) finding the highest luminosity at  L L log ( ) = 5.27 ± 0.12 or  L L log ( ) = 5.37 ± 0.12 dependent on the temperature used in their fits. Our RSG temperature is on the higher end of the range from other studies, with Kilpatrick et al (2023) finding the next hottest temperature at 3920 160 200 -+ K, but also our uncertainties are larger due to the scatter in the photometry.…”

Section: Progenitor Analysis Via Stacked Datasupporting

confidence: 92%

“…Assuming a graphitic dust model, we find that our progenitor properties are consistent with a 14-20 M e star (see Figure 3). This mass range is too high for the electron-capture scenario suggested by Xiang et al (2024).…”

Section: Progenitor Analysis Via Stacked Datamentioning

confidence: 90%

“…To constrain the properties of the progenitor of SN 2023ixf, SEDs of the progenitor are presented by a number of authors (e.g., Jencson et al 2023;Kilpatrick et al 2023;Neustadt et al 2024;Niu et al 2023;Soraisam et al 2023;Xiang et al 2024). Detections in Spitzer channel 1 and channel 2, MMT J, Gemini/NIRI J, UKIRT JHK, and Hubble Space Telescope (HST) F814W and F675W are used here.…”

Section: Progenitor Analysis Via Stacked Datamentioning

confidence: 99%

“…The discovery of SN 2023ixf led to a sustained spectroscopic and photometric follow-up effort (e.g., Berger et al 2023;Bostroem et al 2023;Jacobson-Galán et al 2023;Sgro et al 2023;Smith et al 2023). To date, these multiwavelength follow-up observations and archival data examination have revealed detections of a dusty RSG progenitor and signatures of interaction with circumstellar material (e.g., Berger et al 2023;Bostroem et al 2023;Grefenstette et al 2023;Guetta et al 2023;Hiramatsu et al 2023;Jacobson-Galán et al 2023;Jencson et al 2023;Kilpatrick et al 2023;Koenig 2023;Kong 2023;Li et al 2023;Neustadt et al 2024;Niu et al 2023;Panjkov et al 2023;Pledger & Shara 2023;Qin et al 2023;Sarmah 2023;Singh Teja et al 2023;Smith et al 2023;Soraisam et al 2023;Van Dyk et al 2023;Vasylyev et al 2023;Xiang et al 2024;Yamanaka et al 2023;Zhang et al 2023).…”

Section: Introductionmentioning

confidence: 99%

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SN 2023ixf in Messier 101: The Twilight Years of the Progenitor as Seen by Pan-STARRS

Ransome,

Villar,

Tartaglia

et al. 2024

ApJ

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The nearby type II supernova, SN 2023ixf in M101 exhibits signatures of early time interaction with circumstellar material in the first week postexplosion. This material may be the consequence of prior mass loss suffered by the progenitor, which possibly manifested in the form of a detectable presupernova outburst. We present an analysis of long-baseline preexplosion photometric data in the g, w, r, i, z, and y filters from Pan-STARRS as part of the Young Supernova Experiment, spanning ∼5000 days. We find no significant detections in the Pan-STARRS preexplosion light curves. We train a multilayer perceptron neural network to classify presupernova outbursts. We find no evidence of eruptive presupernova activity to a limiting absolute magnitude of −7 mag. The limiting magnitudes from the full set of gwrizy (average absolute magnitude ≈ −8 mag) data are consistent with previous preexplosion studies. We use deep photometry from the literature to constrain the progenitor of SN 2023ixf, finding that these data are consistent with a dusty red supergiant progenitor with luminosity log L / L ⊙ ≈ 5.12 and temperature ≈ 3950 K, corresponding to a mass of 14–20 M ⊙.

