Possible Detection of the Progenitor of the Type II Supernova SN 2023ixf

Pledger, Joanne; Shara, Michael M.

doi:10.3847/2041-8213/ace88b

Cited by 24 publications

(21 citation statements)

References 41 publications

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“…A broad range of possible masses, 8-20 M e , has been reported for the progenitor of SN 2023ixf from pre-explosion imaging (Pledger & Shara 2023;Kilpatrick et al 2023;Jencson et al 2023;Soraisam et al 2023). As a base model, we use an RSG model with a low mass (M ZAMS = 12 M e and M final = 11 M e ) and large radius (907 R e ) from Goldberg & Bildsten (2020) given the observed bright light-curve plateau (Section 4.1).…”

Section: Continuous Mass Lossmentioning

confidence: 99%

“…The recent discovery of Type II SN 2023ixf in M101 (Section 2) has allowed intensive multiwavelength observations. A dust-obscured RSG progenitor candidate with a possible periodic variability (≈1000-day period over the past ≈13 yr) has been identified in pre-explosion Hubble Space Telescope, Spitzer Space Telescope, and ground-based optical to infrared images (Pledger & Shara 2023;Kilpatrick et al 2023;Jencson et al 2023;Neustadt et al 2023;Soraisam et al 2023). Post-explosion observations have revealed early lightcurve excess in the optical bands (Jacobson-Galan et al 2023;Hosseinzadeh et al 2023;Singh Teja et al 2023;Sgro et al 2023), flash features in low-to-high-resolution optical spectra (Yamanaka et al 2023;Jacobson-Galan et al 2023;Smith et al 2023;Bostroem et al 2023;Singh Teja et al 2023), polarization measurements in spectropolarimetry (Vasylyev et al 2023), early X-ray detections (Grefenstette et al 2023), and millimeter nondetections (Berger et al 2023).…”

Section: Introductionmentioning

confidence: 99%

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From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion

Hiramatsu,

Tsuna,

Berger

et al. 2023

ApJL

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We present the discovery of the Type II supernova SN 2023ixf in M101 and follow-up photometric and spectroscopic observations, respectively, in the first month and week of its evolution. Our discovery was made within a day of estimated first light, and the following light curve is characterized by a rapid rise (≈5 days) to a luminous peak (M V ≈ − 18.2 mag) and plateau (M V ≈ − 17.6 mag) extending to 30 days with a fast decline rate of ≈0.03 mag day−1. During the rising phase, U − V color shows blueward evolution, followed by redward evolution in the plateau phase. Prominent flash features of hydrogen, helium, carbon, and nitrogen dominate the spectra up to ≈5 days after first light, with a transition to a higher ionization state in the first ≈2 days. Both the U−V color and flash ionization states suggest a rise in the temperature, indicative of a delayed shock breakout inside dense circumstellar material (CSM). From the timescales of CSM interaction, we estimate its compact radial extent of ∼(3–7) × 1014 cm. We then construct numerical light-curve models based on both continuous and eruptive mass-loss scenarios shortly before explosion. For the continuous mass-loss scenario, we infer a range of mass-loss history with 0.1–1.0 M ⊙ yr−1 in the final 2−1 yr before explosion, with a potentially decreasing mass loss of 0.01–0.1 M ⊙ yr−1 in ∼0.7–0.4 yr toward the explosion. For the eruptive mass-loss scenario, we favor eruptions releasing 0.3–1 M ⊙ of the envelope at about a year before explosion, which result in CSM with mass and extent similar to the continuous scenario. We discuss the implications of the available multiwavelength constraints obtained thus far on the progenitor candidate and SN 2023ixf to our variable CSM models.

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Section: Continuous Mass Lossmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion

Hiramatsu,

Tsuna,

Berger

et al. 2023

ApJL

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“…Soon after the explosion, the stellar variability of the progenitor in the infrared (IR) band was identified by . Simultaneously, several groups reported the detection of a progenitor candidate for SN 2023ixf on preexplosion images (e.g., Jencson et al 2023;Kilpatrick et al 2023;Pledger & Shara 2023;Soraisam et al 2023). Their results are all consistent with an RSG progenitor enshrouded by a dusty envelope.…”

Section: Introductionmentioning

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 the following, we adopt a host redshift for M101 of z = 0.000804 (de Vaucouleurs et al 1995). From examining preexplosion archival images, a candidate progenitor consistent with a moderate-luminosity RSG progenitor has been identified (Kilpatrick et al 2023;Pledger & Shara 2023;Soraisam et al 2023;Jencson et al 2023), suggesting a star that had an initial mass of around 12-17 M e . SN 2023ixf was quickly rising at the time of discovery and was expected to become very bright, and because it was a Type II event that could potentially show early narrow lines in the spectra, we chose to initiate an intensive observing campaign to obtain high-resolution echelle spectra every night (or almost every night) for the first week or so after discovery, in order to document rapid changes in the narrow emission from CSM.…”

Section: Introductionmentioning

confidence: 99%

High-resolution Spectroscopy of SN 2023ixf’s First Week: Engulfing the Asymmetric Circumstellar Material

Smith,

Pearson,

Sand

et al. 2023

ApJ

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We present a series of high-resolution echelle spectra of SN 2023ixf in M101, obtained nightly during the first week or so after discovery using PEPSI on the Large Binocular Telescope. Na i D absorption in these spectra indicates a host reddening of E(B − V) = 0.031 mag and a systemic velocity of +7 km s−1 relative to the average redshift of M101. Dramatic changes are seen in the strength and shape of strong emission lines emitted by circumstellar material (CSM), including He ii λ4686, C iv λλ5801,5811, Hα, and N iv λλ7109,7123. In general, these narrow lines broaden to become intermediate-width lines before disappearing from the spectrum within a few days, indicating a limited extent to the dense CSM of around 20–30 au (or ≲1014.7 cm). Hα persists in the spectrum for about a week as an intermediate-width emission line with P Cyg absorption at 700–1300 km s−1 arising in the post-shock shell of swept-up CSM. Early narrow emission lines are blueshifted and indicate an expansion speed in the pre-shock CSM of about 115 km s−1, but with even broader emission in higher-ionization lines. This is faster than the normal winds of red supergiants, suggesting some mode of eruptive mass loss from the progenitor or radiative acceleration of the CSM. A lack of narrow blueshifted absorption suggests that most of the CSM is not along our line of sight. This and several other clues indicate that the CSM of SN 2023ixf is significantly aspherical. We find that CSM lines disappear after a few days because the asymmetric CSM is engulfed by the supernova photosphere.

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Possible Detection of the Progenitor of the Type II Supernova SN 2023ixf

Cited by 24 publications

References 41 publications

From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion

From Discovery to the First Month of the Type II Supernova 2023ixf: High and Variable Mass Loss in the Final Year before Explosion

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

High-resolution Spectroscopy of SN 2023ixf’s First Week: Engulfing the Asymmetric Circumstellar Material

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