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Section: Progenitor Analysis Via Stacked Datasupporting

confidence: 92%

Section: Progenitor Analysis Via Stacked Datamentioning

confidence: 90%

Section: Progenitor Analysis Via Stacked Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

SN 2023ixf in Messier 101: The Twilight Years of the Progenitor as Seen by Pan-STARRS

Ransome,

Villar,

Tartaglia

et al. 2024

ApJ

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“…While stellar evolutionary models are still not robust for evolved massive stars, in order to have such high  M values, mechanisms other than steady winds are likely at play in the end point of RSG evolution. For instance, recently revised studies of  M from observed RSGs find that even the most luminous members seem to have quiescent mass losses of at maximum  Kilpatrick et al 2023;Xiang et al 2024). Therefore, a period of enhanced mass loss from a superwind phase, a sudden outburst, or a binary companion in the weeks to years before explosion may need to be invoked, particularly for the class of objects showing flash ionization.…”

Section: The Progenitor Mass-loss Ratementioning

confidence: 99%

SN 2022jox: An Extraordinarily Ordinary Type II SN with Flash Spectroscopy

Andrews,

Pearson,

Hosseinzadeh

et al. 2024

ApJ

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We present high-cadence optical and ultraviolet (UV) observations of the Type II supernova (SN), SN 2022jox which exhibits early spectroscopic high-ionization flash features of H i, He ii, C iv, and N iv that disappear within the first few days after explosion. SN 2022jox was discovered by the Distance Less Than 40 Mpc survey ∼0.75 day after explosion with follow-up spectra and UV photometry obtained within minutes of discovery. The SN reached a peak brightness of M V ∼ −17.3 mag, and has an estimated 56Ni mass of 0.04 M ⊙, typical values for normal Type II SNe. The modeling of the early light curve and the strong flash signatures present in the optical spectra indicate interaction with circumstellar material (CSM) created from a progenitor with a mass-loss rate of M ̇ ∼ 10 − 3 – 10 − 2 M ⊙ y r − 1 . There may also be some indication of late-time CSM interaction in the form of an emission line blueward of Hα seen in spectra around 200 days. The mass-loss rate of SN 2022jox is much higher than the values typically associated with quiescent mass loss from red supergiants, the known progenitors of Type II SNe, but is comparable to inferred values from similar core-collapse SNe with flash features, suggesting an eruptive event or a superwind in the progenitor in the months or years before explosion.

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Circumstellar interaction models for the early bolometric light curve of SN 2023ixf

Martinez,

Bersten,

Folatelli

et al. 2024

A&A

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Type II supernovae ( show growing evidence of an interaction with circumstellar material (CSM) surrounding their progenitor stars as a consequence of enhanced mass loss during the last years of the progenitor's life, although the exact mechanism is still unknown. We present an analysis of the progenitor mass-loss history of SN 2023ixf, a nearby showing signs of an interaction. First, we calculated the early-time ($<$\,19 days) bolometric light curve for SN 2023ixf based on the integration of the observed flux covering ultraviolet, optical and near-infrared bands, and black-body extrapolations for the unobserved flux. Our calculations detected the sudden increase to maximum luminosity and temperature, in addition to the subsequent fall, displaying an evident peak. This is the first time that this phase can be precisely estimated for a We used the early-time bolometric light curve of SN 2023ixf to test the calibrations of bolometric corrections against colours from the literature. In addition, we included the observations of SN 2023ixf into some of the available calibrations to extend their use to earlier epochs. A comparison of the observed bolometric light curve to explosion models with CSM interaction suggests a progenitor mass-loss rate of confined to 12000\ (sim \,8 $\,cm) and a wind acceleration parameter of beta This model reproduces the early bolometric light curve, expansion velocities, and the epoch of disappearance of interacting lines in the spectra. This model indicates that the wind was launched sim \,80 yr before the explosion. If the effect of the wind acceleration is not taken into account, the enhanced wind must have developed over the final months to years prior to the SN, which may not be consistent with the lack of outburst detection in pre-explosion images over the last sim \,20 yr before explosion.

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The dusty and extremely red progenitor of the type II supernova 2023ixf in Messier 101

Cited by 14 publications

References 83 publications

SN 2023ixf in Messier 101: The Twilight Years of the Progenitor as Seen by Pan-STARRS

SN 2023ixf in Messier 101: The Twilight Years of the Progenitor as Seen by Pan-STARRS

SN 2022jox: An Extraordinarily Ordinary Type II SN with Flash Spectroscopy

Circumstellar interaction models for the early bolometric light curve of SN 2023ixf

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